of - United States Navylouis14.nrl.navy.mil/skylab/spectral/skylab/docs/pdf/S082B_Manual.pdf4.0 5.0 6.0 7.0 Table of Contents ... and short-time roll stability was excellent. ... S052:

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Table of Contents

Introduction

The Apollo Telescope Mount

2.1 The Solar Instruments 2.2 Supporting Instrumentation

The S082B Instrument

3.1 General Description 3..2 The Telescope and Pointing 3.3 Astigmatism, Spectral Resolution, and Stray Light 3.4 Optical Coatings 3.5 Thermal Control System 3..6 Film and Film Camera 3.7 . Instrument Performance

Film History

4.1 Batches 4.2 Film Sequence Log 4.3 Mounting 4.4 Processins the Film - 4.5y' Loss of Dmax and Contrast 4.6 Fog

Calibration and Absolute Spectrophotometry

5.1 CALROC Intensity Calibration 5.2 ATM Calibration 5.3 Photometry of S082B Spectra

5.3.1' characteristic Curves 5.3.2 Conversion to Absolute Intensity 5.3.3 Curvature of Spectra

5.4 References

NSSDC Copies of the Data

6.1 Photographic Procedures 6.2 Transfer Curves 6.3 Image Degradation 6.4 Film Catalog

Observing Programs

7.1 The Joint Observing Program 7.2 The Calibration Rocket Program - CALROC 7.3 Solar Forecast Services 7.4 Skylab Associated Solar Programs

Table of Contents

8.0 Spectral Atlas 8.1 References

Appendices

A.

B.

C.

D.

E.

Skylab Documentation

Catalog of Exposures (micro-fiche)

Film Sequence Log

Bibliography

Line Lists f o r So82B Data

E.1 The Short Wavelength Spectra

E.2 The Long Wavelength Spectra

E.3 Forbidden Lines

Wavelenath Scale for NSSDC Copies of S082B Spectra

1.0 INTRODUCTION*

The sun's radiation fron the atmospheric cutoff near 3000 A to 1000 A in the extreme ultraviolet (XUV) is of great interest in solar physics because it can be of assistance in explaining the physical processes by which the sun's energy: is transmitted through its outer atmosphere against a steep temperature gradient. This is the region of the atmosphere where the temperature reaches its minimum value, 4400 K, between the photosphere and the chromosphere, then rises extremely rapidly as the million degree corona is approached. The spectrum from 3000 to 2100 A comes from the layers lower down than the temperature minimum, and is the usual continuum with Fraunhofer lines. From about 1535 to 1000 A the radiation originates in the chromosphere' and transition region, T w 20,000 K, and its spectrum is one of intense emission lines above a weak continuum. But from 1535 to 2100 A the spectrum is an extremely complex combination of absorption lines, emission lines and continuum; this represents a mixture of radiation from layers between the temperature minimum and the chromosphere, with a number of lines from the transition region. Scattered over the entire range, 3000 to 1000 A, are the forbidden lines from the corona.

The Apollo Telescope Mount (ATM), the manned solar observatory on Skylab, provided a unique opportunity for large scale observations:of the sun from above the earth's atmosphere. Supported by a coordinated program of ground- based observations, the joint observing program of its six advanced telescopes brought to bear the greatest possible observational and analytic power on fundamental problems in. solar physics .

The ATM took advantage of all that had been learned from over 25 years of solar space research conducted by means of sounding rockets, Orbiting Solar Observatories (OSO's) and monitoring satellites such as SOLRAD. Each of these programs had excelled in its own particular way: rockets, for development of specialized instruments having extremely great observing power, but which were always severely limited in observing time and wavelength span, or spatial resolution or spectral resolution; OSO's not limited in observing time, but constrained in information acquisition rate, as well as in spatial and spectral resolution; SOLRAD, having excellent time resolution,' but limited 'to broad-band detectors.

* Material for this section has been extracted from a paper in Applied Optics, 16, 879, 1977, by J. D-F. Bartoe, G. E. Brueckner, J. D. Purcell and R. Tousey, Extreme Ultraviolet Spectrograph ATM Experiment S082B.

These programs had established the need for continuous solar observation combining the specialized observing powers that each type of small instrument had provided. ATM came close to realizing this ideal. It provided almost continuous observation of the solar atmosphere for a period instrument was enormous. In addition, by fostering the simultaneous operation of the newest and most powerful’ ground-based observational techniques, the total resulting program represented a massive attack on the problems in solar physics, resembling that mounted during the I G Y for geophysics.

This Guide has been prepared to assist callaboration in the analysis of S082B data, especially from copies of the data supplied through the National Space Science Data Center through the National Space Science Data Center at NASA/GSFC. We have found, however: that by gathering the most useful data into one source, it is of benefit to any researchers who may be familiar with the general experiment but not with the specific details required in making a study of the.data. Therefore, a brief description of the experiment, the instrument, and supporting features of ATM and the Skylab program have been included in addition to specific details of the . calibration of film and instrument.

An extensive bibliography of papers by the NRL ATM analysis team is given in the Appendix indicating fruitful directions of research provided by the data and those staff members knowledgeable in specific areas.

A list of documentation references, the catalog of exposures (on microfiche), a wavelength scale, and line lists to assist in identification of lines are also included.

Requests for information about callaborating with NRL may be directed to specific members of the data reduction team whose names appear on related publications listed in the Bibliography. Access to original flight data and supporting material may be arranged by contacting Dr. Richard Tousey, Principal Investigator.

2.0 THE APOLLO TELESCOPE MOUNT*

' S k y l a b c o n s i s t e d of four p r i n c i p a l p a r t s . Largest w a s t h e S a t u r n Workshop (SWS), which p rov ided l i v i n g and working q u a r t e r s for t h e three-man crews. I t c o n t a i n e d a l so most of t h e e x p e r i m e n t s other t h a n t h e ATM. The hydrogen t a n k of a S a t u r n I V B booster (second s tage o f of S a t u r n I B ) t h a t was c o n v e r t e d t o become t h e SWS was a c y c l i n d e r 15 m l o n g and 6.7 m i n d i a m e t e r .

The second ma jo r s e c t i o n w a s t h e M u l t i p l e Docking Adapter (MDA) , c e n t e r of t h e space complex, 5 .2 m l o n g and 3.2 m i n diameter. T h i s was attached t o t h e SWS th rough a n a i r lock module (AM) and c o n t a i n e d t h e c o n t r o l and d i s p l a y p a n e l for t h e ATM. I t had two docking p o r t s : t h e f i r s t p o r t , located o n t h e l o n g a x i s e x t e n d i n g th rough t h e AWS, w a s fo r d o c k i n g t h e CSM when o n each v i s i t a t i o n it came up w i t h i t s crew of three; t h e second p o r t , 90 away, was a n a l t e r n a t e dock for a r e s c u e m i s s i o n , should it be required. Opposite t h e la t te i : p o r t was t h e ATM. The t h i r d p a r t was t h e CSM i t s e l f , much t h e same a s t h e Apollo Spacecraft developed for t h e l u n a r l a n d i n g s .

The ATM and its so lar i n s t r u m e n t s are shown i n F ig . 2.1. I t c o n s i s t e d of two c o n c e n t r i c e l emen t s : t h e o u t e r framework, o r rack, a n o c t a g o n a l s t r u c t u r e 3.4 m a c r o s s and 4 . 4 m i n l e n g t h , and i n s i d e t h e rack a c y c l i n d e r o r c a n i s t e r , 2 .1 m i n diameter and 3 m i n l e n g t h . The c a n i s t e r housed t h e solar i n s t r u m e n t s . I t was a t tached t o t h e rack through a pair of la rge gimbal r i n g s carr ied on a l a rge r i n g b e a r i n g , which allowed r o t a t i o n of t h e e n t i r e c a n i s t e r a round its a x i s . A s t i f f cruciform s t r u c t u r e d i v i d e d t h e space i n t o f o u r q u a d r a n t s and formed t h e op t i ca l bench t o which t h e ATM i n s t r u m e n t s were attached.

The ATM was d e s i g n e d t o keep t h e i n s t r u m e n t s w i t h i n t h e c a n n i s t e r aimed s t e a d i l y and p r e c i s e l y a t t h e desired p o i n t o n t h e scin regardless of d i s t u r b a n c e s such a s t h o s e c a u s e d by crew movement, w i t h i n 2 2.5 a rc sec i n yaw and p i tch and 5 arc min i n ro l l . T h e s e s p e c i f i c a t i o n s were a c t u a l l y exceeded i n f l i g h t . S h o r t - t i m e ( m i n u t e s ) yaw and p i t c h s t a b i l i t y was + 0.5 arc sec, and short-time r o l l s t a b i l i t y was e x c e l l e n t . s t a b i l i t y c o n t r o l was d e r i v e d from t h e 3 a rc min s t a b i l i t y of t h e e n t i r e Skylab, accomplished b y a n o r t h o g o n a l sys t em of c o n t r o l moment g y r o s ( C M G ) .

Par t of t h e success i n

F i n e p o i n t i n g of t h e ATM was accomplished w i t h a s o l a r p o h t i n g c o n t r o l s y s t e m (PCS), which s e n s e d t h e S u n ' s c e n t e r t o a few t e n t h s of a n arc sec and s e n t error s i g n a l s -- * Material for t h i s s e c t i o n h a s b e e n e x t r a c t e d fr'om a

paper i n Applied Opt ics , 1 6 , 825 , 1977 by R. Tousey, Apollo Telescope Mount of-zkylab: An Overview

i n t o t h e torque motors t h a t con t ro l l ed t h e r o t a t i o n a l pos i t i ons of t h e ATM c a n i s t e r g imbals . Of f se t p o i n t i n g of t h e ATM i n yaw or i n p i t c h by s t e p s of 1.25 a rc sec up t o .

24 a rc min c o u l d b e ' i n t r o d u c e d by c o u n t e r - r o t a t i n g a p a i r of q u a r t z wedges p laced i n t h e s o l a r beam i n c i d e n t on e i t h e r t h e p i t c h or t h e yaw so lar s e n s o r s . Ro ta t ion of t h e p r i sms was accomplished by a crewman w i t h h i s p a n e l " j o y s t i c k " . D i g i t a l i n d i c a t o r s read o u t yaw and p i t c h t o 1 a rc sec, and r o l l t o 1 arc min.

' A most impor t an t subsystem was t h e d i g i t a l computer. It enabled t h e crewman t o i n i t i a t e complex commands s imply . The computer could a l s o be o p e r a t e d by ground command, w h i l e t h e crew was s l e e p i n g , or i n case o f emergency. Thus many expe r imen t s were ope ra t ed w h i l e t h e crew were asleep, and a l s o d u r i n g t h e unmanned p e r i o d s between missions.

s t a b i l i t y required t o p r e s e r v e t h e focus o f t h e u l t r a h i g h r e s o l u t i o n o p t i c a l i n s t r u m e n t s . P a s s i v e thermal s t a b i l i z a - t i o n a l o n e was n o t s u f f i c i e n t t o meet t h e requi rements and was augmented by a n a c t i v e f l u i d - c o o l i n g sys tem for t h e ATM c a n i s t e r . The r e f r i g e r a t o r c o n s i s t e d of a loop, located i n s i d e t h e s k i n o f t h e c a n i s t e r , through w h i c h water and methanol w a s c i rculated t o r a d i a t o r s on t h e outs ide of t h e : can i s t e r , f a c i n g space . T h i s system maintained t h e tempera- t u r e of t h e c a n i s t e r wa l l t o 50 5 5' F w i t h cyclic v a r i a t i o n s of + 3' F. I n a d d i t i o n , s e v e r a l exper iments had t h e i r own thermal-control heater sys t ems , des igned t o main ta in t h e t empera tu re a t a l l l o c a t i o n s t o w i t h i n 2.5' F of t h e d e s i g n and c a l i b r a t i o n t empera tu re and t o l i m i t t h e r a t e of change t o no grea te r than 0.05' F p e r 5 minutes .

A problem i n t h e d e s i g n o f t h e ATM was t h e g r e a t thermal

2 . 1 The S o l a r In s t rumen t s -- Table 2.1 summarizes t h e major s o l a r exper iments and

i n s t r u m e n t a t i o n mounted i n t h e ATM. Brief s k e t c h e s of t h e s e are g i v e n below.

S052: Whi te -- l i q h t Coronaqraph

The w h i t e l i g h t coronagraph o n Skylab was des igned .by t h e High A l t i t u d e Observa tory o f t h e Nat iona l Cen te r f o r Atmospheric Research. The s c i e n t i f i c g o a l of t h e SO52 i n s t r u m e n t was t h e o b s e r v a t i o n ' o f t h e o u t e r corona from about 0.5 solar r a d i u s ( R Q ) t o 5 R o above t h e so la r l i m b , w i t h h i g h s p a t i a l and temporal r e s o l u t i o n , and from t h e s e da t a t o d e d u c e - t h e 3-D form of t h e corona a n d , i t s e v o l u t i o n and r a p i d change. These photographs from Sky lab form a n e a r l y cont inuous 'record of t h e corona for 9 months t h a t is of t h e character o b s e r v e d ' f o r on ly a few m i n u t e s once each yea r o r two a t n a t u r a l e c l i p s e . More t h a n 35 ,000 u s e f u l photographs were secured, inc lud ing coverage of more than 100 t r a n s i e n t e r u p t i o n s i n t h e corona.

S054: X-Ray Spectroqraphic Telescope

The American Science and Engineering Corporation (AS&E) and the Goddard Space Flight Center (GSFC) jointly pioneered the use of the Wolter lens, grazing-incidence

'telescope for imaging the sun in X-rays.

The instrument flown in ATM by AS&E employed a Wolter lens and was equipped with six filters, each with a '

' different transmittance curve. It was also possible to introduce a 1440-lines/mm transmission grating into the beam and thus ob,tain low resolution spectra of small bright features such as flares. Limited operation was carried on in the unattended and unmanned modes. A total of 31,785 exposures were made, with times ranging from 1/64 sec to 256 sec. Soft X-ray images from this telescope show in a most spectacular fashion the coronal holes, where the high speed solar wind streams originate..

S056: X-Ray Telescope

camera for ATM. In dimensions and general characteristics SO56 and SO54 were much alike. The principal difference between them was that SO56 had some three times less light .

gathering area, but was equipped with a different series of filters, which enabled,it to record somewhat harder X-rays . Although the instrument was operated only in the manned mode, 27,972 excellent X-ray images were secured. It was particularly successful in recording images of high spatial resolution, which showed the growth phase of flares in detail.

- -- The' GSFC also utilized a Wolter lens-type telescopic

S055: Ultraviolet - Spectrometer-Spectroheliometer - The Harvard College Observatory spectrometer and

spectroheliometer was designed to secure calibrated EUV spectra and images-of selected portions of the solar disk in the light of a number of strong emission lines. The lines were chosen to sample a broad range of solar temperatures, from the middle chromosphere to the low corona. Detection was entirely photoelectric using seven, independent, open-channel, electron multipliers in a variety of ways. Four modes of operation were available: (1) the spectrum.of a selected 5 x 5-sec arc solar area could be scanned in 3.8 min with a resolution of 1 . 6 . A ; (2) the readings from the seven multipliers, set at seven important wavelengths ranging from 280 A to 1350 A , could be read out as functions of time with 40-msec time resolution; (3) the sun could be recorded at seven wavelengths but with the'instrument scanning a line 5 sec of arc wide and 5 min.of arc long once in 5 sec, or; (4) a 5 x 5-min of arc area could be scanned with 5 x 5-sec of arc spatial resolution in 5 min at seven wavelengths. The instrument

w a s operated i n b o t h - u n a t t e n d e d and unmanned modes, ' b u t w i t h o u t t h e c a p a b i l i t y of f i n e p o i n t i n g except when manned 'and w i t h a crewman i n c h a r g e . E x c e l l e n t r e s u l t s were o b t a i n e d w i t h i n t e n s i t y d a t a c o v e r i n g a wide dynamic r a n g e w i t h h i g h precis ion..

- S082A: Extreme ---- U l t r a v i o l e t S p e c t r o h e l i o g r a p h

The XUV s p e c t r o h e l i o g r a p h of t h e Naval Research L a b o r a t o r y was a n o b j e c t i v e g r a t i n g i n s t r u m e n t which produced s i m u l t a n e o u s , monochromatic images of t h e e n t i r e s u n o v e r a broad r a n g e of t h e XUV. Over t h e 171-630-A r a n g e a s p e c t r u m of solar images e a c h 18.6 mm i n d i a m e t e r w a s r e c o r d e d . The i n s t r u m e n t produced r e s u l t s of e x t r e m e i n t e r e s t and a c q u i r e d a t o t a l o f 1032 u s e f u l e x p o s u r e s .

S082B: U l t r a v i o l e t S p e c t r o g r a p h --------- A type of so la r o b s e r v a t i o n c o n s i d e r e d of g r e a t

i m p o r t a n c e was t h e r e c o r d i n g of t h e XUV spec t rum a t great s p e c t r a l and s p a t i a l r e s o l u t i o n for d i f f e r e n t k i n d s of so l a r r e g i o n s , for example , f i l a m e n t s , active r e g i o n s , t h e l i m b , f l a r e s , and so on. The l a r g e NRL s p e c t r o g r a p h w a s d e s i g n e d for t h i s p u r p o s e . Being a p h o t o g r a p h i c i n s t r u m e n t , it had t r emendous i n f o r m a t i o n - g a t h e r i n g

: a b i l i t y . The s h o r t wave leng th r a n g e cove red the XUV from 970 A t o 1970 A w i t h a spectral r e s o l u t i o n of 0.06 A , which was s u f f i c i e n t t o o b t a i n u s e f u l l i n e p r o f i l e s . The l o n g wave leng th r a n g e e x t e n d e d from 1 9 4 0 A t o 3940 A w i t h 0 .12 A s p e c t r a l r e s o l u t i o n . P h o t o e l e c t r i c s e r v o - c o n t r o l of t h e p r i m a r y mirror w a s p r o v i d e d t o e n a b l e t h e 2-sec o f arc wide s l i t t o be stepped a c r o s s t h e l imb a t i n t e r v a l s of 1 sec of arc. The s l i t was a l s o equ ipped wi th a n imaging s y s t e m which allowed t h e crewman t o s e e exac t ly where t h e s u n ' s l i m b f e l l on t h e s l i t p la te r e l a t i v e t o t h e slit i n order t o c a l i b r a t e t h e a u t o m a t i c image- p o s i t i o n i n g device. The i n s t r u m e n t suffered p r i n c i p a l l y from h a v i n g too l o n g a s l i t t o i so la te s u f f i c i e n t l y t h e smallest s o l a r f e a t u r e s , . b u t it performed v e r y w e l l , and 6400 spectra were o b t a i n e d .

The NRL p h o t o g r a p h i c and HCO photoelectr ic i n s t r u - m e n t s complemented e a c h other i n many ways. The spectral r a n g e covered by HCO, n o m i n a l l y 280-1350 A, o v e r l a p p e d g e n e r o u s l y NRL's S082A r a n g e , 171-630 A , and S082B's range, , 970-3940 A. The a d v a n t a g e s of photoe lec t r ic . o v e r p h o t o g r a p h i c r e c o r d i n g are t h e i n c r e a s e d p r e c i s i o n of t h e i n t e n s i t y measurements and t h e wider dynamic r a n g e c o v e r e d . P h o t o g r a p h i c r e c o r d i n g , on t h e o t h e r hand , is capable of g a t h e r i n g i n f o r m a t i o n f a r more r a p i d l y t h a n . photoelectr ic , b u t t o cover a l a rge dynamic r ange r e q u i r e s making a ser ies of e x p o s u r e s c o v e r i n g a wide r a n g e of times. I n temporal r e s o l u t i o n p h o t o e l e c t r i c r e c o r d i n g is ' s u p e r i o r ;

p h o t o g r a p h i c e x c e l s i n s p a t i a l and s p e c t r a l r e s o l u t i o n . ' To t h e greatest e x t e n t pract icable S 0 5 5 , S082A and B were operated t o g e t h e r .

2.2 S u p p o r t i n g I n s t r u m e n t a t i o n

Each group of ATM e x p e r i m e n t e r s r ecogn ized t h e need for s u p p o r t i n g i n s t r u m e n t a t i o n of v a r i o u s k i n d s i n order t o m a k e optimum u s e of t h e s i x major so l a r i n s t r u m e n t s . The s u p p o r t i n g i n s t r u m e n t s f a l l i n t o several classes as fol lows :

(1) I n s t r u m e n t s t o e n a b l e t h e crewman t o p o i n t t h e ATM a t a pre-selected 'solar p o s i t i o n w i t h p r e - s e l e c t e d roll, w i t h c o o r d i n a t e v a l u e s d i s p l a y e d on-board , a n d telemetered t o ground.

i n v a r i o u s w a v e l e n g t h b a n d s , t o e n a b l e him t o p o i n t t h e ATM a t features of i n t e r e s t t h a t h e c o u l d s e e .

(2) I n s t r u m e n t s t o p r e s e n t so la r images t o t h e crewman

( 3 ) I n s t r u m e n t s t o a l e r t t h e crew t o t h e o c c u r r e n c e of a so la r f l a r e so t h a t t h e y c o u l d i n i t i a t e o b s e r v i n g programs, and a l s o i n s t r u m e n t s t o a s s i s t i n a n t i c i p a t i n g t h e o c c u r r e n c e of a s o l a r f l a r e .

. T h e .-_I_ H - A 9 l i a ---- Telescopes

The t w o H-or telescopes were t h e most u s e f u l d e v i c e s for showing t h e crewmen t h e precise p o i n t i n g of t h e ATM r e l a t i v e t o f e a t u r e s on t h e so la r d i s k and for r e c o r d i n g t h i s p o s i t i o n - . A spectral r e s o l u t i o n o f 0.7 A was a c h i e v e d w i t h Fabry-Pero t - type f i l t e rs . T h i s assured maximum v i , s i b i l i t y of solar f l a r e s and t h e ch romospher i c network. Zoom l e n s e s were a r r a n g e d t o p r o v i d e op t i ca l telescopic s y s t e m s 'which c o u l d be used a t l o w or h i g h m a g n i f i c a t i o n , w i t h a r e s o l u t i o n of 1 t o 2 arc sec a t t h e high s e t t i n g . The ATM c o n t r o l and d i sp l ay (C+D) p a n e l was equipped w i t h two i d e n t i c a l cathode ray t u b e m o n i t o r s o f six i n c h e s diameter, e a c h w i t h a n e l e c t r o n i c r e t i c l e . The images produced by t h e two H-a telescopes c o u l d be p r e s e n t e d on e i ther of these scopes, and a n y o the r TV-type image s u c h as t h e XUV m o n i t o r image c o u l d a l s o be presented. I t w a s t h u s a l so possible t o v iew a t t h e same time a h i g h l y m a g n i f i e d image of a small pa r t of t h e s u n and a n image of t h e e n t i r e sun .

H-a 81 w a s equ ipped w i t h a camera for r e c o r d i n g p h o t o g r a p h i c a l l y on 35 mm f i l m t h e H-a s o l a r image a s projected on t h e SO55 sli t w i t h 1 arc sec s p a t i a l r e s o l u - t i o n . A mechanica l ly-movable r e t i c l e system a d j u s t e d t o t h e r e l a t i v e co-a l ignment between SO55 and S082B t h e n made ,

it p o s s i b l e t o record t h e precise p o s i t i o n s of bo th S082B and 5055. \

H-a # 2 was n o t equ ipped w i t h p h o t o g r a p h i c r e c o r d i n g , and was used m a i n l y t o p r e s e n t for s t u d y by t h e crewman a h i g h q u a l i t y H-o! im-age of t h e e n t i r e sun . L i k e H-a #1 it was e q u i p p e d w i t h a movable r e t i c l e t h a t was v i s i b l e i n t h e image of t h e CRT, and cou ld be zoomed to h i g h magni- f i c a t i o n . T h e r e f o r e i t a l s o could be used f o r p o i n t i n g .

---- White L i g h t - Solar P o i n t i n g D e v i c e s

T h e r e were s e v e r a l i n s t r u m e n t s . t h a t imaged t h e s u n i n w h i t e l i g h t and could be used f o r e s t a b l i s h i n g and r e c o r d i n g so l a r p o i n t i n g c o o r d i n a t e s . The p r i n c i p a l device was t h e op t ica l ' p o i n t i n g c o n t r o l s y s t e m (PCS), descr ibed ea r l i e r . T h i s was d e s i g n e d t o p o i n t t h e e n t i r e ATM a t any d e s i r e d a n g l e s i n p i t c h and yaw r e l a t i v e t o t h e so la r c e n t e r w i t h a n a c c u r a c y of 1 . 2 5 a r c sec. The p o i n t i n g c o o r d i n a t e s were d i s p l a y e d o n , t h e C&D p a n e l and were a l s o t r a n s m i t t e d by t e l e m e t r y for r e c o r d i n g on t h e ground. I n a d d i t i o n , t h e y were recorded on t h e e n d s of t h e f i l m . s t r i p s o f S082A and B by p h o t o g r a p h y o f a pho tod iode m a t r i x b u i l t i n t o e a c h of t h e s e i n s t r u m e n t s . A d d i t i o n a l p o i n t i n g i n f o r m a t i o n was g i v e n by t h e s p e c i a l w h i t e l i g h t p o i n t i n g e r ro r s e n s o r b u i l t i n t o SO52 f o r t h e p u r p o s e o f a l i g n i n g t h e e x t e r n a l and i n t e r n a l o c c u l t e r s and t h e e n t i r e i n s t r u m e n t .

R o l l , however , c o u l d n o t be e s t a b l i s h e d a s e a s i l y 'and a c c u r a t e l y a s yaw a n d . ' p i t c h . S e v e r a l methods were a v a i l a b l e . One u t i i l i z e d t h e S k y l a b r a t e - g y r o s y s t e m which o p e r a t e d t o g e t h e r w i t h t h e CMG's t o s t a b i l i z e t h e e n t i r e Sky lab . A p o s s i b l e b u t l i t t l e used method was t o o b s e r v e a s u n s p o t i n t h e w h i t e l i g h t image p r o j e c t e d on t h e S082B s l i t and d i s p l a y e d on one o f t h e CRTs o f . t h e C&D p a n e l . The most precise i n f o r m a t i o n was g i v e n by a s t a r tracker mounted on t h e ATM. The s t a r t r a c k e r measured t h e a n g l e between Canopus or c e r t a i n o t h e r s t a r s and t h e ATM yaw and p i t c h d i r ec t ions .

The XUV Monitor ------ The XUV moni to r of NRL was a d e v i c e which showed t h e

crew i n r e a l time a v i s i b l e image of t h e s u n produced by its e m i s s i o n i n t h e e x t r e m e u l t r a v i o l e t band 171-500 A , a p p r o x i m a t e l y . T h i s band i n c l u d e d r a d i a t i o n from t h e c o r o n a and t r a n s i t i o n l a y e r , w i t h a c o n t r i b u t i o n of a b o u t 20% from t h e chromosphere. The m o n i t o r was equipped w i t h a re t ic le circle and cross t h a t permitted it t o be used fo r p o i n t i n g w i t h a s p a t i a l r e s o l u t i o n of 15-20 a rc sec. The p a t t e r n of f e a t u r e s and t h e i r i n t e n s i t i e s ' o n ' t h i s mon i to r were more n e a r l y l i k e t h o s e of t h e r a d i a t i o n s t u d i e d by t h e so la r i n s t r u m e n t s t h a n was t h e p a t t e r n o f e m i s s i o n shown by t h e H-a! telescopes. The XUV images were t r a n s - m i t t e d by TV t o t h e ground s e v e r a l times a day fo r u s e b y t h e ATM PI'S i n p l a n n i n g t h e o b s e r v i n g programs. A f i l e

of t h e ground p i c t u r e s p l u s P o l a r o i d e x p o s u r e s of t h e onboard m o n i i t o r is a v a - i l a b l e for s t u d y a t NRL. The XUV m o n i t o r w a s e x t r e m e l y v a l u a b l e for p r e d i c t i n g and l o c a t i n g t h e o c c u r r e n c e o f a s o l a r f l a r e and was a l so found most u s e f u l for l o c a t i n g b o u n d a r i e s of c o r o n a l ho le s and b r i g h t p o i n t s i n b o t h a c t i v e r e g i o n s and t h e network.

X-Ray Detecto.rs --

As par t of MSFC's S056, there was inc luded a device known as t h e X-ray Event Ana lyze r ( X R E A ) . I ts p u r p o s e was t o measure t h e t o t a l X-ray f l u x emi t t ed i n t h e band 2.5-20 A , or 5-20 A and 27-33 A. The detecting s y s t e m made u s e of two p r o p o r t i o n a l c o u n t e r s w i t h p u l s e - h e i g h t a n a l y z e r s and da ta p r o c e s s i n g f o r d i s p l a y t o t h e crewman and for t e l e m e t r y t o t h e g round .

Another d e v i c e somewhat s imi la r t o t h e XREA w a s t h e P h o t o m u l t i p l i e r Exposure Coun te r ( P M E C ) , c o n s t r u c t e d by AS&E for u s e w i t h S 0 5 4 . T h i s used a p h o t o - m u l t i p l i e r t o c o u n t t h e s c i n t i l l a t i o n s produced by X-rays i n a N a I : TA c r y s t a l t h a t viewed t h e e n t i r e s o l a r f l u x . I t was equ ipped w i t h f i l t e r s t h a t res t r ic ted i t s s e n s i t i v i t y t o t h e h a r d X-ray s p e c t r u m . A r a n g e of f i v e decades of i n t e n s i t y was ' conve r t ed by compress ion i n t o a dec imal ' r a n g e of 0-1000 c o u n t s per sec.

S t i l l a n o t h e r X-ray detector was t h e X-ray imaging s y s t e m c o n s t r u c t e d by' ASSE. T h i s c o n s i s t e d of a small Wolter l e n s which imaged t h e s u n i n X-rays onto a t h i n s c i n t i l l a t o r c rys t a l . The v i s i b l e l i g h t s c i n t i l l a t i o n s emi t t ed by t h i s c r y s t a l were detected by an image dissector t u b e which scanned t h e 'image and d i s p l a y e d t h e X-ray s u n o n a separate small CRT.on t h e C&D p a n e l . T h i s image allowed t h e crewman t o d e t e r m i n e which a c t i v e r e g i o n was f l a r i n g . The p r i n c i p a l u s e made of t h i s sys tem, however , w a s f o r d i s p l a y of t h e X-ray c o u n t l e v e l be ing detected b y t h e IDT. .

A l l th ree systems were used t o r e c o r d t h e so l a r X-ray f l u x and t o a l e r t t h e crew t o a n i n c r e a s e i n f l u x l e v e l of magn i tude s u f f i c i e n t t o s u g g e s t t h a t a f l a r e m i g h t be e x p e c t e d or t h a t a . f l a r e was i n p r o g r e s s . The da t a collected by t h e XREA and by t h e PMEC we,re of g r e a t va lue t o t h e p r i n c i p a l i n v e s t i g a t o r teams i n c o n n e c t i o n w i t h p l a n n i n g d u r i n g t h e m i s s i o n and a re a l s o u s e f u l i n t h e i n t e r p r e t a t i o n of resu l t s . They supplement X-ray f l u x measurements made by other ' sys t ems , s u c h a s t h e NRL SOLRAD 9 and 1 0 s o l a r m o n i t o r i n g s a t e l l i t e s .

- The R a d i o ' N o i s e B u r s t _--- Moni tor

of t h e radio b u r s t s e m i t t e d b y t h e w h o l e s u n i n the 6 c m band. T h e s e radio b u r s t s are sometimes p r e c u r s o r s of f l a r e s . The m o n i t o r c o n s i s t e d of a receiver and d . k p l a y t h a t showed o n a meter above t h e C&D p a n e l t h e l e v e l 'of n o i s e i n u n i t s '

of so la r rad io f l u x . T h i s d e v i c e c o u l d also be u s e d t o a c t i v a t e a n a u d i b l e alarm system t o t h e crew when t h e f l u x e x c e e d e d a c e r t a i n t h r e s h o l d v a l u e .

The s o l a r rad io n o i s e b u r s t m o n i t o r p r o v i d e d m o n i t o r i n g

Figure Captions

F i g . 2 . 1 A s k e t c h of t h e Apollo Telescope Mount. Three of the instruments can be seen attached t o t h e c e n t r a l cruciform supporting s t r u c t u r e .

.!a! Fig.x. A sketch of the Apollo Telescope Mount. Three of the instruments can be seen attached to the central cruciform supporting

structure.

.TableA!Surnmaw of ATM Instruments . ~ ~ ~~ ~ ~- ~

Manned (M) Institution Wavelength Wavelength Spatial Field Temporal unmanned (UM)

Name and number P.I. (mission) range resolution resolution of view resolution Recording unattended (UA)

' 8.2" 1.5-6 R . a40 sec Plrotographic, M, UM, UA ' , T V & T M

White light . . HA0 . 3700-7000 - coronagraph R. M. MacQueen SO52 UV spectrograph '

SO82B NRL

:R. Tousey 3940-1940 A 1970-970 A ' '

0.12 A 0.06 a ' 2" X 60" Anywhere

2" X 60" within t24' of sun ctr.

PO.15 scc Photographic M

M, UM, UA EUV spectrometer- ,

spectroheliometer ,

SO55

HCO E. M. Reeves

1350-280 A 1.6A ' , 5" x .5" 5' x 5' 5'x 5' ,

' 5"x 5"

. 57' X -60' 2.5" x 2.5"

5m Photoelectric 5sec . and TM 40 msec > 2.0 sec ' Photographic ' M,UA XUV spectrohelio-

graph S082A

X-ray spectrographic '

telescope SO54 SO54

NRL R. Tousey

630-171 a 0.025A !$

60-3.5 A AS& E 0. Vaiana

Bands gratin 0.15 f a t 7 A

-2" 48' diam 2.5 sec Photographic M, UM, UA

X-ray telescope MSFC' 53-3 A Bands 'SO56 J. E. Milligan

Hu #1 ' ,HCO 6563*0.35 A. . - E. M. Reeves

H u #2 MSFC . 6563r0.35A - P. Hassler, Jr.

R. Tousey XUV monitor NRL . 171-500 18 None

X-ray scope AS&E , 2-10A : . None

PMEC ' AS&E ' 0-8A . Pulse ' G. Vaiana, , 0-8A '. .. '

u 2" 38' diam >3.5sec . Photographic M, UA

u 1" 16-4.4'

u 1" 35-7'

15" X 15" 56' diam

1/30 sec

1/30 SCC

1/30 sec to 4 scc -1 sec

Continuous

Continuous

Continuous

Photographic M, UM, UA TV & TM TV & TM M

T V & T M ' . M

TV & M 6

1' 48' diam

None Full sun

None Full sun

Full sun None

. . digital .Digital & TM Digital M, U h 8c TM Meter . M

M, UM, UA . G.Vaiana . . height

J. E. Millignn height XREA - MSFC . 2.6-33A Pulse

RNBM MSFC 6 cm 0. K. Gnrriott .

3.0 THE S082B INSTRUMENT*

The l a r g e NRL S p e c t r o g r a p h used fo r Experiment S082B w a s a p h o t o g r a p h i c i n s t r u m e n t s imi la r t o t h o s e f l o w n i n rockets by NRL from 1960 t o 1966. The s h o r t w a v e l e n g t h r a n g e c o v e r e d t h e XUV from 970 t o 1970 A w i t h a s p e c t r a l r e s o l u t i o n of 0.06 A , which w a s s u f f i c i e n t t o o b t a i n use- f u l l i n e p r o f i l e s . The l o n g wave leng th r a n g e e x t e n d e d from 1940 t o 3940 A w i t h 0.12 A s p e c t r a l r e s o l u t i o n . Double d i s p e r s i o n was used t o reduce t h e focused s t r a y - l i g h t from t h e , l o n g w%velength p a r t of t h e s o l a r s p e c t r u m , which a t 5000 A is 1 0 more i n t e n s e t h a n a t 1500 A.

To o b t a i n s u f f i c i e n t l y h i g h s p a t i a l r e s o l u t i o n a p r i m a r y . m i r r o r w a s used t o image t h e s u n on t h e s p e c t r o - g r a p h s l i t . I n t h i s way a s o l a r element 2 a r c sec w i d e and 60 a rc sec l o n g was r e s o l v e d . The m i r r o r added a t h i r d r e f l e c t i n g s u r f a c e , however , which g r e a t l y r e d u c e d t h e speed of t h e s y s t e m a t w a v e l e n g t h s less than 1100A, t h e s h o r t wave leng th end of t h e r a n g e where high ref lec- t a n c e c o a t i n g s a r e ava i lab le . To compensa te f o r t h i s a n d . t o i n c r e a s e t h e speed g e n e r a l l y , t h e i n s t r u m e n t a l a s t i g m a - t i s m and t h e r e f o r e t h e l e n g t h s of t h e s p e c t r a l l i n e s were reduced. ,

P h o t o e l e c t r i c s e r v o - c o n t r o l o f t h e p r imary mirror was p r o v i d e d t o e n a b l e t h e 2 arc sec wide s l i t t o be

.stepped across t h e l imb a t i n t e r v a l s o f 1 a rc sec. The s l i t was a l s o e q u i p p e d w i t h a n imaging s y s t e m which allowed t h e crewman t o see e x a c t l y where t h e s u n ' s limb f e l l on t h e s l i t p la te r e l a t i v e t o t h e s l i t i n order to c a l i b r a t e t h e a u t o m a t i c i m a g e - p o s i t i o n i n g d e v i c e . The i n s t r u m e n t s u f f e r e d p r i n c i p a l l y from h a v i n g too l o n g a s l i t t o i s o l a t e s u f f i c i e n t l y t h e smallest s o l a r f e a t u r e s .

a

Temporal r e s o l u t i o n a c h i e v a b l e was a p p r o x i m a t e l y 1 min, s u f f i c i e n t t o follow t h e change i n t h e spec t rum d u r i n g

of a 5 m i n u t e p e r i o d i n t h e l o w chromosphere . , t h e f l a s h p h a s e of a f l a r e , or t o s e a r c h for o s c i l l a t i o n s

3.1 G e n e r a l D e s c r i p t i o n

The o v e r a l l op t i ca l s y s t e m of t h e XUV solar spectro- g r a p h is shown i n p e r s p e c t i v e i n F i g . 3.1. It c o n s i s t e d of a s i n g l e mirror telescope and a double g r a t i n g s p e c t r o - g r a p h .

The s p e c t r o g r a p h directed t h e l i g h t p a s s i n g t h r o u g h t h e s l i t t o o n e of two i n t e r c h a n g e a b l e p r e d i s p e r s e r g r a t i n g s , which selected t h e s h o r t or l o n g wavelength band r e a c h i n g t h e main g r a t i n g t h r o u g h t h e waveband a p e r t u r e .

-- * Material for t h i s s e c t i o n h a s been e x t r a c t e d from a

paper i n App l i ed Opt ics , 16, 879, 1977, byJ.-D. F.' Bartoe, G. E. Brueckne r , J. D. P u r c e l l a n d R. Tousey . Extreme U l t r a v ' i o l e t s p e c t r o g r a p h ATM Experiment S082B.

The main g r a t i n g was c o n c a v e , w i t h 2000 mm r a d i u s o f c u r v a t u r e , ' 6 0 0 l i n e s - p e r mm, and 76 x 1 5 2 mm c lear a p e r t u r e . The second order of t h i s g r a t i n g was used t o cover t h e spectral r a n g e 970-1970 A. a 500 mm r a d i u s predisperser g r a t i n g h a v i n g 300 l i n e s p e r mm. When used i n t h e f i r s t o r d e r t h e r a n g e 1940-3940 A was selected by a predisperser r u l e d w i t h 1 5 0 l i n e s per mm. Each predisperser was r u l e d i n 1 0 p a r t s , fo r e a c h o f which t h e s p a c i n g w a s . changed s l i g h t l y t o i n t r o d u c e a change i n s a g i t t a l f o c u s j u s t s u f f i c i e n t t o compensa te for t h e a s t ig - m a t i s m of t h e main g r a t i n g .

The d i s p e r s i o n of t h e s p e c t r o g r a p h was 8.3 A/mm and 4.2 A/mm i n t h e l o n g and s h o r t w a v e l e n g t h modes, respec- t i v e l y . The spectral r e s o l u t i o n was =0.05 A a t 1500 A and y * : O . l O A a t 3000 A. The s p a t i a l r e s o l u t i o n , d e t e r m i n e 3 by t h e s l i t and mirror, was 2 x 60 a rc sec.

T h i s w a s selected by means o f '

P h o t o g r a p h i c f i l m s used were E a s t m a n Kodak Schumann- e m u l s i o n s , m a i n l y t y p e 104, b u t w i t h some of t h e more s e n s i t i v e type 201. A camera magazine held 2 0 1 f i l m s t r i p s , e a c h of which c o u l d be moved t o 8 p o s i t i o n s , per- m i t t i n g t h e e x p o s u r e of 1608 s p e c t r a per camera. A small chip of f a s t , red s e n s i t i v e f i l m was placed a t t h e end of e a c h f i l m s t r i p f o r r e c o r d i n g e s s e n t i a l exposure d a t a d i s p l a y e d i n b i n a r y code on a diode a r r a y f l a s h e r .

3.2 The Telescope and P o i n t i n g

The t e l e s c o p e mirror was a n off-axis p a r a b o l o i d , of 1 m focal l e n g t h and 54 x 1 2 1 mm c lear a p e r t u r e . The mirror formed on t h e e n t r a n c e s l i t of the s p e c t r o g r a p h a so l a r image of 9.3 mm diameter, w i t h a r e s o l u t i o n of a p p r o x i m a t e l y 1 arc sec, close t o d i f f r a c t i o n l i m i t e d a s measured w i t h v i s i b l e l i g h t .

F i g u r e 3.2 shows t h e t e l e s c o p e and t h e p o i n t i n g ' . r e f e r e n c e sys t em. The t e l e s c o p e m i r r o r was mounted on a one a x i s p i v o t system which permitted it t o be r o t a t e d b y a s e r v o motor about a n a x i s p a r a l l e l t o the s l i t . T h i s mot ion allowed t h e s u n ' s l i m b t o be a l igned more precisely w i t h respect t o t h e s p e c t r o g r a p h s l i t , and p rov ided greater p o i n t i n g s t a b i l i t y i n one a x i s t h a n was achievable w i t h t h e ATM p o i n t i n g sys t em a l o n e .

The s t a b i l i t y i n one a x i s was t h e r e b y i n c r e a s e d t o ,

I ; + 1 arc sec w i t h a j i t t e r I; + 1 arc sec p e r sec. I n I d E o r a t o r y tests t h e s e r v o sysFem was able t o m a i n t a i n t h i s p o i n t i n g a c c u r a c y when exposed t o d r i f t r a t e s a s h i g h a s 14 arc sec per sec. I n a d d i t i o n , t h e p o i n t i n g r e f e r e n c e s y s t e m could p o s i t i o n t h e s o l a r l i m b a t any a n g l e w i t h respect t o t h e s p e c t r o g r a p h s l i t o v e r a r ange of 2 70 a rc sec w i t h a n a c c u r a c y o f 1 arc sec. \

The s e r v o l o o p was c o n t r o l l e d by an image dissector t u b e ( I D T ) , which r ece ived an image of t h e s u n reflected by t h e slit p l a t e . The slit p l a t e i t s e l f was a t h i n f i l m of n i c k e l over copper w i t h a 1 0 mic ron by 300 micron s l i t etched through it. I n a d d i t i o n , f i d u c i a l marks were e tched i n t o t h e n i c k e l l a y e r on ly . These f i d u c i a l m a r k s were used by t h e p o i n t i n g reference system e l e c t r o n i c s t o de t e rmine t h e p o s i t i o n of t h e s o l a r l imb w i t h respect t o t h e s l i t . The s l i t p l a t e and i t s sl i t were designed t o conduct away t h e hea t produced by t h e so la r image.

I n t h e " l i m b p o i n t i n g " mode, t h e system was under s e r v o c o n t r o l . The " b o r e s i g h t " mode was u s e d fo r manual p o i n t i n g of t h e s p e c t r o g r a p h , f o r checking coal ignment w i t h t h e other ATM i n s t r u m e n t s and e s p e c i a l l y t h e ATM p o i n t i n g c o n t r o l system (PCS), and for l o c a t i n g s u n s p o t s . I n t h e la t te r ,mode , ' t h e IDT o u t p u t from t h e w h i t e l i g h t solar image on t h e s l i t p l a t e was d i sp layed on o n e of t h e C R T ' s a t t h e C&D pane l .

Researchers who need t o know t h e l o c a t i o n on t h e sun of a p a r t i c u l a r exposure m u s t r e fe r t o supplementary docu- men ta t ion l i s t e d i n Appendix A. The most d i r e c t l y u s e f u l of t h e s e is t h e Harvard ATM H-Alpha A t l a s and A t l a s G u i d e ( a l l ) , wh ich g i v e s a p r i n t of t h e sun exposued i n H a a s projected on t h e ' s 0 5 5 s l i t , w i t h t h e p o s i t i o n of t h e S082B sl i t i n d i c a t e d . The a p p r o p r i a t e o r i e n t a t i o n c o o r d i n a t e s are a l so g iven . I n a d d i t i o n t o t h e selected A. t las .pr in ts made for each ATM p o i n t i n g change, a l l H a ! exposures made from Skylab are a v a i l a b l e s e p a r a t e l y on 35 mm f i l m . See a l so a d e s c r i p t i o n of t h e H-alpha t e l e s c o p e s i n S e c t i o n 2.2.

3.3 Astigmatism, S p e c t r a l Reso lu t ion , and S t r a y L i g h t

By t h e i n t r o d u c t i o n of t h e t e l e s c o p e mir ror t o t h e s p e c t r o g r a p h d e s i g n , small r e g i o n s o f t h e s u n cou ld be s t u d i e d q u a n t i t a t i v e l y , a n advantage over ear l ier rocket in s t rumen t s . I n t h e former i n s t r u m e n t s t h e p red i spense r g r a t i n g s se rved t o f0rm.a v e r y sma l l image of t h e sun on t h e s l i t , and were a l s o s l i g h t l y deformed t o n e u t r a l i z e t h e a s t igma t i sm of t h e main g r a t i n g . By r u l i n g a special type of predisperser for S082B, i n s t r u m e n t a l a s t igma t i sm was 'reduced and speed was i n c r e a s e d t o o f f s e t t h e loss i n c u r r e d by t h e t h i r d r e f l e c t i o n of t h e t e l e scope .

F igu re 3.3 i l l u s t r a t e s t h e as t igmat i sm acqui red by u s e of t h e Rowland mounting for .a g r a t i n g . With t h e r u l i n g s of t h e g r a t i n g p e r p e n d i c u l a r t o t h e plane of t h e paper, t h e t a n g e n t i a l f o c u s of t h e d i f f r ac t ed s l i t image from A l i es on t h e Rowland c i r c l e a t B, where t h e s l i t width is i n focus . The s a g i t t a l focus, or focus of t h e s l i t l e n g t h , l i es on a l i n e p e r p e n d i c u l a r t o t h e g r a t i n g normal and t a n g e n t t o t h e Rowland c i rc le a s a t p o i n t C:

This is known as Sirk's position. A converse arrangement with the tangential f.ocus at point B and the sagittal focus focus at point C should produce a stigmatic image at point A. The predispersers of the ATM spectrograph were designed to approximate this special condition. The idea was to make use of the change in sagittal focus of a concave spherical grating, secured by continuously changing the grating spacing in the proper way during ruling. This property of a grating has been known for some years in connection with grating errors; it had never been made use of in spectrograph design. To rule such a grating would have required development of a device by means.of which the grating spacing could be changed continuously and precisely. It was possible, however,' to approximate the continuous change with a multipartite grating, ruled in ten 40 mm long and 3.6-mm wide segments, each having .a slightly different ruling spacing. In the reduction of the astigmatism the spectrum was narrowed, and an increase in speed of the instrument was obtained.

Figure 3.4 illustrates the effect of the segmented predisperser. Diffracted rays from each segment come to a tangential focus on the Rowland circle of the predisperser grating, as in a conventional Rowland mount. However, the ,

ray bundles from different panels cross each other at point C before they reach the Rowland circle of the predisperser. Thus a pseudotangential focus is formed at point C. The sagittal focus of each panel still occurs along the predisperser's sagittal focal plane in the vicinity of point B. Therefore the slit width is in f.ocus at point B, while the slit length is in pseudofocus at point C, the Sirk's position for the main grating.

allowed only the central eight segments to be illuminated. As shown in Fig. 3.5, the diffracted beam from these eight perdisperser panels considerably overfilled the main grating. For any particular wavelength, only five adjacent predisperser panels, or four plus a half panel at each end, illuminated the main grating. This permitted the optimization to be made over a greater range of wavelengths because different segments were used at, say, 1200 A than at 1800 A. The ruling spacing of each predisperser segment was chosen to optimize the distance between.points C and B for the different parts of the wavelength range. Figure 3.6 shows the astigmatism at the film plane for both uniformly ruled and segmented predispersers as a function of wavelength. The spectrum height for the case of the segmented predisperser on the average is one-fourth that for the uniformly ruled predisperser. Thus the instrument speed was increased by about a factor of 4 . Without this increase in speed, the long exposure times necessary to obtain the weaker lines and continua of the solar XUV spectra, particularly for recording spectra above the solar limb, would have been too long for practical application on Skylab.

. The size of the clear aperture of the telescope mirror

Although t h e segmented p r e d i s p e r s e r i nc reased t h e i n s t r u m e n t speed , i t degraded s l i g h t l y t h e s p e c t r a l resol- r e s o l u t i o n a t t h e f i l m p l ane . T h i s was caused by t h e of f - p l a n e a b e r r a t i o n s of t h e Rowland mounting. As Fig. 3 . 7 ( a ) i l l u s t r a t e s , t h e beam i n c i d e n t on t h e m a i n g r a t i n g w a s n o t p a r a l l e l t o t he p l a n e of t h e main g r a t i n g ' s Rowland c i rc le , and t h e d e p a r t u r e was a ' f u n c t i o n o f wavelength. P o i n t B is t h e s a g i t t a l focus of t h e p r e d i s p e r s e r : it is a l s o t h e p o i n t a t which t h e main g r a t i n g Rowland c i r c l e i n t e r c e p t s t h e p l a n e o f t h e f i g u r e . The l i n e a t p o i n t B d e f i n i n g t h e e x t e n t o f t h e beam d i v e r g i n g from C is n o t centered w i t h t h e Rowland c i rc le p l a n e , and t h e beam i n c i d e n t on t h e . m a i n g r a t i n g is i n c l i n e d w i t h r . espec t t o t h i s p l ane .

Thus t h e main g r a t i n g is used o f f - p l a n e . F igu re 3.7 ( b ) i l l u s t r a t e s a conven t iona l Rowland ,mounting wi th an o f f -p l ane s l i t s o u r c e ; Fig. 3 . 7 ( c ) shows t h e curved and t i l t e d l i n e image of t h e s l i t t h a t is produced. The a b e r r a t i o n s are exaggera ted and n o t t o s c a l e . When t h e segmented p r e d i s p e r s e r is used, each segment i l l u m i n a t e s t h e main g ra t i . ng a t a s l i g h t l y d i f f e r e n t angle i n such a way t h a t t h e f i n a l image is compressed: however, t h e com- p res sed p o r t i o n s are n o t i n p r e c i s e r e g i s t r a t i o n i n t h e l a t e r a l d i r e c t i o n , a s i l l u s t r a t e d i n F i g . 3 . 7 ( d ) . Hence , t h e s p e c t r a l r e s o l u t i o n is degraded.

F i g u r e 3.8 shows t h e s p e c t r a l r e s o l u t i o n a t t h e f i l m p l a n e as measured from l a b o r a t o r y s p e c t r a . The upper and lower c u r v e s a p p l y , r e s p e c t i v e l y , t o t h e s h o r t and long wavelength r a n g e s of t h e i n s t rumen t . Pho tomet r i ca l ly determined f u l l w i d t h s a t h a l f maximum were used t o ob ta in t h e measured poin , t s . For .compar ison , t h e t h e o r e t i c a l l y a t t a i n a b l e r e s o l u t i o n , a s de r ived from a 3-D ray t r a c i n g computer program, is i n d i c a t e d by t h e so l id l i n e . For t h e most pa r t , t h e spectral r e so lu t ion is 30 ,000 , b u t is decreased t o 2O,OOO a t t h e s h o r t wavelength end because o f t h e o f f -p l ane a b e r r a t i o n s . The s p e c t r a l r e s o l u t i o n of t h e i n s t rumen t achieved d u r i n g f l i g h t agreed w e l l w i th t h e p r e f l i g h t l a b o r a t o r y measurements.

A shortcoming i n t h i s d e s i g n o f a doub le -d i spe r s ion , d u a l p r e d i s p e r s e r spec t rog raph l a y i n t h e u s e of t h e second order of t h e main g r a t i n g i n combination w i t h t h e f i r s t order o f t h e 300-l/mm p r e d i s p e r s e r . The focused s t r a y l i g h t from t h e p r e d i s p e r s e r t h a t included a l l wave- l e n g t h s came t o a v e r t i c a l l i n e a r focus on t h e waveband a p e r t u r e ; t h i s aperture .allowed a s i g n i f i c a n t f r ac t ion t o p a s s through and o n t o t h e main g r a t i n g . ' T h e main g r a t i n g , i n t u r n , b rought t h e long wavelength p o r t i o n of t h e s t r a y l i g h t t o focus i n i ts f i r s t order. The re fo re , t h e desired spectrum, 977-1970 A, w a s o v e r l a i d w i t h a broad, f a i n t spectrum of 1954-3940 A wavelength, whose h e i g h t was determined by t h e waveband aperture. T h i s unwanted spectrum was

of g r e a t e r i n t e n s i t y r e l a t i v e t o t h e XUV f o r s p e c t r a of r e g i o n s on t h e s u n ' s d i s k than f o r p o s i t i o n s close to or above t h e l imb. I t became i n s i g n i f i c a n t a t wave lengths s h o r t e r than 1500 A. The p r e d i s p e r s e r g r a t i n g was r u l e d i n a way t h a t minimized t h e f o c u s e d s t r a y l i g h t .

3.4 Opt ica l , C o a t i n g s

The o p t i c a l s u r f a c e s were c o a t e d t o p r o v i d e t h e maximum r e f l e c t a n c e possible for t h e s h o r t wavelength band and t o r e d u c e t h e speed i n t h e l o n g wave leng th band where t h e s o l a r i n t e n s i t y is so great . F i g u r e 3.9 lists t h e c o a t i n g s on each e l e m e n t and shows . t h e t o t a l i n s t r u m e n t r e f l e c t a n c e , i n c l u d i n g t h e efficiencies of t h e g r a t i n g s .

I n order t o o b t a i n t h e maximum p o s s i b l e e f f i c i e n c y a t t h e s h o r t w a v e l e n g t h s where t h e so la r spectrum is w e a k e s t , t h e 300-l/mm p r e d i s p e r s e r and t h e main g r a t i n g were b l a z e d a t 1200 A. The peak i n t h e i n s t r u m e n t r e f l e c t a n c e a t a b o u t 1300 A shows t h e effect of t h e b l a z e . The sudden decrease i n r e f l e c t a n c e below 1200 A was c a u s e d ma in ly by t h e d e c r e a s i n g r e f l e c t a n c e of t h e magnesium f l u o r i d e : it was e s p e c i a l l y p rominen t b e c a u s e t h e beam was reflected by t h r e e s u c h s u r f a c e s . The minimum a t 2900 A is a c h a r a c t e r i s t i c of t h e m u l t i l a y e r A1-ZnS c o a t i n g .

3.5 Therma l C o n t r o l System

I n order t o m a i n t a i n good f o c u s and t o avo id s m e a r i n g t h e image, t h e o v e r - a l l t e m p e r a t u r e of t h e s p e c t r o g r a p h w a s m a i n t a i n e d between 20.9' C and 21.2' C , and t h e loca l thermal d i f f e r e n c e s were h e l d t o l ess t h a n 0.2' C , a l t h o u g h t h g temperature of t h e ATM canister ranged from 10 27 C and t h a t of t h e ATM spar from 16 ' C t o 21' C. P r i o r t o o i n s t a l l a t i o n i n t h e ATM, t h e i n s t r u m e n t was f o c u s e d a t . 2 1 C . . A c o m b i n a t i o n o f p a s s i v e thermal s h i e l d i n g and a c t i v e thermal c o n t r o l p a n e l s was used t o c o n t r o l t h e over - a l l t e m p e r a t u r e .

C to

P r e v e n t i o n of d i r ec t h e a t i n g by t h e i n c i d e n t solar r a d i a t i o n was accomplished m a i n l y by a mirror t h a t e n c i r c l e d t h e slit p la te . T h i s m i r r o r reflected t h e po r - t i o n of t h e solar image n o t s t r i k i n g t h e s l i t p la te back t o t h e t e l e s c o p e m i r r o r and o u t t h e f r o n t aperture. I n a d d i t i o n , t h e r e was a h e a t r e j e c t i o n m i r r o r s u r r o u n d i n g t h e perimeter of t h e telescope mirror; t h i s reflected o u t t h e f r o n t a p e r t u r e any r a d i a t i o n t h a t o v e r f i l l e d t h e mirror. These hea t r e j e c t i o n mirrors kept d i f f e r e n t i a l h e a t i n g of t h e i n s t r u m e n t at. a minimum, t h u s p r e v e n t i n g s i g n i f i c a n t smear ing of t h e f i n a l image a t t h e f i l m p l a n e d u r i n g l o n g e x p o s u r e s .

3.6 F i l m and F i l m Camera

Kodak Special F i l m t y p e s 104 and 1 0 1 were used. Both are W V s e n s i t i v e Schumann e m u l s i o n s d e p o s i t e d on a t h i c k g e l a t i n pad carr ied on a 7-mil E s t a r base. The g e l a t i n pad between t h e base and t h e e m u l s i o n c o n t a i n e d a yellow a n t i h a l a t i o n d y e t o a b s o r b scat tered solar r a d i a t i o n l o n g e r t h a n 2500 A.

From 1000 A t o 4000 A t y p e 1 0 1 f i l m is a p p r o x i m a t e l y two t o f i v e t i m e s f a s t e r t h a n type 104. H o w e v e r , tests conduc ted pr ior t o t h e S k y l a b m i s s i o n revealed t h a t t y p e 1 0 1 f i l m is d i s p r o p o r t i o n a t e l y more s u s c e p t i b l e t h a n 1 0 4 t o e n v i r o n m e n t a l effects. Therefore, t h e m a j o r i t y of t h e f i l m s t r i p s used i n t h e cameras were of t y p e 104.

When r e c e i v e d from Kodak, t h e f i l m was i n 1 0 0 - f t r o l l s , 70 mm wide. Due t o t h e g r e a t s e n s i t i v i t y t o a b r a s i o n of these e m u l s i o n s , e a c h t u r n on t h e r o l l was separated from its n e i g h b o r s b y ra ised r a i l s t h a t c o n s i s t e d of a band of p o l y s t y r e n e beads secured t o t h e g e l a t i n and placed a l o n g each edge of t h e f i l m . The s t r i p s o f f i l m f o r t h e s p e c t r o - graph, measu r ing 35 mm x 250 mm, were c u t from t h e c e n t e r of t h e 70-mm wide r o l l s and mounted i n f l e x i b l e a n o d i z e d aluminum holders . A c h i p of Kodak Plus-x panchromat i c f i l m was mounted a t t h e end of each h o l d e r t o r e c o r d t h e d i o d e m a t r i x f l a s h e r e x p o s u r e data. Two examples of t h e f i l m s t r i p s and ch ips a re shown i n F i g . 10 . E i g h t so la r spectra and t h e d i o d e a r r a y d a t a e x p o s u r e s c a n be seen on each s t r i p . The top s t r i p is a f l a r e s p e c t r u m i n t h e s h o r t wavelength r e g i o n (970-1970 A). The bot tom i s a l i m b s c a n e x p o s u r e s e q u e n c e c o n t a i n i n g both l o n g a,nd s h o r t wavelength spectra.

The camera car r ied 201 h o l d e r s which were s tacked i n two columns of 100 each, 'one column above t h e o ther . As t h e camera was c y c l e d , t h e p e r i m e t e r of t h e s t r i p t o be exposed was pressed a g a i n s t a ca r r i e r which was shaped t o t h e Rowland c i r c l e focal p l a n e of t h e m a i n g r a t i n g and w a s ' registered t o w i t h i n 0 .1 mm. The carr ier was t r a n s p o r t e d pa ra l l e l t o i ts l o n g dimens.ion i n 3-mm s t eps , t h u s a l l o w i n g e i g h t e x p o s u r e s t o be recorded on each s t r i p . The camera was mounted t o t h e i n s t r u m e n t , a s shown i n F i g . 3.11, by a l a t c h and g u i d e r a i l s y s t e m which p r o v i d e d e a s y i n s t a l l a - t i o n and removal by t h e a s t r o n a u t wh i l e m a i n t a i n i n g a c c u r a t e r e g i s t r a t i o n w i t h t h e focal p l a n e . P r i o r t o b e i n g mounted i n t h e i n s t r u m e n t , t h e camera was s tored i n a sealed c a n i s t e r f i l l e d w i t h n i t r o g e n . A f t e r u s e on t h e i n s t r u m e n t , t h e camera was r e t u r n e d t o t h e canister and sealed w h i l e i n t h e space vacuum.

3.7 I n s t r u m e n t Per formance

The s p e c t r o g r a p h operated w e l l o v e r t h e e n t i r e S k y l a b m i s s i o n . T h e r e were no a n o m a l i e s , e x c e p t those c o n n e c t e d w i t h Schumann f i l m , which are described elsewhere i n t h i s Guide (Sec. 4 ) . One camera was exposed d u r i n g SL-2, two d u r i n g SL-3,' and o n e on SL-4. A t o t a l of 6408 spectra was o b t a i n e d .

I n F i g . 3.12 t h e r e is r e p r o d u c e d a sample s e c t i o n of e i g h t e x p o s u r e s made a t t h e b e g i n n i n g .of t h e f i r s t m i s s i o n . T h i s shows - the 1170-1245 A r e g i o n , less t h a n 1 0 % of t h e e n t i r e c o v e r a g e i n t h e s h o r t wavlength p o s i t i o n . These e x p o s u r e s were made i n t h e automatic limb s c a n mode. Exposures of 160 sec were made be tween t h e w h i t e l i g h t l i m b and -12 sec of arc i n s i d e . The e x p o s u r e s made above t h e l i m b t o +8 sec of arc were four times longer. T h i s l i m b s c a n was c a r r i e d o u t when a n a c t i v e r e g i o n w a s on t h e 1 i m b .

The L y m a n - Q l i n e of hydrogen , 1216 A , is s e e n t o r e a c h greatest i n t e n s i t y i n t h e ch romosphere , 2 s e c o f arc above t h e l i m b . A l l images of it are g r e a t l y overexposed . The p r o f i l e of t h e l i n e is c o n s p i c u o u s ; b r o a d w i n g s , t h e c e n t r a l maximum doub led by d e e p s e l f - r e v e r s a l caused ma in ly by t h e g r e a t o p t i c a l d e n s i t y of t h e s o l a r a t m o s p h e r e a t t h e c e n t e r of t h e l i n e and a l s o by t h e t e l l u r i c hydrogen a b s o r p t i o n core. When o b s e r v e d close t o t h e l i m b , t h e double peaks became so i n t e n s e t h a t t h e i r images were s o l a r i z e d . Between t h e s o l a r i z e d images one c a n see a n e x t r e m e l y n a r r o w non- s o l a r i z e d l i n e ; t h i s is t h e t e l l u r i c a b s o r p t i o n core, whose w i d t h is 0.025 A. The o t h e r c h r o m o s p h e r i c and l o w t r a n s i - t i o n r e g i o n l i n e s , S i 11, S i I n , C 111, N V , m a x i m i z e a t t h e same l imb p o s i t i o n , a p p r o x i m a t e l y , a s does Ly-a..

The b e h a v i o r o f t h e c o r o n a l and h i g h t r a n s i t i o n r e g i o n l i n e s is d i f f e r e n t . For example , Fe X I I , 1242.0 A , is e x t r e m e l y f a i n t on t h e d i s k a t -12 sec o f arc. I t is most i n t e n s e above t h e l i m b and s t a y s i n t e n s e a l l t h e way t o +8 sec of arc above t h e l i m b .

Shown on F i g u r e 3.12 are s e v e r a l l i n e s whose i d e n t i f i - c a t i o n s a r e new*. Mg V I I , 1189.8 A, S X , 1196.2 A and 1213.0 A , S V, 1199.2 A , and Fe X I I I , 1216.4 A. I n o l d e r low d i s p e r s i o n spectra t h e i n t e r s y s t e m l i n e O V , 1218.4 A was b a r e l y v i s i b l e above t h e Lyman-O! wing, much a s is t h e case i n F i g . 3.12 for Fe X I I I , 1216.4 A , which is t h r e e times closer t o Ly- t h a n 0 V.

W i t h i n t h e 1000-A s h o r t wave leng th cove rage of t h e s p e c t r o g r a p h a p p r o x i m a t e l y 4000 l i n e s c a n be r e s o l v e d . Some 50% have been i d e n t i f i e d . I n F i g . 3.12 there are present about 25 u n i d e n t i f i e d l i n e s , m o s t of them w e a k . An e m i s s i o n d o u b l e t of some i n t e r e s t c a n be seen a t 1243.9 A, 1240.4 A, j u s t - t o t h e r i g h t of t h e s h o r t e r cornponent of N V i n t h e e x p o s u r e a t +2 sec of arc. T h i s i s t h e t r a n s i t i o n Mg I1 3s 'S+ - 4p ' a P g l Q t h e f i r s t members of t h e p r i n c i p a l series of Mg If. I n l o n g e x p o s u r e s on t h e d i s k t h e t w o l i n e s are p r e s e n t i n absorption a g a i n s t t h e wing of L y - a ; t h e y are t h e F r a u n h o f e r l i n e s of s h o r t e s t wave- l e n g t h as y e t o b t a i n e d i n t h e so la r spectrum.

----___---- * G. D. S a n d l i n , G. E. B r u e c k n e r , and R. Tousey, Ap . J. -- 214, 898 , 1 9 7 7 , Fo rb idden L i n e s of t h e S o l a r Corona and T r a n s i . t i o n Zone: 975-3OOOA.

F i g u r e C a p t i o n s

F i g . 3 . 1 , The o p t i c a l system o f t h e XUV spec t rograph i n ATM.

Fig . 3.2 The t e l e s c o p e and t h e p o i n t i n g r e f e r e n c e s e r v o system t h a t s t a b i l i z e d t h e s u n ' s image on t h e s l i t ; t h e l o n g dimension of t h e s l i t l i e s i n t h e p l a n e of t h e f i g u r e .

F ig . 3.3 A s t i g m a t i s m of t h e Rowland mounting..

F i g . 3 .4 The pseudoast igmatism of t h e p r e d i s p e r s e r r u l e d w i t h . t e n segments of d i f f e r e n t spac ings .

F ig . 3.5 I l l u m i n a t i o n of t h e main g r a t i n g by t h e t e n paneled p r e d i s p e r s e r f o r d i f f e r e n t wavelengths.

F ig . 3.6 The d e c r e a s e i n l e n g t h o f t h e s p e c t r a l l i n e s achieved by u s e of t h e segmented p r e d i s p e r s e r .

F ig . 3.7 The o f f - p l a n e a b e r r a t i o n s of t h e double-d ispers ion s p e c t r o g r a p h and t h e e f f e c t of t h e segmented p r e d i s p e r s e r .

F ig . 3.8 The spectral r e s o l u t i o n of t h e ATM spec t rog raph , showing p o i n t s p l o t t e d from measurements made p r i o r t o f l i g h t and c u r v e s c a l c u l a t e d w i t h a 3-D r ay t rac ing computer program. The upper s e c t i o n i s for t he sho r t wavelength r a n g e and t h e lower f o r t h e long.

Fig. 3.9 The t o t a l r e f l e c t a n c e of t h e ins t rument , i n c l u d i n g both main and p r e d i s p e r s e r g r a t i n g s and t h e t e l e s c o p e mirror .

F i g . , 3:.10 Photographs of t w o s t r i p s of f i l m exposed by S082B.

Fig . 3.11 The S082B spec t rog raph r e s t i n g on a g r a n i t e b lock and showing t h e thermal c o n t r o l pane l s . The camera is l o c a t e d a t t h e f r o n t c e n t e r o f t h e photograph.

F ig . 3.12 An example of s p e c t r a o b t a i n e d d u r i n g t h e l imb scan mode. The wa.velength r ange i s 1170-1245 A , about 1/10 o f t h e e n t i r e coverage. P o s i t i v e l imb ' p o s i t i o n s ( i n sec of a r c ) r e f e r t o p o s i t i o n s above t h e l imb.

TELEXOPE YIRROS 1 (OFF E U S PARABOLOID)

FiZ! The optical system of the XUV spectrograph in ATM.

Pnnrim nwm

CLASHER

INSTRUMENT

SOLA RAVS

A S I ~ A W T S USPLAI w W*IICUUT w a i l IYX.S 3 ARC U.N VlLLD

SWLCP nul?

~SIROIIWT% OSRAT :or wwn-uva V(XY '

u ) a E y w I ulx a Ynn L e

. . 3 Fig.2. The telescope and the pointing reference servo system that

stabilized the sun's image on the slit; the long dimension of the slit lies in the plane of the figure.

. .

-4 Pig.'b Astigmatism of the Rowland mounting.

a0.L.D CIRCLE

Fi24 T h e pseudoastigmatism of the predisperser ruled with t e r segments of different spacings., .

Fig%. Illumination of the main grating by the ten paneled predis- pemer for different wavelengths.

Fig% The decrease in length of the spectral lines achieved by use of the segmented predisperser.

. . . .-

fb)

. . ROWLAND

--CIRCLE -- :E--. _ _

PLANE I

ldl . I . .

- . . f C )

Fi?? The off-plane aberrations of the double-dispenion Qpectro: graph and the effect of the segmented predisperser.

.~ - . . c y L L w l M luuGSlr)(Yu

.. 3.8 . FigA The spectral resolution of the AThi spectrograph, showing mints plotted from measurements made prior to flight and run= lralculated with a 3-D ray tracing cornpuler program. The u p p e ~ -dun is for the short wavelength range and the !oyer for the Icing.

kb.' The total reflectance-of the instrument, including bothmain 1 1 and predisperser gratings and the telescope mirror.

FILM CHIP

. . .

* 250 mm - r

. .

, SHORT '

END . . WAVELENGTH

3. Fig..10. h

Phatographs of two strips of film exposed by SO82B.

t3 Fig.,,,L. The S082B spectrograph resting on a granite block and showing the thermal control panels. The camera is located at the. . . ' ' .. front center of the photograph.

LONG WAVELENGTH

END

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. . u I l 1 . . I . ' ) < 4 Cm .Sin 12043 Si Dl Ly-0 . .

- . LIMB SCAN ACROSS AR 114-MAY 31,1973 . _ . .

..

"242. An example of spectra obtained during the limb scan mode. The wavelength range is 1170-126 A, about goof the entire coverage. Positive limb positions (in sec of arc) refer to positions above the limb. . .

. . . .

4.0 FILM HISTORY*

Commencing i n 1946, when V-2 r o c k e t s f i r s t made p o s s i b l e e x p e r i m e n t a t i o n from above t h e e a r t h ' s a tmosphe re , t he re h a s b e e n a n i n c r e a s i n g need for p h o t o g r a p h i c f i l m w i t h which t o record t h e XUV s p e c t r u m of t h e s u n . The emuls ion type most s e n s i t i v e t o t h e XUV was i n v e n t e d by Schumann i n 1892 and perfected by 1901. Schumann r e c o g n i z e d t h e f a c t t h a t g e l a t i n is opaque t o t h e XUV. A s a r e s u l t h e deve loped a n emul s ion w i t h j u s t enough g e l a t i n t o h o l d t h e s i l v e r h a l i d e c r y s t a l on t h e base mater ia l , b u t t h e l a y e r of g e l a t i n was so t h i n t h a t it was e f f e c t i v e l y t r a n s p a r e n t t o t h e XUV. T h e s e e m u l s i o n s c o u l d n o t be t o u c h e d w i t h o u t d e s t r o y i n g them.

s e v e r e l y l i m i t e d q u a n t i t i e s . Eastman Rodak was f i r s t t o p r o d u c e a Schumann e m u l s i o n on a f i l m base by machine c o a t i n g . They a l s o deve loped a method of p r e v e n t i n g a b r a s i o n between t u r n s of packaged r o l l s b y c o a t i n g each edge of t h e f i l m w i t h a spacer 0.2 mm t h i c k , c o n s i s t i n g of p o l y s t y r e n e beads he ld down w i t h g e l a t i n . They named t h e new, f a s t emul s ion 101 and produced a s 1 0 4 a slower, b u t f i n e r - g r a i n e d e m u l s i o n h a v i n g t h e beaded s p a c e r s . A l l t he se emuls ions were unpro- tected, hence e x t r e m e l y s u s c e p t i b l e t o a b r a s i o n . A l t h o u g h now n e a r l y f ree from defects, f o g problems and other e f f e c t s have c o n t i n u e d t o ar ise; some are descr ibed i n t h i s G u i d e .

For 50 y e a r s Schumann p l a t e s were made by hand and i n

4 . 1 Batches

The . f i l m s t r i p s r e q u i r e d by t h e XUV s p e c t r o h e l i o g r a p h (S082A) and spectrograph ( S 0 8 2 B ) were 250 mm l o n g and 35 mm wide . To p r o v i d e f o r t h i s s i z e , Eastman Kodak p roduced 1 0 4 and 1 0 1 f i l m s i n spec ia l r o l l s , 70 mm i n w i d t h , and 30 m ( 1 0 0 f t ) i n l e n g t h . The r e q u i r e d s t r i p s were c u t froin t h e c e n t e r . Three r o l l s were s u f f i c i e n t t o p r o v i d e t h e 200 s t r i p s needed for e a c h camera. Ten r o l l s were made from '

o n e batch of emul s ion . S t r i c t c o n t r o l s were r e q u i r e d t o p r o d u c e t h e many b a t c h e s of emul s ion needed t o m a n u f a c t u r e f i l m t h a t was s a t i s f a c t o r y fo r (ATM) e x p e r i m e n t s i n t h e 1 a r g e . q u a n t i t y r e q u i r e d . I n t h e pas t it was n o t uncommon t o f i n d v a r i a t i o n s from batch t o b a t c h , ' a n d even w i t h i n a s i n g l e r o l l , on t h e order of a factor of 2 to 5. Eastman Kodak s 'ucceeded, however, i n improving dramatical ly t h e o v e r - a l l . . q u a l i t y of b o t h 104 and 1 0 1 f i l m s . Large q u a n t i t i e s of t h e s e . f i l m s were produced t h a t were uniform t o a d e g r e e n e v e r p r e v i o u s l y a c h i e v e d ; . t h e y were remarkably f ree from

* M a t e r i a l ' f o r t h i s s e c t i o n has been e x t r a c t e d from a .

paper i n Applied Opt ics , 16,. 887, 1977, by.M. E. VanHoosier , J.-D.. F. B'artoe, G. E. B r u e c k n e f , N. P. P a t t e r s o n , and , R. Tousey. E x p e r i e n c e w i t h Schumann-type XUV F i l m on Skylab . More d e t a i l e d i n f o r m a t i o n a b o u t t h e f i l m may be found i n i n t h a t s o u r c e .

blemishes of a l l k i n d s . G e n e r a l l y , t h e s e n s i t i v i t y t h r e s - h o l d d i d n o t change s i g n i f i c a n t l y w i t h batch o r from place t o place over a r o l l . The maximum d e n s i t y D max and t h e c o n t r a s t var ied be tween ba tches , b u t n o t g r e a t l y . Type 1 0 4 batches h a v i n g D max between 1 . 4 and 1.6 ( a s measured w i t h a G r a n t m i c r o p h o t o m e t e r ) were .accepted f o r u s e i n ATM .

4.2 F i l m Sequence Log

Each of 1 0 cameras exposed fo r e x p e r i m e n t s S082A and S082B d u r i n g Skylab c o n t a i n e d f i l m s t r i p s c u t ' f r o m seve ra l d i f f e r e n t r o l l s , and each camera l o a d of s t r i p s w a s d e v e l o p e d i n s e v e r a l d i f f e r e n t r u n s . A record was kept of t h e --- r o l l of f i l m from which each f i l m s t r i p was c u t , t h e e m u l s i o n -- batch i n which t h a t r o l l was m a n u f a c t u r e d , and t h e --- d e v e l z - --- ment r u n i n which t h e f i l m s t r i p was developed. T h i s rec0r.d is known a s t h e F i l m Sequence Log, and it is rep roduced for S082B . in Appendix C. The e m u l s i o n batch a p p e a r s as t h e second s u f f i x i n t h e . f i l m t y p e number o f e a c h r o l l , i. e.

F i l m Type

1 0 4 - 06 - 05

(Type 104 (7' m i l ( ba t ch 5 ) emu1 s i o n ) Estar

base)

The f u l l complement of f i l m s t r i p s ( a p p r o x i m a t e l y 201) w a s . e x p o s e d i n a l l S082B cameras. Development r u n A was made a s a t es t pr ior t o t h e f u l l t a n k r u n s .

4 .3 Mounting

A major d e s i g n problem i n of b o t h SO82 i n s t r u m e n t s was t h e camera. I t was decided n o t t o attempt t o u s e Schumann f i l m i n r o l l form because of t h e many d i f f i c u l t i e s associated w i t h a b r a s i o n , e n v i r o n m e n t , s t a t i c e l ec t r i ca l . e f f ec t s , and precise r e g i s t r a t i o n of t h e f i l m t o t h e f o c a l s u r f a c e . R a t h e r , each f i l m s t r i p was car r ied i n i t s own metal h o l d e r , and a p p r o x i m a t e l y 200 s t r i p s were h e l d i n each camera.

The d e s i g n of t h e metal ho lder i n v o l v e d t h e c h o i c e o f a s u i t a b l e metal and c o n f i g u r a t i o n s o t h a t , when b e n t i n t o p o s i t i o n , t h e f i l m would l i e p r e c i s e l y on t h e Rowland c i rc le , w i t h i n a t o l e r a n c e of 0.2 mm. An e q u a l l y i m p o r t a n t c o n s i d e r a t i o n w a s t o c h o o s e a mater ia l for t h e h o l d e r s t h a t would not fog Schumann f i l m .

Holders of two t y p e s were used fo r e x p e r i m e n t s S082A and S082B. The f i r s t c h o i c e was 0.25-mm stainless s t ee l which was b e l i e v e d compatible w i t h Schumann f i l m . I t was n e c e s s a r y , however , t o i n c r e a s e i t s s t i f f n e s s for t h e 2 m focal p l a n e r a d i u s o f t h e S082A i n s t r u m e n t by s t a m p i n g f i v e depressed. r i b s l e n g t h w i s e i n t o each h o l d e r ; o t h e r w i s e .

t h e unsuppor t ed area would n o t conform p r o p e r l y t o t h e Rowland c i rc le . As d i s c u s s e d i n a r t i c l e s abou t t h e S082A e x p e r i m e n t , t h e s e g r o o v e s were found t o be a s o u r c e of fog.

The S082B focal p l a n e r a d i u s was o n l y 1 m , and t h e t o l e r a n c e o n c o n f o r m i t y t o , t h e Rowland c i r c l e w a s v e r y t i g h t . For t h i s i n s t r u m e n t t h e h o l d e r s were made of '0.8-mm t h i c k aluminum s h e e t , which was s u f f i c i e n t l y s t i f f and un i fo rm so t h a t r i b s were n o t r e q u i r e d . However , before forming t h e r e t a i n i n g l i p s , it was n e c e s s a r y to r e d u c e by machin ing t h e t h i c k n e s s of t h e aluminum t o be b e n t .

U s e of aluminum f o r f i l m ho lde r s had been a v o i d e d as .

l o n g as poss ib le , b e c a u s e of i t s l o n g h i s t o r y o f f o g g i n g Schumann f i l m , from rocket e x p e r i m e n t s and e x p e r i e n c e i n t h e l a b o r a t o r y . A t es t program was set up t o i n v e s t i g a t e f i l m f o g g i n g b y metals. I t was f o u n d t h a t f r e s h l y machined aluminum d i d , i n d e e d , fog types 104 and 1 0 1 f i l m s ; b u t aluminum, i f c o m p l e t e l y a n o d i z e d , d i d n o t . Therefore, t h e aluminum holders w e r e . t h o r o u g h l y a n o d i z e d a f t e r machin ing and bending . These ho lde r s caused no f o g g i n g o f f l i g h t f i l m . S imilar p r e c a u t i o n s were t a k e n w i t h a l l . pa r t s o f . t h e camera, even though t h e y were n o t l o c a t e d close t o t h e f i l m . B l a c k - anod ized aluminum, made by d y i n g black t h e anod ized layer before it was d r y , was found safe. Magnesium was n o t used because, when c h e m i c a l l y b l a c k e n e d , it produced fog.

F i g u r e 4 . 2 shows a p a r t i a l l y disassembled view of a camera l o a d e d w i t h empty f i l m h o l d e r s . Each camera, . o f which 1 0 were f lown on Skylab, was e x t r e m e l y complex. The q u a s i - c a r r o u s e l d e s i g n allowed t h e loaded ' f i l m holders t o be t r a n s f e r r e d s e q u e n t i a l l y and r a p i d l y i n t o and o u t o f t h e f o c a l p o s i t i o n , from one s tack o f 100 t o t h e o t h e r s t a c k , w h i l e a n o t h e r t r a n s f e r occurred a t t h e back. When a l l t h e h o l d e r s had made t h e c i r c u i t o n c e , t h e camera was f u l l y . exposed . I n f l i g h t , t h e o n l y camera t h a t m a l f u n c t i o n e d was t h e one a c t u a l l y i n place i n t h e S082A i n s t r u m e n t d u r i n g t h e l a u n c h . ,

4 . 4 P r o c e s s i n g t h e F i l m

Over t h e years of u s i n g Schumann t y p e f i l m , and a f t e r c o n s i d e r a b l e a d d i t i o n a l e x p e r i m e n t a t i o n , it was decided t h a t D-19 mixed 1:l w i t h d i s t i l l e d water p r o v i d e s t h e g rea t e s t u n i f o r m i t y , f reedom from chemical fog , and m i n i m u m E b e r h a r d t , edge and a d j a c e n c y e f fec ts . T h e f o l l o w i n g p r o c e d u r e w a s .

adopted t o provide maximum c o n t r o l and uniform q u a l i t y of t h e f l i g h t e x p o s u r e s .

One f l i g h t s t r i p from each m i s s i o n was s e l e c t e d and processed a l o n e a t t h e s t a r t , t o ensure t h a t each r e t u r n e d f l i g h t load had n o t r e c e i v e d d e g r a d a t i o n w h i c h cou ld be corrected by d i f f e r e n t p r o c e s s i n g . The remainder of t h e f i l m was d e v e l o p e d i n batches of 40 f l i g h t s t r i p s and 10 .

l a b o r a t o r y - exposed c o n t r o l s t r i p s . T h e f l i g h t s t r i p s were l e f t i n the i r ho lde r s , t o g e t h e r w i t h t h e Plus-X d a t a c h i p . A l l s t r i p s were a t t a c h e d t o a rack i n a v e r t i c a l p o s i t i o n . The s o l u t i o n s were h e l d i n l a r g e , s t a i n l e s s s teel t a n k s . Each t a n k c o n t a i n e d 4 0 l i t e r s of s o l u t i o n , . a q u a n t i t y c o n s i d e r e d s u f f i c i e n t t o p r o c e s s t h e e n t i r e c o n t e n t s of one camera w i t h o u t d e p l e t i o n .

The rack of 50 f i l m s t r i p s was f i r s t presoaked i n a t a n k of d i s t i l l e d water f o r 4 m i n u t e s . This was a n i m p o r t a n t s t e p b e c a u s e it p r e v e n t e d i n f e c t i o u s development by a l l o w i n g t h e d r i e d - o u t g e l a t i n pad t o swell. O the rwise , w h i s k e r s growing on exposed g r a i n s c o u l d t o u c h a d j a c e n t unexposed g r a i n s , making them developable. Immersion i n t h e water '

was done q u i c k l y , b u t smoo th ly ; i f s t r i p s a r e immersed uneven ly , m a r k s a re produced by t h e stresses of nonuni form s w e l l i n g . All s o l u t i o n s were m a i n t a i n e d a t 2Oo'C. It w a s i m p o r t a n t t o a v o i d e l e v a t e d or chang ing t e m p e r a t u r e s , which would c a u s e r e t i c u l a t i o n o f t h e g e l a t i n pad. Development was f o r 4 min., followed by 30 s e c i n acetic a c i d s h o r t - s t o p , 4 min. i n Kodak acid f i x e r , a 20 min. wash i n f i l t e r ed tap water, removal t o a class 1 0 K c l e a n room, r i n s i n g i n d i s t i l l e d water , and hang ing t o dry .

An i m p o r t a n t p a r t of t h e deve lopment p r o c e s s w a s t h e u s e of N 2 b u b b l e a g i t a t i o n , i n t r o d u c e d through a n a r ray of many small ho les , r o u g h l y 3/4" apa r t , i n a plenum a t t h e bot tom of t h e t a n k . A one second b u r s t of N 2 was produced a t 1 0 sec i n t e r v a l s . I n a d d i t i o n , t h e e n t i r e f i l m rack w a s moved l a t e r a l l y by hand, a l t e r n a t e l y p a r a l l e l and per- p e n d i c u l a r t o t h e f i l m , a t a speed of about 1 cm per sec. T h i s procedure had been found t o produce uniform d e v e l o p - ment.

The f i v e deve lopment r u n s which were required for each camera c o u l d be completed i n o n e d.ay. The development process was c o n t r o l l e d by i n c l u d i n g i n each development t h e 10 c o n t r o l s t r i p s of f i l m from t h e same b a t c h o n wh'ich

a s t a n d a r d series o f _ e x p o s u r e s had been placed 48 h o u r s ea r l i e r . These 2 c m by 10 c m s t r i p s were exposed t o t h e continuum spectrum o f a D 2 lamp, d i s p e r s e d by a McPherson normal- incidence monochromater/spectrograph. The exposure times were 1 and 1 0 sec. The i n t e n s i t y was reduced i n s teps of a f a c t o r of 2 by means of sectored d i s k s , cove r ing t h e r ange of 1:lOO i n t r a n s m i t t a n c e . The s p e c t r a l range .

was 1650 t o 2400 A. Use o f these cont ro l s t r i p s was mainly t o s e r v e a s a check t h a t t h e development w a s t h e same each time it w a s carried ou t . The H - D c u r v e s of c o n t r o l s t r i p s developed i n v a r i o u s runs were found t o ag ree t o - + 0.02 i n l o g E.

F i n a l l y , t h e d r y f i l m s t r i p s , w h i l e s t i l l i n t h e c l e a n room, were mounted between h i g h q u a l i t y g l a s s p la tes of 1.25 mm t h i c k n e s s , which had been a n t i - r e f l e c t i o n coa ted on t h e i n s i d e surfaces t o minimize Newton's r i n g s . The f i l m s t r i p . was surrounded w i t h a brass spacer, o f t h i c k n e s s s l i g h t l y .

g r e a t e r t h a n t h e f i l m . T h i s , t o g e t h e r w i th t h e normal c u r l , p reven ted t h e emulsion from be ing touched by t h e g l a s s . The sandwich was t h e n sealed w i t h p l a s t i c tape and s tored i n a v a u l t .

4 .5 Loss of D m a x and Contras t

An unexpected f i l m effect w a s a r educ t ion i n D,,,, and c o n t r a s t o n a l l of t h e f l i g h t f i l m , appa ren t ly d u e t o pro- longed exposure t o t h e hard vacuum i n space. F i g u r e 4 . 2 shows a comparison between t h e charac te r i s t ic c u r v e s Eor Types 1 0 1 and 104 f l i g h t f i l m and those f o r f i l m samples from t h e same e m u l s i o n batch k e p t a t 2' E s p e c i a l l y conspicuous is t h e l o n g , f l a t maximum on t h e f l i g h t f i l m . T h i s is followed by a sudden turn-down caused by s o l a r i z a t i o n , for ex t remely h igh exposures ( t y p i c a l of s o l a r f l a r e s ) . These c u r v e s show t h a t there was no l o s s i n t h r e s h o l d s e n s i t i v i t y . F i l m s tored for an extended p e r i o d under vacuum i n t h e l a b o r a t o r y d i d n o t show t h i s e f fect . That t h e loss w a s due t o a c a u s e other t h a n degrada t ion of t h e l a t e n t image was shown by s e n s i t o m e t r i c t e s t s made pos t - f l i g h t on unexposed s t r ip s of f l i g h t f i l m . '

C i n t h e l a b o r a t o r y .

4 . 6 Fog

Fog l e v e l s expected from t h e p r o t o n f l u x d i d n o t m a t e r i a l i z e i n f l i g h t . I t had been r e a l i z e d t h a t t h e fog p r e d i c t i o n was n o t t o o c e r t a i n , t h e r e f o r e a s i n g l e s t r i p of t y p e 101 f i l m w a s i n c l u d e d as a test i n most cameras on SL-2 and 3. The p r o t o n fog l e v e l f o r type 1 0 4 f i l m was n e g l i g i b l e and for type 1 0 1 o n l y 0.02. The e x p l a n a t i o n a p p e a r s t o be t h a t t h e p r o t o n f l u x from t h e South A t l a n t i c anomaly was much less t h a n was expec ted , and also t h a t t h e s h i e l d i n g provided by t h e Skylab was more e f f e c t i v e than c a l c u l a t e d . Furthermore, h i g h tempera tures were never

exper ienced . N o fogging of t h e f i l m occurred d u e t o i o n s , metal l ic surfaces , or contaminat ion .

Ther.e was i n s u f f i c i e n t time t o i n c l u d e any type 1 0 1 f i l m i n cameras resuppl ied i n SL-3. However, some w a s i n c l u d e d i n t h e cameras f o r SL-4. The f i v e times g r e a t e r s e n s i t i v i t y made p o s s i b l e s e v e r a l i n v e s t i g a t i o n s . I t permitted r e c o r d i n g co rona l s p e c t r a t o g r e a t e r a l t i t u d e s above l imb t h a n w a s p o s s i b l e w i t h t y p e 1 0 4 . Through its u s e t h e p r o f i l e o f hydrogen Lyaras emi t ted from t h e ex tended hydrogen c loud sur rounding t h e comet Kohoutek was photographed , and it .ex tended t o s h o r t e r wavelengths t h e s p e c t r a l coverage of S082B. T h i s successful u s e of type 101 was, however, a t t h e expense of added r i s k o f fogging, reduced accuracy of c a l i b r a t i o n , and increased g r a n u l a r i t y .

F i g u r e Cap t ions

F ig . 4 .1 A photograph o f a loaded and p a r t i a l l y d i sa s sembled camera. c a n be seen . The c l o s e d s h u t t e r is seen i n t h e p l a t e a t t h e r i g h t . A l l t h e a c t u a t o r mechanisms were l o c a t e d a t t h e s i d e s .

O n l y - t h e upper s t a c k of 100 f i l m h o l d e r s

F ig . 4 . 2 T y p i c a l c u r v e s of d e n s i t y vs log exposure f o r Eastman Kodak t y p e s 101 and 104 f i l m . One s e t a p p l i e s t o f i l m t h a t had been exposed to t h e space vacuum d u r i n g S k j l a b , w h i l e t h e other is f o r c o n t r o l f i l m k e p t a t 2 C i n t h e l a b o r a t o r y . The e x t e n s i o n of t h e t y p e 104 c u r v e t o large va. lues o f exposure shows t h e s o l a r i z a t i o n r e sponse , as e s t ima ted .

+I. Fig. L A photograph of r loaded and partially disassernbled'%DS3g camera. Only the upper stack of 100 film holders can be seen. The closed shutter is seen in the plate at the right. All the actuator

mechanisms were located a t the sides. . . . -

_____.._ . . - - . . . I _' !. . i

. . . . . . I . .

21) - t CONTP5I. IQ-05-D . 3 - Ir

0

ul - . rL io I i cu-os-Io

CONTROL in-06-05 . s -

t ul z

I . 2 EXPOSURE (Log

OO

'4.- . '

'Fig. % i d curves of density vs I c g exposure for Eastman Kodak types 101 and 104 film. One set applies to film that had been e x p d to the spacevacuum duringskylab, while the other is for control film kept at 2OC in the laboratory. The extension of the type 104 curve

to large values of exposure shows the snlarization response, as '

. . . estimated.

5.0 CALIBRATION AND ABSOLUTE SPECTROPHOTOHETRY*

Accuracy of c a l i b r a t i o n of i n s t r u i n e n t a t i o n used i n t h e extreme u l t r a v i o l e t has always been a problem of g r e a t d i f f i c u l t y . E a r l y i n t h e ATM program it was proposed by HCO and by NRL t h a t . t h e i r i n s t r u m e n t s be ca l ibra ted by comparison w i t h c a r e f u l l y s t a n d a r d i z e d i n s t r u m e n t a t i o n flown i n rockets. One c a l i b r a t i o n r o c k e t (CALROC) f l i g h t per mis s ion for each i n s t i t u t i o n - w a s cons ide red to be t h e minimum r e q u i r e d because t h e s e n s i t i v i t y of t h e AT# i n s t r u - ments was expec ted t o change d u r i n g t h e course of t h e n i n e months ove r which t h e y would be used. The fundamental idea was t o make s imul t aneous solar measurements u s ing bo th rocket-borne and ATM ins t rumen t s . Abso lu te i n t e n s i t i e s d e r i v e d from t h e well-calibrated rocket i n s t r u m e n t s would t h e n serve t o c a l i b r a t e ' t h e sun so t h a t it could serve a s a s t a n d a r d source w i t h which t o c a l i b r a t e - t h e ATM ins t rumen t s .

The p l a n of NRL w a s t o f l y in s t rumen t s . almost e x a c t l y l i k e t h o s e of ATPI b u t reduced i n s i z e by a factor of two. The ATM s p e c t r o g r a p h could o p e r a t e i n e i t h e r of t w o wave- . l e n g t h ranges: 970-1.940.A, or 1940-3940A. I n the l a t t e r ,

&&n'well"determined' by' Tousey e t a1 (1) and by Broadfoot ( 2 ) . Therefore t h e CALROC ins t rumen t cou ld be s implif ied and improved over t h e AT&! i n s t r u m e n t by e l i m i n a t i n g ' t h e l o n g wavelength r ange and u t i l i z i n g bo th t h e main and pre- d i s p e r s e r g r a t i n g s i n t h e f i r s t order. I n t h i s manner s t r a y l i g h t which 4as present i n t h e ATM ins t rumen t was e l i m i n a t e d from t h e CALROC ins t rumen t .

' drlz'~'".long:~wav~lcngthn.-.,~~rige,-. absoIut'e"int;,ensit ies . had ' a l r e a d y

NRL, t o g e t h e r w i t h B a l l Brothers Research Corpora t ion (BBRC)]Goddard Space F l i g h t Center ( G S F C ) ) and the A m e s Research Cen te r , deve loped a command sys t em by which t h e i n s t r u m e n t a t i o n s e c t i o n of t h e rocket, a f t e r s e p a r a t i o n from t h e booster, cou ld be p o i n t e d a t p a r t i c u l a r p o s i t i o n s . on t h e sun. T h i s was done by a r a d i o command l i n k combined w i t h a t e l e v i s i o n system which d i s p l a y e d t o the P I on t h e ground an €+&image of t h e sun reflected from the slit plate of t h e s p e c t r o g r a p h . By command loop t h e PI cou ld t h e n o r i e n t t h e slit p r e c i s e l y du r ing t h e f l i g h t t o any d e s i r e d so la r f e a t u r e .

The CALROC program r e q u i r e d a g r e a t e f f o r t , b u t t h e results proved t o be h i g h l y s u c c e s s f u l . I n t h e remaining

b-

L,

* Material for t h i s S e c t i o n h a s been g a t h e r e d from h e l p f u l d i s c u s s i o n s w i t h D r s . K. R. Nicolas, 0. Kje ldse th Moe, N. P. P a t t e r s o n , J. W. Cook, G. A. Doschek, a n d U. Peldman. P o r t i o n s of m a t e r i a l have been e x t r a c t e d from References 3, 5, 6 , 7 , and 8, , l i s t e d a t t he end of t h i s Sec t ion .

p a r a g r a p h s of t h i s S e c t i o n , methods of ob ta in ing absolute so la r i n t e n s i t i e s from t h e ATM da ta a re d iscussed . F i r s t t h e CALROC i n s t r u m e n t and t h e method used for its absolute c a l i b r a t i o n i n t h e l a b o r a t o r y are described. Reduct ion of .

t h e CALROC solar exposures t h e n gave absolute solar i n t e n - . s i t i es , which were p u b l i s h e d i n a s p e c t r a l a t l a s for t h e r a n g e 1175 t o 2100A ( 3 ) . By comparison of i d e n t i c a l spectral f e a t u r e s measured by CALROC and ATM, a wavelength-dependent a b s o l u t e s e n s i t i v i t y p lo t was produced for t h e ATM spectro- ' g r a p h du r ing t h e second Sky lab mis s ion . A method which c a n be used t o t r a n s f e r t h i s c a l i b r a t i o n t o other f i l m batches and other Skylab m i s s i o n s is t hen p r e s e n t e d . Also i n c l u d e d is a d i s c u s s i o n of p r e c a u t i o n s t o be observed i n t h e photometry of t h e ATM f i l m . F i n a l l y , t h e method and i n s t r u m e n t a l r e s p o n s e cu rve needed t o o b t a i n ' abso lu t ' e i n t e n s i t i e s from t h e long wavelength ATM data are p rov ided .

5.1 CALROC C a l i b r a t i o n

CALROC f l i g h t s were made on J u n e 13, 1973, Sept. 4 , 1973 and Jan . 15, 1974. The c a l i b r a t i o n ins t rument , f lown on a B l a c k B r a n t VC rocket, was a 1/2 scale'model of t h e ATM S082B spectrograph and used a 1 m focal l e n g t h o f f - a x i s parabol ic mirror t o focus a so l a r image o n t o t h e s p e c t r o g r a p h

w i t h s l i g h t l y v a r y i n g g r a t i n g . c o n s t a n t (average 200 l i n e s mm &l ) , formed a dispersed inage of ' t h e slit on a s l o t which selected t h e wavelength band t o be recorded and blocked a l l v i s i b l e l i g h t from s t r i k i n g t h e main g r a t i n g (2150 l i n e s '

mm - l ) , which w a s mounted i n a Rowland c o n f i g u r a t i o n . Both g r a t i n g s were used i n t h e f i r s t order; t h i s e l i m i n a t e d s t r a y l i g h t which was p r e s e n t i n t h e ATM ins t rument . (See Sec. 3.3). The f i l m s t r ips on t h e Rowland c i rc le were 200 mm l o n g and ,

covered t h e spec t rum from 1170 t o 2100 A with a d i s p e r s i o n of ' 4 . 7 A mm and a spectral r e s o l u t i o n of 0.07A, closely com- parable t o t h e ATM s p e c t r o g r a p h (See Sec. 3).

,,.s_lLi:t _- :,Beh i nd 3. he __ e n .._.. t E9sc.e;: .,- .--- &-- : . s 1: i-t. : w a s -:;.a- .:d:Ou.b le:.: dl.s.p . . . . . e. r-eioo -:- -. >-: L1 .._A .. . . -' .: : specfr.ograph...." . A. 'pr;e'&lsperser g r a t i n g , f c b n s i s t i n g ;.of :panels

An a b s o l u t e c a l i b r a t i o n of t h e CALROC spec t rog raph was made i n t h e l a b o r a t o r y u t i l i z i n g a s t a n d a r d d e u t e r i u m (D-) lamp c a l i b r a t e d as a f u n c t i o n of wavelength between 16.5OA and 2600 A a t t h e N a t i o n a l Bureau of S t a n d a r d s (NBS) before and a f t e r t h e f l i g h t s . For s h o r t e r wavelengths t h i s s o u r c e c a n n o t be used as a s tandard because of the appearance of numerous D2 molecular l i n e s . Between 1250 A and 1700 A a r e l a t i v e spectral c a l i b r a t i o n was . o b t a i n e d a f t e r t h e f l i g h t u s i n g a h i g h pressure argon arc a s an i n t e n s i t y s t a n d a r d (Br idges and O t t , ( 4 ) ) . By matching t h i s relative c a l i b r a t i o n from t h e a rgon arc t o t h e deu te r ium lamp absolute c a l i b r a t i o n above 1700 A, it w a s t h e n possible t o ex tend the a b s o l u t e ca l ib ra t ion of t h e rocket i n s t r u m e n t t o 1250 A. A deta i led d e s c r i p t i o n of t h e deu te r ium lamp c a l i b r a t i o n is g i v e n by Brueckner e t a l . (5 ) , w h i l e K j e l d s e t h BIoe et a l . (3) have descr . ibed t h e a rgon a rc c a l i b r a t i o n .

Spectra of t h e d e u t e r i u m lamp were exposed by t h e i n s t r u m e n t before and a f te r each f l i g h t t o d e t e c t any change i n i n s t r u m e n t s e n s i t i v i t y . I n a d d i t i o n , segments of t h e lamp spectrum were p laced on each s t r i p of t h e f l i g h t f i l m p r i o r t o f l i g h t t o minimize e r ro r s r e s u l t i n g from f i l m inhomogenei t ies , development problems, and f i l m environment d u r i n g f l i g h t . These segments were exposed w i t h t h e f l i g h t i n s t rumen t , u s ing a 1 m o f f - a x i s pa rabo la as a c o l l i m a t o r . S h o r t of i n - f l i g h t c a l i b r a t i o n , t h i s method was as close as p o s s i b l e t o an idea l c a l i b r a t i o n for i r r a d i a n c e measurements. The on ly op t i ca l e lement which had t o be measured independ- e n t l y was t h e collimator mirror. Care was t a k e n t o assure t h a t t h e i l l u m i n a t i o n of a l l op t ica l elements of t h e f l i g h t i n s t rumen t was i d e n t i c a l d u r i n g t h e ca l ibra t ion and t h e solar exposures.

The f i l m character is t ic c u r v e s r e l a t i n g f i l m d e n s i t y above fog l e v e l t o r e l a t i v e exposure were cons t ruc t ed from a series o f f l i g h t exposures i n t h e manner described i n Sec. 5.3.1. Fig. 5.1 g i v e s an example of t h e CALROC charac te r i s t ic curve .

A b s o l u t e s o l a r i n t e n s i t i e s d e r i v e d from the CALROC program for u s e i n t h e ATM c a l i b r a t i o n have been publ i shed a s "A Spectral At las of t h e Sun between 1175 and 2100 A" ( 3 ) , d e s c r i b e d i n more d e t a i l i n Sec. 8. The data have a lso been used. . i n v a r i o u s o t h e r .s . tudies of t h e sun , . which are. . l i s t e d . . .. i n t h e Bib l iography, Appendgx. D..

5:'2 ATM C a l i b r a t i o n

CALROC e s s e n t i a l l y cal ibrated t h e sun , making it a secondary s t a n d a r d source. A s n e a r l y as possible t h e CALROC ins t rumen t observed t h e same r e g i o n s a s the ATM, a l though a t a t i m e which was a f e w hour s away from t h e ATM obse rva t ions . The accu racy a t t a i n e d i n p o i n t i n g both ins t ruments , t o g e t h e r w i t h t h e closeness i n times of o b s e r v a t i o n , made t h e C a l i - b r a t i o n of t h e ATM i n t e n s i t i e s from CALROC.both simple and accurate. Only a , d i r ec t t r a n s f e r of i n t e n s i t i e s from t h e CALROC spectra t o t h e ATM spectra was involved , w i thou t t he need t o consider t h e p o s s i b i l i t y of changes i n ins t rument or f i l m s e n s i t i v i t y .

' The in s t rumen t s e n s i t i v i t y cu rve derived from a com- p a r i s o n of ATM and CALROC exposures is presented i n F i g . 5.2. (K je ldse th Moe and Nicolas ( 6 ) and Nicolas ( 7 ) ) . The loga r i thm of exposure, E, (=I t ) is p lo t ted vs. wavelength. Absolu te u n i t s on t h e o r d i n a t e scale a r s gfvenlinlterms - of t h e i n t e n s i t y , I , of t h e s o u r c e i n e r g s cm- s sr- A- r e q u i r e d to produce an exposure .o f d e n s i t y 0.30 i n 1 sec. Above 1500A t h e cu rve w a s de r ived from measurements o f ' t h e continuum and a l s o of emis s ion l i n e s from n e u t r a l and s i n g l y ionized atoms.

Below 1500 A, on ly l i n e s from n e u t r a l and s i n g l y

I n a d d i t i o n , t h e ca l ib ra t ion curve has been modified

i o n i z e d species were used ( 7 ) .

t o i n c o r p o r a t e more accurate data ob ta ined from a r e f l i g h t of t h e CALROC ins t rument on O c t . 22, 1976. A t t h a t t i m e , t h e a rgon arc had become a v a i l a b l e a s a c a l i b r a t i o n source, and measurements of t h e arc i n t e n s i t y were made close to t h e da t e of f l i g h t , bo th before and a f t e r launch.

For photometry on t h e l i n e a r p a r t of t h e f i l m character- i s t i c curve, ' a s described i n Sec. 5.3.1, t h e estimated accurac of i n t e n s i t y measurements d e r i v e d from t h e d a t a of Fig. 5.2 is 50% rms. The u n c e r t a i n t i e s i n t h e f i l m c h a r a c t e r i s t i c cu rve , i n t h e o r i g i n a l d e u t e r i u m lamp c a l i b r a t i o n , i n t h e r e l a t i v e c a l i b r a t i o n w i t h t h e argon a r c , and i n t h e t r a n s f e r of t h e rocket c a l i b r a t i o n t o t h e ATM ins t rumen t a l l c o n t r i - b u t e t o t h e t o t a l error .

An independent c a l i b r a t i o n of t h e sho r t wavelength ATP! da ta has been pub l i shed by Doschek, Feldman, VanHoosier, and Bartoe (8). They compared a r b i t r a r y continuum i n t e n s i t i e s o b t a i n e d from t h e Skylab spectra w i t h t h e absolute i n t e n s i - t i e s a t s u n c e n t e r i n t h e q u i e t s u n continuum publ i shed by Samain e t a l . ( 9 ) . From t h e comparison they de r ived conver- s i o n factors- t o place the%% l i n e intensitiesron-an-absolute scale. T h e i r i n t e n s i t i e s t h u s conver ted t o a b s o l u t e v a l u e s a g r e e w e l l w i t h t h e spectral i n t e n s i t i e s der ived from Fig . 5.2 between 1400A and 1700A. Above 1700A t h e values agree t o w i t h i n a fac tor of 2 , w i t h Doschek e t a l . h igh by a fac tor of about 1.8 a t 19OOA.

B e l o w 1400A, where t h e ATM continuum became too w e a k t o measure, Doschek e t a l . made u s e of t h e r e f l e c t i v i t y curve for t h e S08'2B i n s t rumen t (10 ) for t he i r de t e rmina t ion of con- v e r s i o n f a c t o r s . Absolute v a l u e s for the i r i n t e n s i t i e s i n t h i s spectral range l i e below t h e CALROC c a l i b r a t i o n by a t most a factor of 2.

5.3 Photometry of S082B Spectra

A l l i n t e n s i t y measurements of t h e S082B da ta of NRL have been de r ived from s p e c u l a r d e n s i t y measurements of t h e f i l m made w i t h a G r a n t microdensitometer, ope ra t ed under c o n t r o l of a PDP-8 minicomputer. Various members of t h e s t a f f have developed i n d i v i d u a l methods and computer programs for reducing t h e data. I n v e s t i g a t o r s a n a l y s i n g t h e spectra may wish t o make c o l l a b o r a t i v e arrangements t o u t i l i z e . t h i s e x p e r t i s e .

5.3.1 Gharacter is t ic Curves

The f i l m character is t ic c u r v e s m u s t be constructed from t h e f l i g h t exposures . The method c o n s i s t s of com- p a r i n g f i l m d e n s i t i e s above fog l e v e l a t e x a c t l y t h e same wavelengths on exposures t aken w i t h d i f f e r e n t exposure times b u t a t t h e same p o i n t i n g . Spectral f e a t u r e s a r e selected t o cover a wide range of i n t e n s i t i e s . T h u s many se t s of f i l m d e n s i t i e s vs. exposure a r e obta ined . The c u r v e of d e n s i t y vs. l o g exposure ( log E) is s y n t h e s i z e d by s l i d i n g t h e many sets of p o i n t s independent ly a l o n g t h e l o g E a x i s u n t i l a best f i t t o an average curve is obtained, The method assumes t h a t a possible reciprocity f a i l u r e is small and c a n be d i s r e g a r d e d . The assumption is v a l i d i n .

g e n e r a l for exposure times w i t h i n a factor of 1 0 of o n e ano the r . Exposures f a r the r apart m u s t be i n v e s t i g a t e d on an i n d i v i d u a l basis. The c u r v e should be normalized t o a s t a n d a r d p o s i t i o n of l o g E = 0.00 a t D = 0.30 f o r a 3. sec exposure i n order t o m a k e direct u s e of t h e absolute cal i - b r a t i o n data of Fig. 5.2, as described i n Sec. 5.3.2 below.

F i g u r e 5.3 shows two r e p r e s e n t a t i v e H&D c u r v e s deve loped i n the above manner for t h e wavelength r e g i o n s s h o r t e r and l o n g e r t h a n 1400 A. I t w a s found from examinat ion of s m a l l wavelength i n t e r v a l s t h roughou t the s p e c t r a l r a n g e _,.._ Yhag . -for t h e s e ' . p a r ~ _.. t i cu l a r : . exposures , ..f;$p ::one "fklm * . ,.-. bqtch; and::development. ?uh, " t h e r e . w a s 'a 'continirous' t r a n ' s f t i o b " in t he slope of t h e q u a s i l h e a r p a r t of t h e C h a r a c t e r i s t i c c r u v e w i t h i n c r e a s i n g wavelength. Other f i l m - b a t c h and development r u n s have n o t a lways shown t h i s .

I n de ' r i v ing t h e AT14 characterist ic c u r v e s , a t t e n t i o n . must be paid to t h e f i l m b a t c h number and development run. For t h i s purpose t h e " F i l m Sequence Loga g iven in Appendix C lists each f i l m s t r i p or "plate," and t h e batch number of t h e f i l m r o l l from which t h e s t r i p w a s c u t . Also i n c l u d e d is t h e development run i n which t h e f i l m w a s developed. The characteristic c u r v e s may va ry w i t h each of these parameters. (See Sec. 4 for a d i s c u s s i o n of the ATM f i l m ) . For one batch and development run it is of ten p o s s i b l e t o cove r t h e r ange 1175-1960 A w i t h two c u r v e s , for wave leng ths above and below 1400 A, r e s p e c t i v e l y . The shape of t h e s e character is t ic c u r v e s is similar for a number of b a t c h number and development r u n s , b u t can d i f f e r and should be examined. There is no " s t anda rd" characterist ic curve .

\

Scatter of t h e data p o i n t s abou t t h e f i n a l curves o b t a i n e d u s i n g t h e above method v a r i e s cons ide rab ly , depending t o some e x t e n t on t h e s p e c t r a l w i d t h of t h e band from which t h e p o i n t s are s e l e c t e d . There is u s u a l l y i n c r e a s e d scatter a t f i l m d e n s i t i e s below a b o u t 0.05 above fog level, t h e toe r e g i o n of t h e curve, and a lso i n t h e s h o u l d e r of t h e curve. Photometry i n t h e s e ranges s h o u l d be avoided , i f a t a l l possible.

6 5 . 3 . y Conver s ion t o A b s o l u t e I n t e n s i t y

The a b s o l u t e i n t e n s i t y , IA s, fo r any exposure E, (= I t ) , a t any w a v e l e n g t h , A , is found prom t h e r e l a t i o n s h i p

l o g I A b s ( A ) = log E A b s ( A ) - log t + d o g E r e l o (5 .1 )

Log EAbs v a l u e s a re read from Fig . 5.2. v a l u e s which m a k e a c o n v e n i e n t t a b l e for computer u s e have a l s o been l i s t e d i n Table 5.1. p o s u r e c o r r e c t i o n required t o take i n t o a c c o u n t t h e ac tua l measured d e n s i t y of. t h e p a r t i c u l a r feature . I t is read d i - r e c t l y from t h e H-D c u r v e which is n o r m a l i z e d f o r log E = 0.0 a t D = 0.3. Exposure t i m e is t.

S e v e r a l o f t h e

Delta l o g Erel i s t h e l og ex-

To i l l u s t r a t e t h e method, Table 5.3 l ists v a l u e s f o r t h e l o n g wave leng th r e l a t i v e c h a r a c t e r i s t i c c u r v e of Fig. 5.3. A f i l m d e n s i t y of 0.4 a t 1500 A on a n e x p o s u r e of 1 0 sec wou ld g i v e a n a b s o l u t e i n t e n s i t y whose l o g is 4.891- 1 .0 0+0 238. The a b s o l u t e i n t e n s i t y is t h e n 1 .35 x l o 4 e r g s cm-9 s-1 sr-1 A-1.

5.4 Slew C a l i b r a t i o n s and V a r i a t i o n s i n t h e ATPI S e n s i t i v i t y Curve

. . . . . :Sp+ci&i .:.*ax ibr'st.ipn: e&p&sbres...bnde.r;- c o h d i t Ions:- 5s'.

n e a r l y i d e n t i c a l a s p o s s i b r e ' were programed dur-ing' t h e S k y l a b m i s s i o n s t o a i d i n ' e v a l u a t i n g : t h e s e v e r a l i n s t r u - m e n t a l ' p a r a m e t e r s ' which were susceptible t o v a r i a t i o n w i t h t i m e . These i n c l u d e t h e a b s o l u t e s e n s i t i v i t y of t h e f i l m and t h e r e f l e c t i v i t i e s of t h e op t i ca l surfaces. The exposures were programed e v e r y s e v e r a l d a y s and were made w i t h t h e ATM s p e c t r o g r a p h p o i n t e d t o a q u i e t r e g i o n 300" i n s i d e t h e so l a r l i m b ( p =0.73) . The i n s t r u m e n t was s l e w - e d back and f o r t h i n a d i r e c t i o n p e r p e n d i c u l a r t o t h e s l i t l e n g t h t o a v e r a g e o u t f l u c t u a t i o n s a l o n g t h e s l i t and t h e r e b y c o v e r e d a q u i e t solar area of o n e square a rc min. o n a r e g u l a r basis. Throughout t h e m i s s i o n o t h e r e x p o s u r e s u s e f u l a s c h e c k s on t h e a b s o l u t e c a l i b r a t i o n were made a t q u i e t r e g i o n p o i n t i n g s 12" and 25" i n s i d e t h e limb, where i n s t r u m e n t a l s t r a y l i g h t was low.

A l i s t i n g of t h e s l e w e x p o s u r e s is g i v e n i n Tab le 5.2, which is o r g a n i z e d by f i l m groups. P la tes from a common '

f i l m b a t c h , r o l l , and development are l i s t e d , t o g e t h e r oppo- s i t e columns c o n t a i n i n g t h e i d e n t i f i c a t i o n numbers of t h o s e parameters. Se r i a l numbers of t h e plates c o n t a i n i n g s l e w e x p o s u r e s and t h e day of y e a r d a t e of t h e exposures a re g i v e n opposite t h e ' g r o u p o f p l a t e s w i t h i n which they are found. A more detai led l i s t i n g , which i n c l u d e s exposure frame and e x p o s u r e t i m e , is a v a i l a b l e among t h e Skylab documents a t NRL.

C. Y. Yang, N. P. P a t t e r s o n , and 0. K j e l d s e t h Moe have made a t h o r o u g h s t u d y of t h e slew e x p o s u r e s o n 1 0 4 f i l m (11). They found t h a t t h e most c o n s i s t e n t i n f o r m a t i o n was o b t a i n e d from d e n s i t o m e t e r s c a n s of con t inuum a r e a s between 1914 a n d 1956A, which were almost c o m p l e t e l y f ree of scat tered l i g h t . S c a n s of e m i s s i o n l i n e s were d i f f i c u l t t o e v a l u a t e b e c a u s e of v a r i a t i o n s i n t h e amount of ne twork ce l l s or bound- a ry areas i n c l u d e d i n t h e s lewed r e g i o n . O t h e r d i f f i c u l t i e s e n c o u n t e r e d w i t h t h e s l e w e x p o s u r e s i n v o l v e d t h e manual con- t r o l of t h e e x p o s u r e s , w i t h e r rors up t o + 1 /4 sec. a t t h e b e g i n n i n g and end of a n e x p o s u r e . A "worst case" error was o b s e r v e d for 2 e x p o s u r e s t a k e n on t h e same day by t h e same a s t r o n a u t , d i f f e r i n g i n r e l a t ive e x p o s u r e by 44%. Three d a y s l a t e r t h e same c o n d i t i o n s registered a r e l a t i v e e x p o s u r e d i f f e r e n c e of o n l y 20%. A p l o t i n c l u d i n g t h e slew measure- m e n t s from a l l m i s s i o n s shows t h a t v a r i a t i o n s i n e x p o s u r e were w i t h i n + 258, and t h a t no s i g n i f i c a n t d e g r a d a t i o n of t h e i n s t r u m e n t o r opt ics c o u l d be detected.

From Table 5.2 it may be n o t e d t h a t each of t h e cameras u s e d w i t h t h e S082B i n s t r u m e n t c o n t a i n e d f i l m from o n l y one ba tch , and t h a t each camera c o n t a i n e d a d i f f e r e n t batch. A l - though no d i f f e r e n c e s i n t h e s l e w c a l i b r a t i o n s were n o t e d which might correlate to batch, r o l l , or development r u n , s e v e r a l i n v e s t i g a t o r s have n o t i c e d v a r i a t i o n s i n D, . and c o n t r a s t when H-D c u r v e s have been p l o t t e d . recommended t h a t t h e a b s o l u t e . v a l u e of t h e s e n s i t i v i t y . c u r v e ..

of Fig . 5 .2 'be ,checked a t o n e or.more wave leng ths .

compar ing a b s o l u t e i n t e n s i t i e s d e r i v e d from s e l e c t e d r e g i o n s of slewed spectra closest t o t h e spectra b e i n g interpreted .

w i t h v a l u e s c o n t a i n e d i n t h e CALROC spectral a t l a s p u b l i s h e d by K j e l d s e t h Moe e t a l . (3 ) . From t h e comparison, a cor- r e c t i o n factor for Fig. 5.2 a t o n e or more w a v e l e n g t h s c a n be o b t a i n e d . Assuming t h a t f i l m s e n s i t i v i t y r e m a i n s u n i f o r m w i t h w a v e l e n g t h t h r o u g h o u t t h e S k y l a b m i s s i o n s , t h e e n t i r e c u r v e f o r Fig. 5.2 c a n t h e n be s h i f t e d t o match t h e corrected p o i n t s . ' T h e best spectral r e g i o n s t o use for t h e c o m p a r i s o n measurements l i e above 1850A or below 1500A, where where t h e f i r s t order s t r a y l i g h t is minimum. (See Sec. 3.3 for a d i s c u s s i o n of t h e s t r a y l i g h t . ) Above 1950A there is a m i x t u r e of cont inuum, a b s o r p t i o n and e m i s s i o n f e a t u r e s , w h i l e below 1500A, o n l y e m i s s i o n l i n e s are a v a i l a b l e . Al though i n p r i n c i p l e o n l y o n e r e g i o n n e e d s t o be checked, i t is u s e f u l t o compare s e v e r a l i n order t o o b t a i n an estimate of t h e e r ror i n c a l i b r a t i o n .

I t is. #erefore

The a b s o l u t e s e n s i t i v i t y c u r v e c a n be checked by

5.5 C u r v a t u r e of Spectra

Both t h e ATM and t h e CALROC spectra a re bowed a l o n g t h e d i s p e r s i o n , t h e e n d s of each s p e c t r u m l i n e d e v i a t i n g s e v e r a l hundr.ed micrometers from a t a n g e n t t o t h e middle p o s i t i o n . To e n s u r e t h a t t h e photometer s l i t a l w a y s s tays i n t h e r e g i o n of u n i f o r m e x p o s u r e , d e n s i t o m e t r y of t h e spectra m u s t be

performed i n segments, or a computer program may be devised t o c o n t r o l t h e scan au tomat i ca l ly , t h e exac t procedure depending upon t h e user 's p r o j e c t .

5.6 Long Wavelength C a l i b r a t i o n

range of t h e spectrograph was made. I t was considered un- .

necessary , because t h e i n t e n s i t y d i s t r i b u t i o n i n t h e s o l a r spectrum from 2000 t o 3000A, approximately, is w e l l known and is be l ieved not ' to vary s i g n i f i c a n t l y with changing s o l a r con- d i t ions.

No d i rec t i n t e n s i t y c a l i b r a t i o n of t h e long wavelength

The s t e p s requi red t o conver t f i l m d e n s i t y measured from a long wavelength spectrum t o a b s o l u t e u n i t s have been described by Doschek, Feldman, and Cohen ( 1 2 ) . The convers ion begins w i t h t h e e s t ab l i shmen t of a c h a r a c t e r i s t i c curve f o r t h e f i l m batch of i n t e r e s t , a s descr ibed i n Sec. 5.3.1 above. Re la t ive i n t e n s i t i e s der ived from t h e c h a r a c t e r i s t i c curve a r e t h e n converted t o abso lu te i n t e n s i t i e s by re ference t o one of s e v e r a l publ ished s o l a r a t l a s e s covering t h e s p e c t r a l reg ion , s u c h a s Tousey, e t a l . (1) 1974, or Broadfoot ( 2 ) 1972.

The major d i f f i c u l t y encountered i n ob ta in ing a b s o l u t e va lues f o r t h e ATM da t a involves s e l e c t i n g t h e proper cor - rect ion f o r l i m b darkening i n o rder t o r e l a t e t o t h e v a l u e s t abu la t ed i n t h e a t l a s e s , w h i c h apply t o t h e r a d i a t i o n from t h e t o t a l sun . Doschek et a l . made- use of t h e v a l u e - f rom. A l l e n (13) f o r 2800A based on work by Bonnet ( 1 4 ) . Depend- ing upon t h e ind iv idua l research problem, each i n v e s t i g a t o r w i l l undoubtedly se lec t h i s own approach to t h i s c o r r e c t i o n . The l i m b darkening func t ion is by no means independent o f Wavelength i n t h e UV. A forthcoming p u b l i c a t i o n by K j e l d s e t h Moe and Milone (15) lists c o e f f i c i e n t s €or limb darkening equat ions , der ived a s f u n c t i o n s of from t h e ATM da ta .

5 5 3 R e f e r e n c e s

1. Tousey, R., E. F. Milone, J. D. P u r c e l l , W. P a l m aSchnei ,der , and S. G. T i l f o r d , NRL R e p t . 7788, 1974 "An A t l a s of t h e S o l a r U l t r a v i o l e t Spectrum Between 2226 a n d 2992 Angstroms."

2. . B r o a d f o o t , A. L y l e , A p . J. 173 , 681-689, 1972, "The Solar Spectrum 2100-3200 A".

3. K j e l d s e t h Moe, O., M. E. VanHoosier , . J . -D.F. B a r t o e , and G. E. Brueckne r , NRL R e p o r t 8056, 1976 "A S p e c t r a l A t l a s

. of t h e Sun Between 1 1 7 5 and 21.00 Angstroms."

4. B r i d g e s , J. M., and W. R. O t t , App. Optics, 16, 367- 376, 1977. "Vacuum Ul t rav io le t Radiometry. 3: The Argon Mini -a rc a s a N e w Secondary S t a n d a r d of Spectral Radiance".

5. Brueckne r , G. E. , J.-D. F. Bartoe, 0. K j e l d s e t h Moe and M. E. VanHoosier , Ap . J. - 209, 935-944, 1976, "Abso lu te Solar U l t r av io l e t I n t e n s i t i e s and T h e i r V a r i a t i o n s w i t h Solar A c t i v i t y . I. The Wavelength Region 1750-2100 A."

6. K j e l d s e t h Moe, 0. and K. R. Nicolas, A p . J. - 211, 579-586, 1977, "Emiss ion Measures , E l e c t r o n D e n s i t i e s and Non- , t h e r ma 1 - Ve 1 o C:i t ies :. frqrnr-m t ic.a&.&-; Th in.. UV-. Line s. N e a g,.., a Quiet Solar Limb;.'!

7. Nicol.as, K. R., Ph. D. T h e s i s , . . U n i v e r s i t y of Mqryland. 1977, "The A p p l i c a t i o n of S i I11 L i n e I n t e n s i t y Rat ios t o De te rmine t h e Solar T r a n s i t i o n Zone D e n s i t y a n d P r e s s u r e . " ..

8. Doschek, G. A., U. Feldman, M. E. VanHoosier, and J.-D. F. Bartoe, Ap . J. Suppl . 31, 417-443, 1976, "The

. E m i s s i o n - l i n e Spectrum Above t h e L i m b of t h e Q u i e t Sun: 1175-1940A. 'I

9. Samain, D., R. M. Bonnet , R. Gayet , and C. Ligambert , A s t r . and Ap. 39, 71-81, 1975, "Stigmatic S p e c t r a of t h e Sun B e t w e e r 1 2 0 0 A and 2100A."

10 . Bartoe, JD-D. F., G. E. Brueckner , J. D. P u r c e l l , and R. Tousey, Appl. O p t . 1 6 , 879-886, 1977, "Extreme Ul t ra - v i o l e t S p e c t r o g r a p h A T r E x p e r i m e n t S082B.I'

11. Yang, C. Y., N. P. P a t t e r s o n , and 0. K j e l d s e t h Moe, p r iva t e communcation.

12 . Doschek, G. A., U. Feldman, and Leonard Cohen, Ap. J. Suppl. 33, 101-111, 1977, "Chromospheric Limb Spectra from Skylab: 2000 t o 3200A."

1 3 . A l l e n , C . W . , " A s t r o p h y s i c a l Q u a n t i t i e s " (London: A t h l o n e ) p. 1 7 2 , 1973.

1 4 . Bonnet , R . , Ann. dOAp. - 31 , 5 9 7 , 1968.

1 5 . K j e l d s e t h Moe, 0. and E . F . M i l o n e , submitted to A p . J. S u p p l . , "Limb Darkening 1945A t o 3245A for t h e Q u i e t Sun from S k y l a b Data."


F i g . 5.1 Example of f i l m c h a r a c t e r i s t i c cu rve d e t e r m i n e d fr'om t h e CALROC e x p o s u r e s . C r o s s e s mark t h e obse rved p o i n t s s h i f t e d a l o n g t h e e x p o s u r e a x i s t o form t h e best p o s s i b l e a v e r a g e curve, K j e l d s e t h Moe e t a l . ( 3 ) .

F i g . 5.2 A b s o l u t e c a l i b r a t i o n c u r v e for ATE4 1 0 4 - t y p e film.

F i g . 5.3 Example of r e l a t i v e c h a r a c t e r i s t i c c u r v e s f o r . one

P r e p a r e d by K j e l d s e t h Eloe a n d N i c o l a s ( 6 ) and ( 7 ) .

f i l m b a t c h and development r u n on ATN 104- type f i l m . .

F i g . 5.3 ( a ) Wavelengths s h o r t e r t h a n 1400 A.

F i g . 5.3 (b) Wavelengths l o n g e r t h a n 1400 A.

5'7t ' A-CONTINUUM 5.61 +-NEUTRAL LINE

I I I I 1 I 1 1 I I I I I I I

I 0-SINGLY IONIZED LINE

(3

0

%o

4.9

4.8

s" 0 Po +

T I. . . 0 i' + 0 + x, + "

+ ' + ' + 0

I I I I O I I I I I I 1 I I I

1200 1300 1400 1500 !" 1600 1700 1800 1900 x (A, I .

Fig. '5.2

-0.8 -0% -0.4 -0.2 0 0.2 0.4 06 0.8 ..

-0.8 -0.6 -0.4 -0.2 .O 0.2 0.4 0.6 0.8

Table 5.1 Absolute Calibration of S082B Instrument (104 film)

Wavelength

1160.0 1200.0 1206 .O 1400.. 0 1450 . O 1500 . O 1514.0 1535.0 1557.5 1577.0 1600 .O 1900.0 1960.0

5 . 4 9 7 5 . 394 5.379 4 . 883 4.884 4.891 4.900 4.915 4.935 4 . 95% 4 . 989 5.425 5.512

Table 5 . 2 Data from F i g . 5.3 Characteristic Curve

Density

0 . 0 0 0 . 0 . 0 2 0 0 . 0 4 0 0 . 0 6 0 0 . 0 8 0 0.100 0 . 150 0 , 2 0 0 0 . 2 5 0 0 . 3 0 0 0 .350 0 - 4 0 0 0 . 4 5 0 0 . 5 0 0 0 . 5 2 0 0 . 540 0 .560 0 . 5 8 0 0 . 6 0 0

a*.954

0.729 0.633 0.548 0.472 0.316 0.196 0.095 0.000 0.106 0.238 0.412 0 . 6 4 3 0.755 0 . 879 1.017 1 170 1.338

&35>

L

Table 5.2 S082B Slew Exposures and Film History

Plate Nom DOY

Mission - SLY2 lBOOl Camera B1 '1B002

1B003-1B018 150 lB019-1B041 J53 lB042-1B078 153

157/158 1B079-1B081 18082-18103 1B104-1B107 lBlQ8-1B142 lB143-1B177 . lB178-1B182 18183-1B201

SL-3 2B001 Camera B2 2B002

2B003-2B021 2B022-2B040 2B041-2B080

28081-28091 2B09 2-2B103 2B104-2B144 2814 5-2B150 2B151 2B152-2B184

2B185-2B192 2B19 3 - 2B2 0.1

161 162

164

167 168

220

225 225

229

. 231 231

233 234 235

Slew Batch - Plate Nom

lBOll 1B035 1BO 61/2 lB075

1B083 .,;:. 1B106

1B145/6

13192 .;a

18194

2E014

2B057/8 2B064/5

2B140

28172 2B175

28194 2B198/9 253200

0 4 04 04 04 04

04 04 04 04

CALROC I 0 4 0 4 04

06 0 6 06 0 6 0 6

06 06 06 06

06 .OS( 101)

0 6 06

-- Roll

6A 3

78 0A OA

78 7B 7B 7A 7A 7B 7B

3 2 2 1

1 1' 2 2 2 3(101) 3

3 2

DevRun

3 1 1 1 2

2 3 5 5 4 4 3

1 A 1 1

2 3 3 5 4 4 4

3 3

T a b l e 5 . 2 (Cont.) S082B S l e w Exposures and F i l m His tory

Miss ion P la t e No.

SL-3 2B301-2B303

2B305-2B339 2B340-2B341 2B342-28376 2B377-2B380 .2 B3 8 1- 2 B 4 0 1

Camera B3 2B304

2B402 2B403-2B439

2B440-2B479

2B480-2B499

2B500 ,

2B501 '

SL-4 3B001-3B017 Camera 8 4 3B018-3B036

3B037-3B047 3B048-38073 3B0.7 8-381 00 3B101-3B108 3B109-3B123 3B124-3B158 38159-3B164 3B165 33166-3B184 3B185-3B201

Slew ' -

DOY Plate No. - 237 2B303 237 2B304 238 2B332/3

2 4 1 2B355/6/7

244 2B387 244 2B391/2

247 247 249 2 5 1 254 255 257 258 260 262

2B418/2q 2B426/7 2B446 28465 ,

2B477 2B480/1 2B483 2B488 2B492 28498

333 ' 38004 340 3B026/7

0 0 7 38154/7 011 3B159/60

B a t c h

06 05(101) 05 05 05 05 0.5'

05 CALRQC I1 05

05

05

05 05

08' 0 8 08 08 08 08 10( 1 0 1 ) 10( 1 0 1 ) 08 08

016 ' 38175 ,CALROC I11 08 030 3B200/01 08

- Roll

3 3 ( 1 0 1 ) 1 7 . 1 7 18 1 7 17

1 7 1 6

1 6

17

1 7 1 7

8 8 8 9 9 9 . 4 4 8 8 8 8

DevRun

1 1 1 2 2 2 3

$5 4

3 '

A 1

4 3 1 1 2 4

5 5 1 3 2

The S 0 8 2 B f l i g h t f i l m is kept i n a secure a r e a a t t h e Naval Research L a b o r a t o r y , Washington , D. C. Anyone who n e e d s t o perform a n a n a l y s i s from t h e o r i g i n a l f i l m s h o u l d c o n t a c t D r . Richard Tousey, Code 7140, P r i n c i p a l I n v e s t i g a t o r , or Mr. R i c h a r d Schumacher, Code 7149, Program Manager.

I n d i v i d u a l f l i g h t f i l m s t r i p s a r e 35 x 250 mm i n s i z e and have been mounted f o r p r o t e c t i o n between 2 x 1 2 i n c h g1as.s p l a t e s separated by t h i n brass s p a c e r s . N o w referred t o as " p l a t e s " , a l l o r i g i n a l mater ia l , c o n s i s t i n g of 6408 s p e c t r a , has been copied a t 1.8-times m a g n i f i c a t i o n o n t o 70-mm Kodak 2421 Aerial D u p l i c a t i n g r o l l f i l m (Es ta r Base) and a r c h i v e d a t t h e N a t i o n a l Space S c i e n c e Data C e n t e r (NSSDC). A 21-s t ep wedge was a l s o e n l a r g e d and pho tographed w i t h t h e p la tes t o e n a b l e t h e g e n e r a t i o n of t r a n s f e r c u r v e s f rom f l i g h t f i l m t o users' copies. Members o f t h e s c i e n t i f i c community may o b t a i n h i g h q u a l i t y f o u r t h - g e n e r a t i o n p o s i t i v e s and f i f t h - g e n e r a t i o n n e g a t i v e s f rom NSSDC ( t h e f l i g h t f i l m is c o n s i d e r e d f i r s t g e n e r a t i o n ) . A l s o a v a i l a b l e w i t h t h e s e d a t a a r e f i l m c a t a l o g s on m a g n e t i c tape or microfiche and t h e . " N R L / A T M U s e r ' s G u i d e t o Experiment S082B."

F i g u r e 6 .1 i l l u s t r a t e s t h e p h o t o g r a p h i c h i s t o r y o f c o p i e s a v a i l a b l e fo r d i s t r i b u t i o n t o i n t e r e s t e d u s e r s . The master p o s i t i v e copy, produced a t NRL, was u s e d t o make a c o n t a c t working n e g a t i v e a t NSSDC, and a working posit ive was t h e n p r i n t e d from t h e f i r s t working n e g a t i v e . Users' c o p i e s , as i n d i c a t e d , are t h e n produced from t h e w o r k i n g c o p i e s . ' D u r i n g t h e e n t i r e p h o t o g r a p h i c p r o c e d u r e , care was t a k e n t o p roduce a h i g h q u a l i t y u n i f o r m product , and good q u a l i t y c o n t r o l is exercised a t NSSDC i n t h e f i l m p r o c e s s i n g . W i t h m u l t i p l e g e n e r a t i o n c o p i e s , however , there is some loss of f i n e d e t a i l i n t h e f a i n t e r spectral e x p o s u r e s . I t i s expected t h a t t h e copies w i l l be u s e f u l p r i m a r i l y a s i n t e r m e d i a t e n e g a t i v e s o r p o s i t i v e s f rom which p r i n t s c a n be made, o r t h e y can be used i n v a r i o u s q u a l i t a t i v e or s u r v e y - t y p e i n v e s t i g a t i o n s .

6 . 1 P h o t o g r a p h i c P r o c e d u r e s

I n t h e d u p l i c a t i o n of t h e f l i g h t e x p o s u r e s it was f o u n d n e c e s s a r y t o d e v e l o p p h o t o g r a p h i c e q u i p n e n t fo r t h e p u r p o s e . T h i s equipment , t h e d u p l i c a t i n g f i l m , ' and. t h e p r o c e s s i n g were selected t o o b t a i n opt imum r e s o l u t i o n , moderate g r a i n compress ion on t h e copy f i l m , and t o r e t a i n t h e f u l l d e n s i t y r a n g e of t h e data. I n t h e e n l a r g e r , a 2600W q u a r t z lamp was used t o o b t a i n maximum r e s o l u t i o n , a c u t a n c e , and image con- t r a s t . T h i s p o i n t l i g h t source was a d j u s t e d i n p o s i t i o n t o minimize color f r i n g i n g and p a r a l l a x and t o a c h i e v e best u n i f o r m i t y of i l l u m i n a t i o n . The u n i f o r m i t y a t t a i n e d w a s found t o be w i t h i n +6% o v e r t h e e n t i r e f i l m plane. The l e n s was selected t o minTmize d i s t o r t i o n s and c u r v a t u r e of f i e l d . -

Alignment or t h e system was a c h i e v e d w i t h a helium-neon a u t o c o l l i m a t i n g l a se r , u s i n g t h r e e - p o i n t c o n t r o l a t t h e l e n s board and a t t h e car r ie r for t h e f i l m magazine. A vacuum back was used t o ho ld t h e f i l m f l a t a t t h e e n l a r g i n g surface.

The f i l m was s t o r e d a t 55' F u n t i l 24 hour s p r i o r t o u s e and was r e f r i g e r a t e d a f t e r e x p o s u r e u n t i l t i m e t o be processed. These p r e c a u t i o n s were t a k e n t o m i n i m i z e l a t e n t image l o s s and f o g g i n g of t h e f i l m .

The p l a t e s were copied i n small g r o u p s . A t t h e b e g i n n i n g and end of each p h o t o g r a p h i c s e s s i o n , t h e f i l m was g i v e n a s e n s i t o m e t r i c e x p o s u r e u s i n g a Kodak Process Cont - ro l S e n s i t o - meter, Model 101. These frames reside on t h e f i l m a t NSSDC, and were used p r i m a r i l y t o check t h e u n i f o r m i t y of f i l m deve lopment from b e g i n n i n g t o end of a p a r t i c u l a r g roup . A g r e a t amount of c r e d i t is d u e NSSDC i n m a i n t a i n i n g its p rocess .o r c o n t r o l t o s u c h a degree t h a t no s i g n i f i c a n t d i f f e r e n c e s c o u l d be measured from end t o end i n t h e v a r i o u s deve lopment r u n s .

The processor was a Kodak Model 11,Versamat w i t h one rack, employing Hunt E. R. Aeroflo ( R e g u l a r ) d e v e l o p e r a t 8S3 F. The f i l m was of o n e batch number and w a s processed t o a gamma of 1 . 0 . S e n s i t o m e t r i c s t r i p s a t NSSDC deve loped a t i n t e r v a l s d u r i n g t h e r u n s v e r i f i e d t h e gamma t o a tolerance of about 0.02 as d e r i v e d from measurements w i t h a Macbeth Model TR524 d e n s i t o m e t e r ( d i f f u s e d e n s i t y ) .

6 .2 T r a n s f e r Curves

O f more i m p o r t a n c e t o a user who would attempt rough p h o t o m e t r i c u s e of t h e f i l m is t h e 2 1 s t ep Kodak cal ibrated wedge which was'photographed w i t h t h e copy camera a t l ea s t o n c e d u r i n g each copy s e s s i o n a t NRL. The f i l m i n t h e wedge conforms closely t o t h e d i m e n s i o n s and g r a n u l a r i t y of t h e f l i g h t f i l m and was mounted i d e n t i c a l l y between g l a s s p l a t e s of t h e same s i z e and t h i c k n e s s a s t h e S082B mounting p la tes . Table 6 .1 is a l i s t i n g of t h e v a r i o u s e x p o s u r e s , g i v i n g t h e l o c a t i o n o f a p a r t i c u l a r wedge whose e x p o s u r e and g e n e r a l h i s t o r y matches a group of f l i g h t frames. The symbols i n .

f r o n t of t h e p l a t e numbers i n d i c a t e a wedge image j u s t prior t o or j u s t a f t e r t h a t p la te . For example , a wedge exposed and processed w i t h p l a t e number 2B148 w i l l be found j u s t before p l a t e 2B146 and a n o t h e r j u s t before p l a t e 2B151 on t h e r o l l f i l m . Al though t h e wedge i n f r o n t . o f 2B161 w a s processed a t t h e same t i m e , it w a s exposed n e a r e r i n t i m e t o p la tes 2B161 t h r o u g h 2B201, i n d i c a t e d ' b y a semicolon d i v i d i n g t h e g r o u p s i n t h e table . F r e b u e n t u s e w a s made of t h e s tep wedge t o i n s u r e e v a l u a t i o n o f . p o s s i b l e l a t e n t image l o s s or c h a n g e s caused by d i f f e r e n c e s i n t h e deve lopment process which m i g h t occur from one group of e x p o s u r e s t o a n o t h e r . I n e i t h e r case a t r a n s f e r c u r v e c a n be plo t ted

f o r any p a r t i c u l a r g r o u p o f e x p o s u r e s by p l o t t i n g s tep d e n s i t i e s o f t h e wedge l i s t e d i n Table 6 . 2 agains t wedge d e n s i t i e s measured from t h e u s e r s ' copy.

T y p i c a l t r a n s f e r c u r v e s d e r i v e d from t h e wedge images are shown i n F i g s . 6 . 2 and 6 . 3 . F i g u r e 6 . 2 c h a r a c t e r i z e s t h e master p o s i t i v e f i l m a r c h i v e d a t N S S D C . D i f f u s e d e n s i t i e s o f t h e copy were measured on a Macbeth Model T D l O O A d e n s i t o m e t e r and are p l o t t e d a g a i n s t t h e Table 6 .2 specular d e n s i t i e s of t h e wedge i t se l f , o b t a i n e d w i t h t h e t h e NRL p r e c i s i o n G r a n t m i c r o d e n s i t o m e t e r . B o t h s p e c u l a r and d i f f u s e s t e p d e n s i t i e s of t h e wedge a r e g i v e n i n Table 6 . 2 . S p e c u l a r d e n s i t y was used i n t h i s case i n order t o re la te t o t h e v a r i o u s phenomena measured o n t h e f l i g h t f i l m by members of t h e NRL da t a a n a l y s i s team. S i n c e most d a t a o f v a l u e f a l l between a b o u t 0 .10 and 1.00 s p e c u l a r d e n s i t y u n i t s on t h e f l i g h t f i l m , t h e copy d a t a were deemed u s e f u l when t h e t r a n s f e r c u r v e was s t r a i g h t i n t h a t d e n s i t y r a n g e . A s shown i n F i g . 6 . 3 , a good c u r v e was a l s o m a i n t a i n e d for t h e u s e r ' s g e n e r a t i o n s of f i l m , w i t h D m a x ( d i f f u s e ) o f a b o u t 1.8 for t h e Users' P o s i t i v e and a b o u t 2 .0 for t h e User's N e g a t i v e . Dmin v a l u e s for t h e P o s i t i v e s and N e g a t i v e s are 0 . 2 2 and 0.35 r e s p e c t i v e l y .

6.3 Image D e g r a d a t i o n

Mounted between g l a s s p la tes h o l d i n g t h e Rodak C a l i - brated s t ep wedge d i s c u s s e d i n S e c t i o n 6 . 2 were t w o p r e c i s i o n r e s o l u t i o n f i l m t a r g e t s of t h e s t a n d a r d A i r Force 1 9 5 1 t y p e . One , a medium c o n t r a s t t a r g e t , had a c o n t r a s t r a t i o of 6.3: l for a d e n s i t y d i f f e r e n c e (AD)of 0.8 between t h e l i n e s and .

t h e background. T h i s c o n d i t i o n is c l o s e t o t h a t of t h e *

S082B spectra , where D m a x ( specular ) , is about 1 . 0 and Dmin about 0.1. An opaque l i n e t a r g e t on a c l e a r background was s e l e c t e d t o c o r r e s p o n d w i t h t h e n e g a t i v e spectral l i n e s on t h e f l i g h t f i l m . R e s o l u t i o n r a n g e of t h e t a r g e t was one t o 228 l i n e p a i r s p e r mm.

The second t a r g e t was h i g h c o n t r a s t , w i t h a c o n t r a s t .

r a t i o of 1 O O : l and A D = 2 . 0 or h i g h e r . An exposure of b o t h t a r g e t s w a s o b t a i n e d e a c h t i m e t h e wedge was photographed (Table 6 . 1 ) . P la te 1B168 was a l s o pho tographed a t t h e begin- n i n g of e a c h copy s e s s i o n t o p r o v i d e a s t a n d a r d by which t o j u d g e l o s s of spectral d e t a i l from g e n e r a t i o n t o g e n e r a t i o n a s s u b s e q u e n t contact p r i n t s were made. .

E n l a r g e d p r i n t s on Kodak p o l y c o n t r a s t RC paper were made.from e a c h copy g e n e r a t i o n and t h e f l i g h t f i l m , from i n selected wavelength r e g i o n s . Exposures were a d j u s t e d s l i g h t l y t o a c h i e v e a p p r o x i m a t e l y equal d e n s i t i e s from e a c h copy.

A s c o u l d be s e e n from t h e e n l a r g e d paper p r i n t s , r e s o l u - t i o n was l o s t between t h e o r i g i n a l f i l m and t h e f i r s t copy. Compared w i t h a b o u t 83 l i n e pairs/mm r e s o l u t i o n of t h e f l i g h t f i l m , about 53 l i n e pairs/mm c o u l d be r e s o l v e d on t h e medium c o n t r a s t t a r g e t s o f t h e copies. N o s i g n i f i c a n t d i f f e r e n c e s among t h e copies u p t o 5 t h g e n e r a t i o n c o u l d be measured , e x c e p t t h a t s l i g h t l y better r e s o l u t i o n c o u l d be o b s e r v e d from t h e n e g a t i v e copy t a r g e t s t h a n w i t h t h e p o s i t i v e copy t a r g e t s . S l i g h t l y more r e s o l u t i o n was l o s t i n t h e h i g h c o n t r a s t t a r - g e t s , which a v e r a g e d a b o u t 46 l i n e pairs/mm.

6 . 4 Fi lm C a t a l o g

A complete l i s t i n g of t h e S082B e x p o s u r e s , Appendix B, is c o n t a i n e d i n a m i c r o f i c h e catalog of 5 p a r t s located i n pockets attached t o t h i s Guide. Table 6.3 is a sample s h e e t showing t h e f i l m or p la te number (each p la te c o n t a i n s 8 e x p o s u r e s ) , d a y o f y e a r da t e of e x p o s u r e , t i m e o f s h u t t e r o p e n i n g , e x p o s u r e d u r a t i o n , and p o i n t i n g i n f o r m a t i o n i n yaw, p i t d h , and r o l l . The da t a were d e r i v e d from b i n a r y coded decimal i n f o r m a t i o n p r o j e c t e d o n t o a f i l m c h i p a t t a c h e d t o . each S082B f i l m s t r i p . The t ime-of-day r e c o r d e d by t h e d i o d e a r ray was m i s s i o n e l a p s e d t i m e (MET) f u r n i s h e d by a n ATM on-board computer . T h i s computer t i m e v a r i e d f rom,Greenwich Mean Time (GMT) by as much as a few s e c o n d s and r e q u i r e d periodic updates by ground'command. The times l i s ted i n Appendix B have been corrected by t h e a p p r o p r i a t e u p d a t e i n f o r m a t i o n .

P i t c h and yaw are g i v e n i n a rc sec, w h i l e r o l l is a n a r c min. For cor rec t r o l l i n f o r m a t i o n , o n e must u s e t h e " R e c o n s t r u c t e d R o l l " referred t o i n s e v e r a l documents l i s t e d i n Appendix A.

The column headed Iloff" g i v e s t h e P o i n t i n g R e f e r e n c e System (PRS) l i m b o f f s e t i n arc sec. A minus s i g n i n d i c a t e s a p o s i t i o n on t h e so l a r d i s c . F i f t y ( 5 0 ) i n d i c a t e s t h e . P R S is of f on i n w h i t e l i g h t d i s p l a y s t a t e .

A zero ( 0 ) or one (1) i n any o n e of t h e p l a c e s i n t h e .

"mode" 4 b i t column had t h e f o l l o w i n g meanings:

Auto Step/ 2 ,,he L O = NRL bias n o t i n Aut 1 = NRL bias i n

Errors t h a t h a v e b e e n found t o be d iode a r r a y e r r o r s have been marked w i t h a $ symbol. An e x c e p t i o n t o t h i s symbol is t h a t minus ( - ) o f f s e t e r r o r s a re c o r r e c t e d w i t h a p l u s (+) and are t h e o n l y p l u s m a r k s found i n t h e log.

It will be noted that 4 cameras were used to supply the film for the 3 manned missions. The cameras and film trace- ability information, including development runs, are listed .in Appendix C, Film Sequence Log, described in Section 4.2 of this Guide. The cameras carried film.strips of the fol- lowing numbers:

Mission --- Camera I_--- Film Stripor -------- Plate No. ----- 1. 2. 3. 4.

lBOOl - 1B201 2BOO1 - 2B201 2B301 - 1B501 38001 - 3B201

SL-1/2 SL-3 SL-3 SL-4

Other listings of the data are contained in documents described in Appendix A, Skylab Documentation.

Exposure times available for the automatic and flare mode operation of S082B are given in Tables 6.4 and 6.5 , respectively. Normal exposures on the solar disc were those listed under the “Zone 1” column. Times shown should be accurate to within a millisecond.

ATM F l i g h t Fi lm

4

User's P o s i t i v e

*

Enlarged (1.8X) Master Copy

P o s i t i v e

b

I NSSDC Contact

Fig. 6.1 - Duplication process for NRL/ATM photographic data

m

W cn 3 LL L D

>- I- cn z . W 0 >- a

Y

-

s

2.0 I I I I I I I I I I I I I I I i 1 ' 1 I I I I

1.8 - - MASTER FILM -

KODAK TYPE 242 I - POSITIVE COPY

-

0.8 - 0.6 - -

0.4

-

- - - I

0 0.3 0.6 0.9 1.2 1.5 1.E 2.1 WEDGE DENSITY (SPECULAR)

Fig.*- NSSDC archived master - -

I . _

WEDGE 'DENSITY. (SPECULAR) Figs - Transfer curves

2B0 5 1 -2B 100 2B101-2B145 2B146-2B201 2B301-2B350 2B351-2B400 2B401-2B444 2B445-2B501 3B001-3B095 3B096-3B100 3B101-3B125 3B126-3B201

lBOO l-1BO 15 2 1B016- 113030 2 1B031-1B080 3 lB081-1B140 3 1B141- 1B200 3 1 B 2 0 1 , 2B001-2B050 3

3 3 4 4 4 4 4 4 5 5 5

T a b l e b . 1 Location of S tep Wedges Filmed wi th Groups of S082B P la . tes

Fi lm Groups Copy Roll* Wedge Locat ions

C l B 0 0 1 , >1B015 ClB012 , >1B030 a B 0 3 1 , >1B080 c l B O 8 1 <1B141, >1B150, >1B165; C l B 1 6 6 , >1B200 <1B201, >2B025, >2B050 <2B051; C2B076, >2B100 <2B101; <2B126 <2B146, c2B151 ; C2B161 C2B301, >2B350 <2B351, >2B400 <2B401 , >2B440 C2B445, >2B501 c3B001 , >3B025, >3B050; c 3 B 0 5 1 , >3B075 el3096 4 B 1 0 1 , 4 B 1 2 6 ;

*,Copy f i l m was Eastman Kodak "ype 2421, i n 4 d i

> Exposure jus t a f t e r XBXXX plate. Exposure j u s t p r i o r t o XBXXX p l a t e

>3B125 . ,

G B 1 5 1 ; G B 1 7 6 ; C3B201

f e r e n t r o l l s , a l l of same ba tch nun Iers.

; Pause i n exposure of p l a t e s j u s t p r i o r t o next wedge l i s t e d .

Time l a p s e of 1 hour t o ove rn igh t may e x i s t between wedges.

STRIP NR DOY HR/MN/SEC EXPT I ME YAW

-966. -966 . -966 -9 66 -966 -966 -966 -984

P I T C H ROiL O F F MODE .. . . .

0.25 l i l .Od 1.25

40.00' 5.00

160.00 20.00 359.50

lQ210. 1021n. 10210. 10210. 10210. 1021 00.. i 0207. 10143.

0101 ninr 0101 01 0 1 0 1 0'1 0101, 0101 oooi

28121A1 28 1.2 1-2 28121-3 28321-4 28121-5 281 2 1-6 28121-7 29121-8

228 228 228 220 228 228 228 228

18/38/14.75 l8I3W17.00 18/38/28.75 18/38/32.00 18/39/13.75 18/39/20 e75 18142/ 2.50 18/50/18.25

-7 . -7 . -7. -7 . -7. -7 . -7.

O i

50 0

5n. 50 . 50. 5C)r 50 . 50 . 50.

228 228 228 228 228 228 228 228

-969 i -969 -944 6 -944 . -944 . -944 . -944 . -944.

2; 22. -31 -31 -31 -31 . -31 . -31.

10287. 9497. -7793 . -7793 . -7793 . -7793 . -7793 . -7793 .

25 i 25. 0130 -12; -12, -12. -1 I . -12;

000 I 000 1 1001 1001 1001 1001 1001 1001

28 122- 1 28 122-2 28 122'-'3 28 122-4 28 122;-'5 28 122-6 28 f 22-7 28 122-8

28123-1 28 123-2 28 123-3 28 123-4 26 123i5 28 12306 28 12317 28 123-8

28124-1 28 124-2 281 24-3 28 124-4 28124-5 28124-6 28 124-7 28 124-8

958 75 602.25 2.50 0.25 lO.00

1.25 40 . 00 5.00

21/13/ 1.25 2 1 / 15/43 00 21/16/ 4.75 21/Id/ 9.@0 21/16/11.25 2.1/16/23.@0 21/16/26*00 21/17/ 8.00

228 228 228 228 228 228 228 228

159.75 19.75 2.50 0.50 1o.m 1.25

40,OO 4.00

-944 -944 . -944 . -944 . -944 . -944 . -944 . -944 .

-31. -31 -31 -31. -31 -31 -31 . -31 .

-7793 . -7793 . -7793 . -7793 -7793 . -7793. -7793 . -7793;

-12. -12, -3 . -4 . -4 6 --4 . -4 . -4 .

1001 1001 1001 1001 1001 1001 inoi 1001

160.00 20.00 2.50

10.00 1 e25

40.00 4.50

' 0.i)OS

228 228 220 228

228 228 220

228

2 I / I 7 1 1 6.50 2 I ) I 9j58.25 21/20/20.00 21)20/24050 21/20/26.75 21i2oi38.50 21/20/41450 21/21/23.50

-944 . -944 . -944 . -944 a -944 . -844 . -944 . -944 .

-31 -31 -31 . -31 - 3 1 -31 -31 e

-31

-7793 - 779.3 -7793 . -7793 a -7793 . -7793 . -7793 . -7792 .

-4 -4 -2 . -2 . - 1 . -2 . -2 . -2 .

1001 1001 1001 1 6 0 1 1001 1001 1001 1001

21 /2 1 /32 ;OO

2 1 /24/35 050 21/24/39.75 21j24j42.00 21/24/53075 21/24/56.75 21/25/38.75

2 i j 2 4 ~ 3.75 160.00 20 . 00 2.5d ,0.50 10.00 1.25

39.25 5.00

2R125-1 28 125-2 28 125-3 28 1 25-4 28 125-5

28 125-7 28 125-8

281 2 5 ~ 6

228 ' 228 228 228 228 228 228. 228

-944 . -944 . -944 . -944 -944 . -944 . -944 . -944 .

-31 -31 a

-131 . -31 . -31 . -31 . -31. -31

-7793 . -7793 . -7793 . -7793 . -7793. -7793. -7793; -7793 .

-2 . -2 . 6.

- 1 . OF

Ll. 0. 0.

1001 1001 .1001 1001 1001 1001 1001 1001

Table 6.3

STEP DENSITIES OF KODAK CALIBRATED WEDGE

I I I Specular* Dif fuse+ I 1 .135 .12

2 .275 .22

3 .400 .32

4

5

.535

.660

.42

.51

6 .795 .61

7 .935 .71

8 1.06 ' .81

9 1.19 .91

1.32 1:00 10

11 1.44 1.10

12 1.58 1.20

13

14

15

16

17

18

1.72

1.84

1.99

2.09

2 .21

2.35

1.30

1.39

1.50

1.58

1.68

1.78

1 * Measured with G r a n t Microdensitometer

+ Kodak Cal ibra t ion i

.(above :clear -f.ilm.. s t e p ) .' % !

._ .

Table 6.4 AUTO MODE EIGHT EXPOSURE SEQUENCE

Exposure Number -

1 2 3 4 5 6 . 7 8

LW: sw:

ZONE 1 ZONE 2 ZONE 3 Duration (Sec) Duration (Sec) Duration (Sec) LW sw - LW sw LW sw .312

2.5

10.0

40 .O

160.0

1.25

5 .O

20 .o

2.5 4 .O 10 .o 16 .O

10 .o 16 .O 40 .O 64 .O

40 .O 64.0 160 .O 256 .O

256 .O 640.0 1024.0

160.0

253 Sec 4.2 Min 1076 Sec 17.9 Min 1714 Sec 28.6 Min

Long Wavelength Range Short Wavelength Range

Zone 1: Zone 2: +2 to +9 arc sec off limb and in Limb Scan or Limb PTG Zone 3: Moving from Zone 1 to Zone 2 increases exposure by factor of 4 Moving from Zone 2 to Zone 3 increases exposure by factor of 1.6

Sun Center to +1 arc sec or with PRS O f f or in WL Display

+10 arc sec or greater off limb and in Limb Scan.or Limb PTG

Table 6.5 S082B FLARE MODE, 48 Exposure Sequence

(12.8 min)

Duration E X P No. WL

33 S

34 S

35 S

36 S

37 L

38 L

39 L

40' L

2 rnin wait

41 S

42 S

43 S

- - Duration Duration

(Sec 1

17 S 0.321 1.250 1 S 0.312

2 S 1.250 18 S 1.250 5 .OOO

19 S 3 S 5 .OOO 5.000 20.000

20.000 80.000

0.156

4 S 20.000 20 S

5 S 0.312 21 L 0 .I56

6 S 1.250 22 L 0.625 0.625

2.500 7 S 5 .OOO 23 L 2.500

8 S ' 20.000 24 L 10.000 10.000

9 S 0.156 25 S 1.25

10 s 0.625 26 S 5 .OOO 1.250

5 .OOO

20.000

11 S 2.500 27 s 20.000

80.000 12 S 10.000 28 S

0.312 29 L 0.156 44 S

1.250 30 L 0.625 45 L

5 .OOO 31 L 2 .SO0 46 L

20.000 32 L 10.000 47 L

2 min wait 48 L

80 .OOO

0.256

0.625

2.500

10.000

13 S

14 S

15 S

16 S

7.0 OBSERVING PROGRAMS"

I n s u p p o r t of t h e ATN exper iments c a r r i e d o u t from Skylab , a number of l a r g e and impor t an t programs of so l a r r e s e a r c h were carried o u t from t h e ground, both by solar o b s e r v a t i o n s a l l over t h e wor ld , and by experiments f l o w n i n r o c k e t s . I n a d d i t i o n , a complex p l a n was developed f o r c o o r d i n a t i n g t h e i n d i v i d u a l S k y l a b o b s e r v a t i o n s , t o op t imize t h e r e t u r n from each i n s t r u m e n t and t o produce t h e most v a l u a b l e o b s e r v a t i o n s for so l a r phys ics . As a r e s u l t , a l a r g e number of i n s t r u m e n t s covering t h e spectrum from t h e v i s i b l e t o x-rays were brought t o f o c u s on g iven so l a r t a r g e t s , s u c h a s f l a r e s , and many times more da ta were acquired t h a n could otherwise have been ga the red . T h u s , a massive a t t a c k was made on problems of s o l a r p h y s i c s du r ing Sky lab ' s n i n e m o n t h s , which might w e l l be cal led " t h e yea r of t h e s u n " .

7.1 The J o i n t Observing Program

The J o i n t Observing Program ( J O P ) was devised t o m a k e it f e a s i b l e t o use s imul t aneous ly t h e maximum number of i n s t r u m e n t s t o produce t h e most v a l u a b l e s o l a r results. The key t o accomplishing t h i s was t o p l a n t h e observations i n a way t h a t offered t h e best chance o f c o n t r i b u t i n g t o t h e s o l u t i o n of t h e most impor t an t problems i n so l a r phys ics . A l i s t was drawn up t h a t covered the problems which t h e ATM ins t rumen t s were expec ted t o be m o s t l i k e l y t o e x p l a i n , such a s t h e mechanism for t r a n s f e r of energy through t h e so la r atmosphere, or t h e t r i g g e r mechanism o f s o l a r f l a r e s and wha t goes on d u r i n g f l a r e s . Observa- t i o n s r e l e v a n t t o each of t h e s e problems were l i s t e d , i n s t rumen t by ins t rument . From t h i s a n a l y s i s , a set of JOP's was developed t h a t came close t o making u s e of e v e r y experiment d u r i n g a l l t h e t i m e a l l o t t e d t o ATM. There were many c o n s t r a i n t s because t h e o b s e r v a t i o n s desired for one in s t rumen t were o f t e n n o t compa t ib l e w i t h those for a n o t h e r . The complex s e t of TOP'S took t h e form of an i l l u s t r a t e d manual c o n t a i n i n g de t a i l ed i n s t r u c t i o n s f o r t h e o p e r a t i o n o f each J O P , of which t h e r e were 13 i n SL-2. To implement t h e J O P ' s , a f u r t h e r s u b d i v i s i o n i n t o "bu.ild- i ng blocks'' ( B B ) , or e l emen ta l o p e r a t i o n a l sequences, w a s required. There were 23 b u i l d i n g b locks , which c o u l d be combined so as t o c a r r y o u t any of t h e JOP's. A small p o r t i o n of t h i s manua l , a c t u a l l y about one p e r c e n t , is reproduced i n F igu re 7.1.

*Mate r i a l for t h i s section h a s been e x t r a c t e d from a paper by R. Tousey, Applied O p t i c s 1 6 , 8 2 5 , 1977, Apollo Telescope Mount of Skylab: an OveriTew".

I n p l a n n i n g t h e J O P s d u r i n g t h e m i s s i o n , t h e pre- v a i l i n g so l a r c o n d i t i o n s were f i r s t c o n s i d e r e d . Once decided be tween, f o r example , a c t i v e r e g i o n s , JOP-2, or l i m b s c a n s , JOP-5, t h e b u i l d i n g blocks were chosen t o accomplish t h e p a r t i c u l a r J O P i n t h e b e s t way. Time blocks were c o n t r o l l e d t o one m i n u t e u n i t s , and s i n c e t h e time a v a i l a b l e p e r o r b i t w a s a maximum of 55 m i n u t e s , and o f t e n much less, t h e perfect f i t was rare.

The J O P sys t em worked s o w e l l i n SL-2 t h a t t h e number of J O P ' s w a s i n c r e a s e d i n t h e f o l l o w i n g m i s s i o n s , r e a c h i n g 27 for SL-4. I n a d d i t i o n , so much c o n f i d e n c e i n t h e crew was deve loped t h a t by l a t e SL-4 f r e e t i m e was g i v e n t o them i n s u b s t a n t i a l amounts f o r o b s e r v i n g events of o p p o r t u n i t y which appeared t o be of interest - t h e so- called " shopp ing l i s t" . Appendix A o f t h i s G u i d e c o n t a i n s a d e s c r i p t i o n of t h e J O P Summary Sheets a v a i l a b l e a t NRL a s a reference document and a n a b b r e v i a t e d l i s t i n g o f t h e JOPS for SL-3.

7.2 The C a l i b r a t i o n Rocke t Program - CALROC

Accuracy of c a l i b r a t i o n of i n s t r u m e n t a t i o n used i n t h e e x t r e m e u l t r a v i o l e t has always been a problem o f e x t r e m e d i f f i c u l t y , y e t i t s i m p o r t a n c e f o r solar r e s e a r c h c a n n o t be u n d e r e s t i m a t e d . E a r l y i n t h e ATM program it was p roposed by HCO and by NRL t h a t t h e i r i n s t r u m e n t s be ca l ibra ted by r e f e r e n c e t o c a r e f u l l y s t a n d a r d i z e d i n s t r u - m e n t a t i o n f lown i n rockets. One r o c k e t f l i g h t p e r m i s s i o n for each i n s t i t u t i o n was t h e minimum a c c e p t a b l e b e c a u s e t h e s e n s i t i v i t y of t h e ATM i n s t r u m e n t s was expec ted to .

change d u r i n g t h e c o u r s e of t h e n i n e months over which t h e y would be used. The f u n d a m e n t a l idea was t o m a k e a t t h e same t i m e t h e same measurements of s o l a r r a d i a t i o n u s i n g b o t h t h e rocke t -bo rne and t h e ATM i n s t r u m e n t s . The rocket i n s t r u m e n t s had been ca re fu l ly and r e c e n t l y calibrated before f l i g h t . Therefore t h e y could be used t o " s t a n d a r d i z e " t h e s u n s o t h a t it c o u l d s e r v e a s a s t a n d a r d s o u r c e w i t h which t o c a l i b r a t e t h e ATM i n s t r u m e n t s .

The p l a n of NRL was t o f l y i n s t r u m e n t s almost e x a c t l y l i k e t h o s e of ATM b u t reduced i n s i z e by a f a c t o r of two. The Harvard CALROC i n s t r u m e n t w a s d e s i g n e d i n a similar f a s h i o n . N R L , t o g e t h e r w i t h BBRC and t h e Ames Research C e n t e r , d e v e l o p e d a command s y s t e m by which t h e i n s t r u m e n - t a t i o n s e c t i o n , a f te r s e p a r a t i o n from t h e b o o s t e r , c o u l d be pointed at p a r t i c u l a r places o n . t h e sun . T h i s was done by a ragi0 command l i n k , combined w i t h a t e l e v i s i o n s y s t e m t h a t permitted t h e P I on t h e g round t o watch a d i s p l a y showing i n rea l t i m e t h e s u n ' s image i n H - a on t h e s l i t p la te of t h e rocket i n s t r u m e n t and t h e p r e c i s e l o c a t i o n of t h e s l i t on t h e sun .

The CALROC program required a g r e a t e f f o r t b u t t h e r e su l t s proved t o be h i g h l y s u c c e s s f u l . I n a d d i t i o n t o be ing e s sen t i a l for ATM, t h e p r o j e c t se rved a l s o t o pro- v i d e for t h e s c i e n t i f i c community i n g e n e r a l vehicles of much g r e a t e r s o p h i s t i c a t i o n for u s e i n ongo ing s o l a r research t h a n were a v a i l a b l e p r io r t o Skylab.

S e c t i o n 5 of t h i s G u i d e dea l s w i t h t h e c a l i b r a t i o n resu l t s from t h e program.

7 . 3 S o l a r F o r e c a s t S e r v i c e s

I t was ext remely impor t an t n o t o n l y f o r p lanning purposes b u t a l s o f o r making changes i n near r e a l t i m e i n t h e obse rv ing program being conducted by t h e ATM crewman t o have up-to-the-minute in fo rma t ion on s o l a r a c t i v i t y . A l though t h e crewman h i m s e l f could observe changes i n solar a c t i v i t y i n r ea l t i m e , it was h a r d l y p o s s i b l e for t h e crew t o ma in ta in t h e con t inuous monitor ing of t h e sun necessa ry t o detect a l l e v e n t s because t i m e was r e q u i r e d for o t h e r a c t i v i t i e s and for s l e e p i n g . Monitoring on a 24 hour basia.. was 'done through t h e ne twork of ground-based so la r o b s e r v a t o r i e s main ta ined by t h e Nat iona l Oceanic and Atmospheric Admin i s t r a t ion (NOAA) w i t h suppor t from t h e A i r Weather S e r v i c e and w i t h in fo rma t ion s e n t t o them by o ther o b s e r v a t o r i e s a l l over t h e world.

NOAA so la r forecasters were s t a t i o n e d i n t h e ATM c o n t r o l c e n t e r a round t h e c lock. They made a n i n v a l u a b l e c o n t r i b u t i o n by p rov id ing t i m e l y and complete knowledge of s o l a r c o n d i t i o n s t o t h e ATM team who prodiced t h e de t a i l ed p lann ing of t h e obse rv ing program, and a l so t o t h e ATM science Czar i n t h e ATM miss ion c o n t r o l c e n t e r .

Complete in fo rma t ion on t h e sun was made a matter o f record by NOAA. A l l t h i s material was d i s t r i b u t e d t o each ATM P I a f t e r t h e complet ion of t h e m i s s i o n for use i n t h e i n t e r p r e t a t i o n of t h e da t a ga the red by h i s solar i n s t r u m e n t s i n ATM. Appendix A l i s ts t h i s d a t a a v a i l a b l e among t h e r e f e r e n c e m a t e r i a l a t NRL.

7.4 Skylab Assoc ia t ed Solar Programs

Many associated s o l a r programs were carried on for t h e most p a r t by ground-based o b s e r v a t o r i e s and t o a lesser e x t e n t by space expe r imen ta t ion . The Coordinated Observing Program (COP) spearheaded by HCO, made con- tonuous ly a v a i l a b l e by radio b r o a d c a s t t h e o b s e r v a t i o n s a c t u a l l y be ing carried o u t by ATM t o g e t h e r with t h o s e planned for t h e fo l lowing day. T h i s information w a s r e c e i v e d by a s many as 250 d i f f e r e n t groups located a l l over t h e world. S e p a r a t e from t h i s was t h e Sky lab

ground-based astronomy program through which some eight or ten major observatories were funded to make specialized observations of a character closely related to the objectives of the ATM experiments. In addition, there was the ATM guest investigator program. This took the form of. proposals from a large number of solar physicists and .

astronomers to provide post-mission relevant observational material or specialized interpretative skills in exchange for data gathered by ATM. In effect the guest investigator program was simply a large collection of agreements between collaborating scientists and PI'S to share data. These various collaborative programs have proved to be most rewarding.

As a new experiment in collaboration, NASA, through the NSF and NCAR, has provided support for a series of Skylab Workshops which commenced in October 1975. These Workshops were organized by the High Altitude Observatory. The first was devoted to the study of coronal holes and .

the second dealt with the problem of explaining the flare mechanism.


F i g . 7 . 1 A sample s e c t i o n f r o m t h e volume t h a t c o n t a i n e d d e t a i l e d i n s t r u c t i d n s t o t h e crew c o n c e r n i n g t h e o p e r a t i o n of t h e ATM i n s t r u m e n t s . .The t o p s e c t i o n i s t h e first s t e p i n JOP 2B, a t t h e r i g h t a r e l i s t e d s e t u p t i m e s (SU), o p e r a t i o n t i m e s , and t o t a l e l a s p s e d t i m e s , i n t h i s c a s e 44 min. The B u i l d i n g B l o c k s (BB) are shown i n t h e lower l e f t , and o p e r a t i o n A-E a r e d e f i n e d i n t h e f i v e columns. The sample H-a image shows s u g g e s t e d s l i t p o s i t i o n s for S082B w i t h t h e SO55 s q u a r e s l i t l o c a t e d a t i ts c e n t e r .

JOP-28 . . - ACJIVE REGIONS: Long Term Evolution - Disc (RcSRe) Y -

4 A

8

C

D . E

BB I . Tarset ~. ~~

a Ro l l 82A XUV dispersion clear o f act ive region. a Point 55 OFFSET so that 55 MAR covers most o f active region.

a Point Hal a t a Habright point. a Ro l l s l i t for uniform emission. a Maximize DET 1 o r 3. a Repeat 8 a t a second H d b r i gh t point.

0 Point H d a t a r e l a t i v e l y dark HQ area. Ro l l 828 s l i t f o r uniform emission.

a Pointing and r o l l same as 4A. a Repoint 828 s l i t f o r uniform emission.

@.Record point ing coordinates RL+/- U+/D- L-/R+.

861: SPATIAL AND SPECTRAL RESOLllll0N.- BRIGHT FEATURES

- AT/ZAi - su:. 4 7/10

sui 3 6/20

6/29 su: 2 5/36

su: 2 6/44

su: 3

' .$.t Fig.% A sample section from the volume that contained detailed instructions to the crew concerning the operabon of the ATM instrument The top section is the first step in JOP 28, a t the right are listed setup times (SU). operation times, and total elaspsed times, in this case 4 min. The Building Blocks (BB) are shown in the lower left, and operations A-E are defined in the five columns. The m p l e ii-a image shov

suggestqd slit positions for S082B with the SO55 square slit located at its center.

8.0 SPECTRAL ATLAS*

Atlases of t h e s o l a r u l t r a v i o l e t r ad ia t ion h a v e been p r e s e n t e d for t h e wave leng th r e g i o n 2226 - 2992 A by Tousey e t a l . (1) and for t h e r e g i o n 2988 - 3629 A by Brueckner ( 2 ) . However, c o r r e s p o n d i n g l y comple t e i n f o r m a t i o n o n l i n e p r o f i l e s and c o n t i n u a w i t h good s p e c t r a l r e s o l u t i o n and re l iab le c a l i b r a t i o n of a b s o l u t e i n t e n s i t y have n o t been p u b l i s h e d f o r w a v e l e n g t h s below 2226 A. Data from t h e CALROC program, which had good a b s o l u t e i n t e n s i t y c a l i b r a t i o n , have been used t o compile " A Spectral A t l a s of t h e Sun be tween 1175 and 2100 A". T h i s A t l a s i s a v a i l a b l e i n t h r e e forms: a n 8x10 i n c h document , NRL Report 8056; a 1 2 x 2 1 i n c h hardbound volume, NRL Report 8057; and m a g n e t i c com- p u t e r tapes, World Data C e n t e r - A f o r Rocke t s and Sa te l l i t e s i d e n t i f i c a t i o n number RS-12A.

The a t l a s p r e s e n t s t h e a b s o l u t e i n t e n s i t y o f t w o q u i e t r e g i o n s , one l o c a t e d 300" i n s i d e t h e so l a r l i m b (case = 0 . 7 3 ) and r e p r e s e n t a t i v e o f t h e s p e c t r u m of most of t h e d i s k . The o t h e r q u i e t r e g i o n is l o c a t e d 50" i n s i d e t h e limb (cos = 0.32) and is more r e p r e s e n t a t i v e of a l i m b spectrum.' I n a d d i t i o n , t h e s p e c t r u m o f a c t i v e r e g i o n McMath 508 is pre- .

s e n t e d f o r w a v e l e n g t h s l o n g e r t h a n 1680 A. The logar i thm o f t h e specif ic i n t e n s i t y i n erg s-l s r A - l is p lo t ted v s wavelength i n Angstroms. T h e ' s p e c t r a of t h e q u i e t r e g i o n s and t h e . a c t i v e r e g i o n are p lo t ted above e a c h other o n t h e same page . T h i s f a c i l i t a t e s compar ison of d e t a i l s i n t h e t h r e e t y p e s of s p e c t r a . The wavelength a x i s i s marked i n . l A i n t e r v a l s and l oga r i thmic i n t e n s i t y l e v e l s a r e l a b e l e d i n . l o i n t e r v a l s .

For w a v e l e n g t h s be low 1400 A o n l y isolated e m i s s i o n l i n e s a r e d i s p l a y e d . The cont inuum between l i n e s is too weak t o be r e c o r d e d even w i t h t h e l o n g e s t exposure times .

(see Table 8 . 1 ) . For w a v e l e n g t h s below 1200 A o n l y t h e e m i s s i o n l i n e s a t t h e l i m b p o s i t i o n ( 5 0 " ) are shown:' t h e c o r r e s p o n d i n g s p e c t r a l f e a t u r e s o n t h e d i s k ( 3 0 0 " ) f a l l below t h e d e t e c t i o n l i m i t . The a c t i v e r e g i o n s p e c t r u m is shown o n l y a t w a v e l e n g t h s above 1680 A b e c a u s e e x p o s u r e c o n d i t i o n s d u r i n g f l i g h t d i d n o t p e r m i t re l iab le c a l i b r a t i o n for s h o r t e r wave leng ths .

I n f o r m a t i o n on t h e e x p o s u r e s used t o p r e p a r e t h e A t l a s i s g i v e n i n T a b l e 8.1. For t h e e x p o s u r e s a t 50" i n s i d e . t h e l imb and i n t h e a c t i v e r e g i o n , t h e f u l l s p a t i a l r e s o l u - t i o n of t h e i n s t r u m e n t (2'' by 6 0 " ) was used. During t h e

------------------ * M a t e r i a l fo r t h i s s e c t i o n h a s been o b t a i n e d from NRL

Report 8056, (1976) " A Spectral A t l a s of t h e Sun Between 1175 and 2100 Angstroms", by 0. K j e l d s e t h Moe, M. E. VanHoosier , J.-D. F. Bartoe, and G. E. Brueckner

e x p o s u r e s a t 300" i n s i d e t h e l i m b t h e s l i t was moved back and f o r t h p e r p e n d i c u l a r t o i t s l e n g t h , c o v e r i n g a n area of a b o u t 6 0 " by 60" on t h e so l a r d i s k . T h i s was done t o a v e r a g e t h e inhomogeneous so la r e m i s s i o n a s s o c i a t e d w i t h t h e ch romospher i c ne twork .

The q u i e t so l a r r e g i o n s were selected c a r e f u l l y t o a v o i d any so la r a c t i v i t y , c o r o n a l h o l e s , or f i l a m e n t c h a n n e l s . I n t h e case o f t h e a c t i v e r e g i o n 90% o f t h e slit w a s covered by t h e p l a g e . F i g u r e 8 . 1 is a d e t a i l e d d r a w i n g of t h e loca- t i o n of t h e s p e c t r o g r a p h s l i t i n s i d e t h e p l a g e .

I n t e n s i t y c a l i b r a . t i o n s for t h e A t l a s were made a s described i n S e c t i o n 5 of t h i s Guide . The scans p r e s e n t e d i n t h e a t l a s were smoothed by removing h lgh - f r equency n o i s e i n t h e f i l m emul s ion and pho tomet ry u s i n g a F o u r i e r f i l t e r i n g t e c h n i q u e described by Nicolas e t a l . ( 3 ) A low-frequency component caused by g r a i n c l u m p s i n t h e e m u l s i o n of s i z e 1 0

m could n o t be removed by f i l t e r i n g w i t h o u t deg rad ing the e f f e c t i v e i n s t r u m e n t a l w i d t h . These g r a i n clumps may d i s t o r t s l i g h t l y t h e i n t e n s i t i e s and prof i les . Broadening c a u s e d by t h e i n s t r u m e n t p r o f i l e h a s n o t been removed from t h e a t l a s spectra , because t h e s h a p e of t h e i n s t r u m e n t profile is n o t known i n enough de t a i l . F u r t h e r m o r e , t h e low-frequency n o i s e component s t i l l p r e s e n t i n t h e d a t a may .cause s t r o n g d i s t o r t i o n s i f d e c o n v o l u t i o n is attempted. One may. estimate t h e l i n e w i d t h s from

7 where M o i s t h e o b s e r v e d l i n e w i d t h , A X ' t h e i n s t r u m e n t a l '7 w i d t h , and

T h e o r e t i c a l c a l c u l a t i o n s u s i n g a r a y - t r a c i n g method gave a c o n s t a n t i n s t r u m e n t a l w i d t h of 0.055 A f o r a l l wave leng ths between 1200 and 2100 A. T h i s s h o u l d be r e g a r d e d a s a lower l i m i t s i n c e t h e effect of t h e f i l m emul s ion h a s n o t been t a k e n i n t o a c c o u n t . From t h e w i d t h of t h e n a r r o w e s t e m i s s i o n l i n e s i n t h e s p e c t r u m , it seems more l i k e l y t h a t t h e e f f e c t i v e i n s t r u m e n t a l w i d t h is 0.07 A .

7 t h e t r u e w i d t h of t h e l i n e p r o f i l e .

The L y a l i n e p r e s e n t e d a special problem. On t h e 1974 CALROC f l i g h t t h i s l i n e became s e r i o u s l y overexposed i n t h e l i n e c o r e , e v e n f o r t h e s h o r t e s t e x p o s u r e times a t t h e 50" and 300" p o i n t i n g s . The c e n t r a l r e g i o n (1 A wide) of t h e l i n e was t h e r e f o r e o m i t t e d from t h e a t l a s . F i g . 8.2 is a sample page from t h e A t l a s , The high r e s o l u t i o n spectra presented have been compared w i t h r e s u l t s o b t a i n e d by o t h e r s i n o r d e r t o e v a l u a t e t h e r e l i a b i l i t y of t h e absolute i n t e n s i t i e s . I n so d o i n g , care was t a k e n t o d e r e s o l v e t h e CALROC spectra t o f i t t h e lower r e s o l u t i o n of t h e o t h e r i n v e s t i g a t o r s . The agreement is i l l u s t r a t e d i n Fig. 8.3, showing t h e mean i n t e n s i t y of t h e sun a v e r a g e d

o v e r 10 A i n t e r v a l s a s g i v e n by v a r i o u s o b s e r v e r s . For t h i s f i g u r e t h e A t l a s i n t e n s i t i e s a t 300" i n s i d e t h e l imb were c o n v e r t e d t o so l a r mean i n t e n s i t i e s u s i n g t h e center- to-limb v a r i a t i o n s g i v e n by Samain e t a l . ( 4 ) . A l l t h e i n t e n s i t i e s agree w i t h i n t h e A t l a s e r ror l i m i t o f + 25%. A separate p u b l i c a t i o n is b e i n g prepared l i s t i n g the i n t e n s i t i e s a v e r a g e d o v e r ' w a v e l e n g t h i n t e r v a l s r a n g i n g from 0.1 t o 10 .0 A bandwidths .

8.1 References

1. R. Tousey, E. F. Milone, J. D. Purcell, W. Palm Schneider, and S. G. Tilford, "An Atlas of the Solar Ultraviolet Spectrum Between 2226 and 2992 Angstroms," NRL Report 7788, 1974.

3. K. R. Nicolas, G. E. Brueckner, R. Tousey, D. A. Tripp, 0. E. White, apd/R..G. Athay, submitted to ------ Solar Physics --_ (1977). C-a;.'&. /"&*, .I ;:;-,-e. { e : ) / a 7 4

! . - L.

1 ' -&' ." %

4. D. Samain, R. M. Bonnet, R. Gayet, and C. Lizambert, I------- Astron. Astrophys. -- 39, 71 (1975).

5. D. Samain and P. C. Simon, to be published in Solar ----- - Physics, --- (1977) . 6. G. J. Rottman, Trans. Amer. Geophys. UnLon 56, 1157 . -----I----- ---------

(1974).

7. L. Heroux and R. A. Swirbalus, ---- J. Geophys. - _I----___ Res. 81 r 436 (1976).

F i g u r e Capt ions

F ig . 8.1

Fig . 8.2

F i g . 8.3

P o s i t i o n of t h e s p e c t r o g r a p h s l i t i n s i d e a c t i v e r e g i o n McMath 508 on September 4, 1973.

Sample A t l a s Page

Comparison o f s o l a r mean i n t e n s i t i e s averaged ove r 10 A i n t e r v a l s . The f u l l l i n e r e p r e s e n t t h e NRL CALROC d a t a used i n t h e a t l a s . Open c i r c l e s are t h e o b s e r v a t i o n s of Samain and Simon (5) c r o s s e s t h e obser- v a t i o n s of Rottman ( 6 ) , and t r i a n g l e s t h e o b s e r v a t i o n s of Heroux and Swirba lus (7) .

N

I i M

E- . --w i i !

8~ I Fig. 3 - Position of the spectrograph slit inside active region

McMath 508 on September 4,1973. ' I

I

5.0 I I I I I I I I - - &

7 4.0-

r 5 0

v)

v)

''O 14bO 15bo 16W d 0 l8bo 19bO ' 2d00 21bO WAVELENGTH (n)

813 Fa.% - Comparison of solar mean intensities averaged over 10 A intervals. The full line represent the NRL CALROC data used in the atlas. Open circles are the observations of Samain and Simon

~~~~, crosses the observations of Rottman IS], and triangles the observations of Heroux and Swirbalus (71.

8- I Tabled - Data for Exposures Used to Make the Atlas

Date

Sept. 4,1973

Jan. 15; 1974

a : .

Target

Active Region

McMath 508

300” 2 30”

50“

.- - . .

Exposure Time (4

5.45

1.07

55.45

1.95,

9.45

31.45

39.45

3.45. :

‘9.45 .

111.45

Altitude at Start of Exposure (km)

120.4

111.3

174.0

218.7

220.1

224.8

234.2

230.6

227.4

225.9

APPENDIX A. S k y l a b Documentation*

(1) NRL/ATM Exposure Catalog

V o l . I (Rev A ) Time L i s t i n g Vol. I1 (Rev A ) J o i n t Obse rv ing Program L i s t i n g V o l . I11 (Rev A ) Target L i s t i n g

These t h ree volumes l i s t t h e t i m e , J O P , s t e p and b u i l d i n g block, t h e t a r g e t , e x p o s u r e time a n d wavelength band of each S082A (and S082B) exposure . They a l so i n c l u d e n o t e s i d e n t i f y i n g special e v e n t s , s e q u e n c e s and p o i n t i n g s .

( 2 ) NRL/ATM Miss ion E n g i n e e r i n g Data Book (Rev 'A) ----I ---- --- --_--.- -----------

T h i s catalog ( o n e volume f o r each of t h e fou r S082B cameras) lists: t h e o p e n i n g and c l o s i n g t i m e o f t h e camera s h u t t e r for each e x p o s u r e and t h e c o r r e s p o n d i n g e x a c t e x p o s u r e t i m e , wavelength band , and i n s t r u m e n t o p e r a t i n g mode; o t h e r i n s t r u m e n t s operat ing a t t h e t i m e , and t h e i r m o d e s t ' a n d a v e r i f i c a t i o n of c o r r e c t temperatures t h r o u g h o u t t h e S082B i n s t r u m e n t d u r i n g t h e e x p o s u r e .

For each e x p o s u r e , t h e v a l u e s are a l so g iven for t h e recon- s t ruc ted ("cor rec t" ) ATM r o l l p o s i t i o n , ROLL or r RR , t h e maximum e x c u r s i o n of any d i s t u r b a n c e i n t h e ATM p o i n t i n g . p o s i t i o n d u r i n g t h e e x p o s u r e , t h e S082B BIAS, t h e beta a n g l e of t h e S k y l a b o r b i t , t h e a l t i t u d e of t h e S k y l a b and i t s l i n e of s i g h t t o t h e s u n , and t h e o r b i t number.

T h i s c a t a l o g a l so i n c l u d e s t r a c e a b i l i t y c h a r t s for e a c h f i l m s t r i p , t h e temperature and r a d i a t i o n h i s t o r i e s of e a c h camera, and t r a n s m i s s i o n c u r v e s and p i n h o l e maps for each aluminum f i l t e r .

( 3 ) -----e ATM Miss ion O p e r a t i o n ----- Log ( V o l s . 1-5, and magnet ic t a p e )

T h i s catalog, prepared for 5055, l ists t h e t i m e , p o i n t i n g , o p e r a t i n g modes and o t h e r i n f o r m a t i o n , for a l l o b s e r v a t i o n s by every ATM i n s t r u m e n t (S052, S054, S05.5, S056, S082A, S 0 8 E n d H a l ) .

I t s h o u l d be n o t e d t h a t t h e ATM rolJ p o s i t i o n v a l u e s t h r o u g h o u t t h i s c a t a l o g are n o t t h e r e c o n s t r u c t e d ( "correct") v a l u e s .

------------- * . T h i s Appendix was prepared by N. P a u l Pat terson, B a l l B r o t h e r s

Research C o r p o r a t i o n .

( 5 ) R o l l Reference D e t e r m i n a t i o n Summary Report

The f i r s t three of these documents p r o v i d e i n f o r m a t i o n from which a u s e r c a n d e t e r m i n e t h e c o r r e c t v a l u e of t h e ATM r o l l p o s i t i o n (rRR = GAMMARR=EXP ROLL=ROLL), and a s c e r t a i n i ts un- c e r t a i n t y ( - + 4 0 - arc-min). The r o l l v a l u e c o r r e s p o n d s t o t h e a n g l e , i n arc-min, be tween solar n o r t h and the U P p o i n t i n g a x i s of t h e ATM ( p a r a l l e l t o t h e a x i s of t h e S082B s l i t , and a t r i g h t ang1,es t o t h e SO55 r a s t e r l i n e s ) . The e r ror and u n c e r t a i n t y of t h e telemetered v a l u e s deve loped a s a r e s u l t - of t h e f a i l u r e o f t h e star-tracker r o l l r e f e r e n c e d u r i n g t h e m i s s i o n .

The p o i n t i n g b i a s required t o c o a l i g n t h e c e n t e r of t h e S082B sl i t w i t h t h e ATM f i n e s u n - s e n s o r , and its v a r i a t i o n o v e r t h e m i s s i o n i s d i s c u s s e d i n t h e f o u r t h document.

( 8 ) ATM JOP Summary Sheets ( w i t h Shopgjng L i s t s ) , SL 1/2, SL-3, SL-4.

T h i s s e t . o f documents c o n s i s t s o f c o p i e s of p l a s t i c sheets used by t h e a s t r o n a u t operat ing t h e ATlY c o n t r o l p a n e l . These s h e e t s , w i t h g u i d e l i n e s for t h e i r u s e i n each of t h e JOPs, p r o v i d e d e x p l i c i t , s e l f - c o n t a i n e d , s t ep -by- s t ep i n s t r u c t i o n s f o r p o i n t i n g and o p e r a t i n g t h e ATM e x p e r i m e n t s i n u n i s o n . P h o t o g r a p h i c examples o f so la r f e a t u r e s , and a b b r e v i a t e d d e s c r i p t i o n s o f desired p o i n t i n g s a re shown together w i t h v a r i o u s c o m b i n a t i o n s ( " B u i l d i n g B l o c k s " ) of s i m u l t a n e o u s l y operated i n s t r u m e n t modes. Each shee t summarized a l l t h e i n f o r m a t i o n needed by S k y l a b crews and solar s c i e n t i s t s t o c o o r d i n a t e o b s e r v a t i o n s w i t h t h e d a i l y scientific objectives. A s c h e d u l e was telemetered e v e r y morning t o t h e crews, which gave s u g g e s t i o n s for o b s e r v a t i o n s and o p e r a t i n g modes, and g u i d e l i n e s for r e s p o n d i n g t o f l a r e s and o t h e r i n t e r e s t i n g e v e n t s .

T h e sheets evo lved t h r o u g h a n i t e r a t i v e p r o c e s s , d u r i n g many months of pract ice on t h e ATM s i m u l a t o r , and much d i s c u s s i o n i n m e e t i n g s between s c i e n t i s t s r e p r e s e n t i n g t h e ATM e x p e r i - menter g r o u p s . The sheets changed from o n e manned phase t o t h e n e x t . N e w JOPs were added, a few.were dropped, and t h e o p e r a t i n g s t ra teg ies were made more e f f i c i e n t and f l e x - i b l e . J O P and s tep number ings a re t h e r e f o r e n o t always t h e same from one m i s s i o n t o a n o t h e r : A simplified l i s t i n g of J o i n t Observ ing Programs fo r SL13 fo l lows :

c-2

( 9 )

J O P 1 Chromospheric N e t w o r k J O P 1 0 Lunar L i b r a t i o n C l o u d s J O P 2 A c t i v e Regions J O P 11 Chromospheric O s c i l l a t i o n s J O P 3 Flares and H e a t i n g J O P 4 Prominences J O P 1 2 C a l i b r a t i o n s J O P 5 C o n s t a n t L a t i t u d e J O P 1 3 Nigh t Sky Ob jec t s

J O P 6 S y n o p t i c O b s e r v a t i o n s J O P 1 4 E c l i p s e (deleted for SL-3) J O P 7 Atmospher ic E x t i n c t i o n J O P 1 5 Coronal Holes

S t u d i e s

J O P 8 Corona l T r a n s i e n t s J O P 1 6 D i s k T r a n s i e n t s J O P 9 Solar Wind J O P 1 7 B r i g h t P o i n t s

Because of t h e f o r m a l i t y of t h e NASA m i s s i o n protocol w h i c h r e g u l a t e d t h e i m p l e m e n t a t i o n o f t h e J O P p rograms , a sheet o f informal "Shopping L i s t " items was i n c l u d e d o n e a c h of t h e '

l a s t two manned phases. These p r o v i d e d t h e a s t r o n a u t w i t h a l ist of pet projects for e a c h of t h e e x p e r i m e n t e r g r o u p s , t h a t h e c o u l d c o n d u c t a t h i s d i sc re t ion when. t i m e . was a v a i l - able.

--__ ATM E 9 e r i m e n t s __-__-------_----------------I---_ R e f e r e n c e Book (SL 1 / 2 , SL-3 SL-4)

T h i s document is a copy o f a book used a s a t r a i n i n g t e x t and car r ied on boa rd S k y l a b for crew reference d u r i n g e a c h manned phase. It p r o v i d e s a de ta i led d i s c u s s i o n of t h e ' b a c k g r o u n d , r a t iona le and s c i e n t i f i c o b j e c t i v e s o f each of t h e J O P s . S p e c i f i c terms are d e f i n e d , and p h o t o g r a p h s are g i v e n of fea- t u r e s a s t h e y would appear i n H and XUV e m i s s i o n s . Graphs and t ab le s o f f i l t e r t r a n s m i s s i o n s , d e t e c t o r p o s i t i o n s o f XUV l i n e s , and other i n f o r m a t i o n u s e f u l t o t h e ATM o p e r a t o r a r e i n c l u d e d . I n a d d i t i o n , t e c h n i c a l d a t a is i n c l u d e d on each of t h e ATM i n s t r u m e n t s and m o n i t o r s , as w e l l as t e l e p r i n t e r a b b r e v i a t i o n s , and ATM s c h e d u l i n g c o n v e n t i o n s .

( 1 0 ) NOAA/Skylab Solar Da ta Books ---- ----------I- S e v e r a l dozen l o o s e - l e a f vo lumes c o n t a i n i n g copies of t h e so l a r p h o t o g r a p h s and da ta p r o v i d e d ATM e x p e r i m e n t e r s by NOAA d u r i n g t h e S k y l a b m i s s i o n .

(11) Skylab ATM H-Aleha A t l a s , and A t l a s Guide (49 vols.) - ----_---__ _----I---------

Copies of p h o t o g r a p h s t a k e n by t h e H . a t e l e s c o p e on ATM (Hal). A p r i n t is i n c l u d e d w i t h a scale o f 2 arc-min per i n c h , for t h e b e g i n n i n g and end of each o r b i t , for each s i g n i f i c a n t ATM p o i n t i n g change , a n d , when no p o i n t i n g change o c c u r r e d , a t 15 m i n u t e i n t e r v a l s , for t h e e n t i r e Sky lab m i s s i o n .

c-3

Roughly two dozen loose-leaf volumes containing information pertinent to the operation of N R L ' s two instruments on the ATM, logged in real-time by NRL representatives who manned consoles in the mission control center round-the-clock. These logs contain summary charts of the orbits in which the ATM was operated, and the as-flown schedule of ATM operations relative to orbital sunrise and sunset. Of particular value to users of S082B data, are notes of crew-reported solar events, operating errors, and special observations.with the S082B instrument.

This is a complete set of all voice communication between the. Skylab astronauts and the ground, of both live conversations and comments taped on an onboard recorder and dumped.. . In addition, a set of transcripts is available edited for ATM- related communications.

Detailed diagrams of ATM instruments, as well as the ATM, and the 'checklists of their operating procedures.

c-4

k Re,l s*;q AiAAL J

7 B - 6 L 7a- c 5 7 B - t 4 78- C b 7a-cc 78*7 '

7B-ca 78- 70 7D- 71 78-72 78-73 7a- 7 4 74-7s fa-TC 78- 77 96- 7d 8 A - 5 66% BA- 7 8 A -8 8 A - 3 8 A - I O ' 8 A - I 1 BA- IC 8A- I8 BA - I4

@A-17 BA-le 8 A - I 6 8A-Z0 81-21 8 A ' Z C 8 A 2 S 8 A - C+ 8 A - C C 84-27 8 h - 2 8 0 A - Z B &A-30 &i'aI ell -3L BA-JS % A - W

8 A - ) 7 ?A - a8

m - t c

8 A - 3 6

UA -39

I

!

Appendix C* 1 ! i

F;lm wr %#l

&A-40 8 A -41 8 A - 4 L 8 A - 4 3 8 A - 9 + 8 A - 4 . s BA-46

814-.C9 84-bo EA-SI 84-5L 8 A -S3 8 A - 3 V 8 A - 3 5 BA-SC 8 A - 3 7 EA-S-3 BA-60 ea -c I

811-48 .

8 A - C Z 8 A - G I 8 A - C C 8 A - 6 5 8 A - 6 6 8A-67

!;3; f a - 3 4 7 8 - 3 3 7B-JZ 78-31 76 -30 78-23 ?A-28

78-24 7 6 - 2 3 78-ZC 7B-l?t 7 k 2 0

78-18 18-17 76-IC 78-14 78-13

'~a-27 7s-cc

7a-13

- .

3 6 / m ' Dcu

Pait '$3 R 7a-11 7a-10 ta-OS

ta-7 r8-8

78-c 78-s 7rP-80 74. - 79 7A -78 ?A - 77 1 A - 7C 7A- 7 5 7A-74 '

?A-73 7A-72 7A-71 14 -53 7A -66 7A-67 7A-CC ?A-C6 7A -5* 7 A - C 3 7A-CL 7A-61 I4 -60 7A-Sd 74-37 7A-SC 74 -5Y 7 4 - b c 7A-63 7A-Sk 7A-SI 7A- 7A-49 74-47 7A-46 . 7A-4s 7A-4+ 7 A - 4 d 7A -4C ?A--It 74-40 7A-39

74-3s 7 A - 3 9 7 A - M

74-8.9

7a-5i m - 3 b 7A-3 1

7A-LI) 7A-28

. 7A-L7 . 74-CC

7A-24 7 4 - 2 3 7rr-22 7A-21 74-20 7449 7A-18 7A-/7 74.16 7a-14 7A -/3 7A-m 7a-11 74-10 ?A- 9 7A-8 74- 7 7A-c 74-5 78-37

~ A - Z J O

7a-ae 7a-30

. ' 7 0 4 L 7a-43 76 -ff 7a-41

' 78-4c 78-48 78 -45 7b-50

78-32

;:3?

7a-5t

7b-5 ta-r* 76-5r 78-5c 76-X8 7b-55 78-60 7eJ-c1 ( A - E

L I

I

* Appendix C compiled at NRL by Warren H. Funk.

1 - 7 3 I - 7 8 1-77 / -7s 1 - 7 5 , 1 -7+ I - 73 I - 7c / - I / 1 -c9 1 -ca 1-c7 1-CC I-cs /-e* 1 4 3 /- cc 1-GI I- co 1-so 1 - 6 7 1 -5c 1-SS /-s* I -s3 1 -SL 1 -s/

I -13 1-+r I -4c I -4h 1 - * 4 / -a

-42 1-91 I - f O I -33 1-38 I -3c #-as I -3+ 1-33 I -&! I'Jl 1-30 1-99 1-26 1-27 #-a- 1-26 1-23 I-& 1-21 1 -z0 1-19 I -18 1-17 / - IC / - I + I -1s t -1x / - I1 I - 1 6 I - 9 I -e 1 - I

F; /m ?all =$I2 c -47 2-+g 42-*b

9 -50 2- SI z-sa 2 -S3 2-s+ 2 - S b 2 -5s 2-cl 9- sa Z-60 2 - C I 2 - C Z 2 - c 3 x - c 4 z-c5 2-cc z - c 7 2 - C 8 z - ?O

2 - 7 1 2- 72 2-?3 2 - 7 4 I- 7 5 z- 7c z- 77 X-78 8- 79 3-81 z-ea E - B ~ =-a+ C-8s Z - B C Z-#7

P -89 P -90 z -&? 2-33 2-9+ a- 9r 2- 9c 2-97 I- 98 2- 93 E - 100

z -aa

a I aut

3-6 3- 7 3-8 3-9 3-00 3 - 8 1 3-14 3 -13 3-14 6-16

,3-17 a-re 3-19 3-20 3-2) 3-22 3-23 1-2+ * - e 5 3 -27 J - te 3-29 d-30 5-a1 3-32 d-33 3-34 3 -a*- a-36 a-3a d-35 3-40 3-41 J - g L

1 7 - 5 2 ~- 17-s.3 1 7 - 5 4 /7- 55 17- 56 17-b7 17-58 17-60 17-61 17-CL 17-c3 1 7 - c 9 17 - cs 17-66 17-C7 17-C8 17-cs 17-71 17-7z 11-71 17- 74

, 17-75 1 7 - 7 6 . 17- 77 17-76

. 17-79 17-80 17 -82 1 7 - 8 3 17-8+ 17- 83 17-86 17-87

17 -89 1 7 4

i;:; 18-c 18- 7 l a - 8 18-3 t w o 18-11 1 8 J Z /e - 13

I I

film i%L%E

/ 8 -/+ / 8 - f C 18-17 18-18 18-19 18-20 18'21 18-ZZ 18-23 18-24 18-25 16-27 18 -28 18'2% 18-36 18-31 16-32 18-33 1%-34 16 -35 10-3C

18 -33

re-41 18-92 17 -34 17 -= - 11-96 17-97 17-98 /7 -99 17-/OL 17-P4 17-23 /7-22 17-21 17- 20 17-13 17- 18 17-17 l r - 10 17-1s 17-13 /7 -11 /?-/I 11-10 1 7 - 9 17- e 1 7 - 7

18-38

/e -40

Sequence La3

/P6 1 7 - 2

16-88 ' 16-81 16-86 16-8s 16-84 I C - 0 3 16-82 16-81

16-7s

IC- 76 16- 75 16- 74 16-73 16-72 16-71 16-70 16-69 16- 68 16-66 16-63 16- t4 1 6 - 6 3 16-CZ 16-CI I 6 - G O 16-55 I C - 5 8 16-56 16- 5's l6-$4 16-53

16-51 16-50 I C - 4 9 IC-48 IC-47, 16-4s 16-44 1 6 4 3 16-92 16-41 16-40 16-3s IC-58 IC-3 7

tc-eo

IC-77

1 6 - 5 Z

ATM A 2b451 ZBQS! ZR453 28454 Z R 4 1 5 2045c 2 6 4 5 7 ZA458 z13m Z B4CO 28461 2 8 4 6 2 z8563 2 6 4 C 4 26465 Z 6 4 C C 28467 Zd468 28469 Z W 7 0 Zb471

2 8 4 73 28474 2 8 9 7 6 284 76 26477 264 78 284 7 3 26980 28481 EB+82 ZE483

2 ~ 4 7 ~

pa484 Z ~ M C

~ 6 4 8 7 2848 6

26488 28489 Z8490 2649 I Z W Z 28493 2 8494 z B431 n5496 28497 a645e 2 8 4 9 9 ZB5- d6j01

F;lh.l %/I %:

16 -36 16-39 1 6 - 3 5 16-32 16-31 16-30

16-29 16-28 16-21 16-26 1c-55 16-X3 16-22 16-it I 16-29 1c-19 I C - I B 16-17 16-15 IC-tC 16 -13 16-12 16-11 16-10 IC-b 16-8 16- 7 IC-c 16-C 17-26 17-27 17 -Z8 17-23 17 -30 1-7-31 47-32 t7 -33 1 7 -34 1 7 - 3 5 17-36 17-97 t f - 3 t 4 7 - 9 0 17-91 t7-42 1745 17-44 1 7 - 4 5 17-47 t 7-48 8 7 4 9

Sequence L o ,

6 - 25 9 - 3 4 6-6-3 8 -bL 8-St 8-5-0 8 -42 8 -47

8-45 8- 44 8 -43 8 -42 e -41 8-40 8 - 3 3 8-38 8-3s 8-35- 8 -34

8 -JL 8-31 8 - 3 0 8 - 69' 6 - 2 8 8 - 2 7 8 -LC 8 - 29 e- L J 8 - 2 2 a - 2 1 8 -LO 8 - ?a 8 - t 6 8 - 1 7 8 - IC 8 - t 4 8 -13 8 -12 8 -11 8-10 8 - 9 8 - 8 6 - 7 8 - 6

a-+c

e -33

- Dev m 4

* 4 3

t 3

!

9-8 9 - 9 a - t o 9- I 1 3-18? 9- I3 9-14 9 - I C 9 - 1 7 S- 18 9 - 1 3 9- 20 9 - 21 9 - L I Z s-23 3- 24 9- 2 5 3 - 2 7 9 - 2 8 9 - 2 9 3 - 3 0 9-31 9-db? 9-33 3 - 34 3- 3s 9 - 3 c 9 -38 9 -39 3 - 4 0 3- 41 3 - 4 2 9 -43 9 -44

. 9-46 9-4s 9 -47 9-49 9 -so S - 5 1 a -bZ 9 -53 3 -b4 9-55 9-sc 9 - 5 7 9 -;re g -co 9 - C I 3 - C Z

ATM

3 6 / 0 1 b - e 3 9-c+ 9- c c 9-cc 3 - 6 7 9 -68 9- 69 9- 70 4 -3 4 - 9 4 - c 4 - 6 4 -. 7 + - 8 4 - 9 +- 10 4 - 1 1 4 -13 4 - 1 4 4 - 1 6 4 - I6 4 - I 7 4 -18 4 - 1 9 4 -CO 9 - 2 1 4-22 4 - 2 4 4 - 2 6 4 -26 4 - 2 7 4 - 2 8 4 - 2 9 4 - 3 0 4 -31 4 -32 4 - 3 3 . 4 - 3 s 4 -36 4-37 4-38 4 - 3 9 4 -40 4 - 4 1 9-42 4 - 4 s

a - l o r 8 - 101 8 - 1 0 0 e- 33 8 -98 8 - 9 7 8- 96 e- 35 8 -94 8- 33 e-=# a -90 8 - 8 9 8 - 80

6 - 8 6 8 - 8 5 8 - 8 + 8 - 6 3 e - 8 2 . 8 -80 B - 73 8 - 7 8 8 - 7 7 8-?6 8 - 7 s 8 - 7 4 8- 73 8 - 7 2 8 - 70 8 - 6 ¶ 8 - C 8 8 - 6 7 8 -cc 8 -6s 8 -64 8-63 8-62 8 - 6 1 8 -60

B-S7

e -87

e-sa e-s6

I

1 A5ay 1 977.

(Commences with the initiation of the ATM Project and includes all publications and papers based on S082R and B material up to the present. )

1.

11.

111.

IV.

v. VI.

VI1 .

Professional Publications Published or in Press

Professional Publications - Submitted

Abstracts .

ProPessional Talks - Invited

3?ro!.jssional Talks - Contributed

Colloquia

0th er Public ations

I. PROFESSIONAL PUBLICATIONS - PUBLISHED OR IN PRESS

1457

1481

1489

1502

i5i5

1517

1518

1522

1529

1548

1549

1566

1570

Apollo Solar Experiments - Paving the Way for Advanced Space I t

Observatories", Winter, T. C., Jr. 1969, Astronautics and Aeronautics, March, p. 64.

I ?: Observations of the Extreme Ultraviolet Solar Spectrum", Tousey, R. 197 1, in 'A Discussion on Solar Studies with Special 'R.eference to Space Observations', Phil. Trans. Roy. SOC. Lond. A 270, 59. (Invited)

Semi-Autoniatic Acquisition of Es t r em6 Ultraviolet Reflectance' Data for Calculating Optical Constants", Hunter, W. R. 1970, Rev. Sci. Instr. 41, 1419.

"Spectral'Radiance of the Carbon A r c Between 2500 R t z , E. E. 1:971, Appl. Opt. - 10, 813.

- ?I

- and 2900 At',

. .

Survey of New Solar Results", Tousey, 'R. 1971, in 'New Tech- 11

niques in Space Astronomyt, IAU Symp. - 41, 223, ed. F.'Labulzn and R. Lust, Reidel, Dordrecht.

"High Angular Resolution Absolute Intensity of the Solar Continuum f rom 1400 A to 1790 A", Brueckner, G. E., and Moe, 0. I(. 1972, Space Research XII, Vol. 2, 1595, ed. S. A. Bowhill, L. D. Jaffe, and M. J. Rycroft, Akademie-Verlag, Berlin.

'Developments in Applied Spectroscopy', Vol. 10, 19 1, ed. A. J. Perkins, E. L. Grove, E. F. Kaelble and J. E. Westermeyer, Plenum, .New . . .York. (Invited)

Solar Spectroscopy f rom Space Vehicles", Tousey, R. 1972, in I I

High Angular. Resolution Observations from Rockets : Solar XUV I t

Observations",' .Tousey, E. '1 972, Space Research XII, Vol. 2, 1719, ed. S. A. Bowhill, L. D. Jaffe, and M. J. Rycroft, Akademie- Verlag, Berlin. (Invited)

"On the Classification of Some Highly Ionized Iron and Nickel Lines in the 200-400 A Region of the Solar Spectrum", Widing, K. G., .

Sandlin,.G. D., and Cowan, R. D. 1971, Astrophys. J. - 169, 405.

ment", Bohlin, J. D. 1972, Appl. Opt. - 11, 961. Simultaneous. Optical Monitoring of Angu?ai- and Translational Align- I?

"Extreme Ultraviolet Solar Images Televised In-Flight with a Rocket- Borne SEC Vidicon System", Tousey, R. and Limansky, I. 1972, ,

Appl. Opt. - 11, 1025.

"Rocket Observation of A r XII-XVI and Ca XN-XVIII in the XUV Spectrum of a Solar Flare", Purcell, J. D. and Widing, K. G. 1972, Astsophys. J. - 176, 239.

"Cleaning of Contaminated Channel Electron Multiplier Arrays", '

Harlow, F. E. andHunter, W. R. 1972, Appl. Opt. 11, 2719. - 1-1

1573 '' Comparison of an Aluminum-Coated Phosphor Layer and a Channel- t ron Electron Multiplier Array a s Extreme Ultraviolet -to-Visible Image Converters for U s e in Space Applications", . Hunter, w.. R . , and Harl.ow, F. E. 1973, Appl. Opt. - 12, 968.

The Extreme-Ultraviolet Spectrum of Fe XV i n a Solar Flare"., Cowan, R. D. and Widing, K. G. 1973, Astrophys. 3'. 180, 285.

' I ' New' Stigmatic, Coma-free, Concave Grating Spectrograph, 'I

Bartoe, J. -D. F. and Brueckner,-G. E., 1975, JOSA 6 5 , 13.

'I The Increase in Transmittance of Unbacked Aluminum Filters Exposed to R F and DC Discharge in Oxygen", Hunter, W. R. , ..

"A Preliminary Study of the Extreme Ultraviolet Spectroheliograms f rom Skylab", Tousey, R., Bartoe, J.-D. F., Bohlin, J. D., Bruecltner, G. E., Purcell, J. D., Scherrer, V. E., Sheeley, N. R., Jr., Schumacher, R. J. andVanHoosier, M. E. 1973, Solar Phys, 33, 265.

"The Extreme Ultraviolet Spectrograph", Bartoe, 5. -D. F., Brueckner, G. E., Purcell, J. D., and Tousey, R. 1974, SPIE 44, 153.

I 1 1579 -

1603 -

1606

. Steele, G. 'N. and Gillette, R. B. 1973, Appl. Opt. - 12, 2800. . .

1620 .

. .. - 1642

- On the Fe X X N Emission i n the Solar Flare on June' 15, 1973",

Widing, K. G. and Cheng, C. C. 1974, Astrophys. J. Lett. 194, L111.

"Structure of the Sun's Polar Cap in the Wavelengths 240-600 A", Bohlin, J. D., Sheeley, N. R., Jr., andTousey, R., 1975 Space Research X V , 651, ed. Akademie-Verlag, Berlin.

"Preliminary Results from the NRL/ATM Instruments from Skylab 211, Tousey, R . , Bartoe, J. -D. F.. Bohlin, J. D., Brueckner, G. E., Purcell, J. D., Scherrer, V. E., Schumacher, R. J., Sheeley, N. R . , Jr., and Van Hoosier, M. E. 1974, in Coronal Disturbances', p. 491, ed.. G. Newkirk, Jr., Reidel, Dordrecht.

"Implications of NRL/ATM Solar Flare, Observations on Flare Theories", Cheng, C. C. and Spicer, D. S. 1975, in 'Solar Gamma-, X-, and EUV Radiation.', p. 423, ed. S. R. Kane, Reidel, Dordrecht.

I t 1647 -

1650

1652

- .

1655

1666 "Some Reflections on the Use of Conventional and Holographic Diffraction Gratings in the Vacuum Ultraviolet Spectral Region", Hunter, W. R. 1974, Proc. IV International Conf. on Vacuum- Ultraviolet Radiation Physics, p. 683; .

"Diffraction Gratings for the X W - Conventional vs. Holographic", Hunter, W. R. 1974, Japanese J. of Spectroscopical SOC. 23,. 37.

167 1 .-

1673 I t Flare-Like Ultraviolet Spectra of Active Regions", Brueckner; G. E. 1975, i n 'Solar Gamma-, X-, and EUV Radiation', 105, ed. S. R. Knne, Reidel, Dordrecht.

1675 "TJltraviolet Emission Line Profiles of Flares and Active Regions", Brueckner, G. E. 1.975, in S o l a r Gamma-, X-, and E W Radiation', 135, ecl. S. R. Kane, Reidel, Dordrecht.

The Fine Structure of the Solar Atmosphere in the.Far Ul t ra - violet", Brueckner, G. E. , and Bartoe, J. -D. F. 1974, Solar

'Phys. 38, 133.

"Fe XXIV Emission in Solar Flares Observed with.the NRL/ATM X.W Slitless Spectrograph", Widing, K. G. 1975, 'Solar Gamma-,

I I 1676

_. . 1677

.. X-, and EUV Radiation', 153,. ed. S. R. Kwe, Reidel, Dordrecht.

1678 . "Flares C:3served by the NRL/ATM Spectrograph and Spectrohelio- gram During the Skylab Missions", Scherrer, V. E. and 'i'uusey, R. 1975, Proc. International Conf. on 'X-rays i n Space', Vol. II, 986,

. Univ. of Calgary.

1683 "Observations of the Hydrogen Ly-cu (1216 A) Emission Line of Comet Kohoutek (1 973f) by the SkylabIATM S082B Spectrograph", Keller, H. U., Bohlin, J. D., and Tousey, R. 1975, Proc. Comet Kohoutek Workshop, NASA SP-355, ed. G. A. Gary.

"High Resolution Ly-a Observations of Comet Kohoutek by Skylab and Copernicus", Bohlin, J. D., Drake, J. F., Jenkins, E. B., and Keller, W. U., Proc. IAU Colloq. 25, 'The Study of Comets', Part 1,

"XUV Observations of Coronal Magnetic Fields", Sheeley, N. R., Jr., Bohlin, J. D., Brueckner, G. E., Purcell, J. D., Scherrer, V. E., and Tousey, R. 1975, Solar Phys. 40, 103.

Multiplet Tables; NI, MI, NIII", Moore-Sitterly, C. E. 1975, NSRDS-NBS 3, Section 5.

"Observed Heights of EUV Lines Formed in the Transit ion Zone andCorona", Simon, G. W., Seagraves, P. H., Tousey, R., Purcell, J. D., Noyes, 1:. W. 1974, Solar Phys. 39, 121.

"Ultraviolet Solar Identifications Based on Extended Absorption Series Observed in the Laboratory Spectra of Si I", Moore, C. E., Tousey, R., Sandlin, G. D., Brown, C. M., Ginter, M. L., andTilford, S. G., 1975, Astrophys. and Sp. Sci., 38,-359.

1684

- NASA SP-393, 315.

1686

- Selected Tables of Atomic Spectra; Atomic Energy Levels and I' 1688

1687

- 1689

-

1691

1692

1695

1709

1713

1715

1716

1718

Erilptive Prominences Recorded by the XUY Spectroheliograph on I I

Sl;yl;iS", Tousey, R. 1976, Atmosphere', Phil. Trans. Roy. SOC. Lond. A 281, 359.

"High Resolution Ly CY Observations of Comet Kohoutelc Near Perihelion", Keller, H. U., Uohlin, J. D., and Tousey, R. 1975, Astron. and Astrophys. 38, 413.

"A Comparison of Spicules in the Ha and He I1 (304 A) Lines", Moe, 0. K,, Engvold, E. and Beckers, J. 1975, Solar Phys. 40, 65. .

Sheeley, N.R., Jr., Bohlin, J. D., Brueckner, G. E., Purcell, . J. D., Scherrer , V. E., and Tousey, R. 1975, Astrophys. J. Lett. 196, L129.

"Forbidden Lines of Highly Ionized Iron in Solar Flare Spectra", Doschek, G. A, , Feldman, U., Dere, K. P., Sandlin, G. D., Van EIoosier, M. E., Brueckner, G. E., Purcell, J. D., and Tousey, R. 1975, Astrophys. J. Lett. - 196, L83.

"XUV Results from Skylab", Tousey, R. 1975, Proc. International Conf. on 'X-Rays in Space1, Vol. I, 472, Univ. of Calgary. (Invited)

"The XUV Sun a:, Observed by ATM S0.82", Tousey, R. ,: Proc. of AIlsAIAGU Space Scient;:. Conf. on 'Scientific Experiments of

"Classification of F la re s and Flare-Like Events Observed by the ATM XUV :;pectroheliograph SO82A and Spectrograph S082B During the Skylab Missions!', Scherrer, V. E. and Tousey, R., Proc. of AIAA/AGU Space Science Conf. on 'Scientific Experiments of Project Skylab', in press .

'A Discussion on the Physics of the Solar

. -

- .

The Reconnection of Magnetic Field Lines in the Solar Corona", . ?I

-

.

Project Skylab', in press . . ..

1720 I' The Stark Broadening Mechanism in an Unstable Plasma", Spicer, D. S. and Davis, J. 1975, Solar Phys. - 43, 107.

"On the Fe XXIV Emission in the Solar F l a re of 1973 June 15", Widing, K. G . and Cheng, C. C. 1974, Astr'ophys. J. Lett. - 194, L115.

"Fe XXIII 263 %, and Fe XXIV 255 Widing, K. G. 1975, Astrophys. J. Lett. - . 197, L133.

1721

1724 Emission in Solar Flares",

1727 "A Newly Observed Solar Feature: Macro-Spicules in He I1 304 AI', Bohlin, J. D., Vogel, S. N., Purcell, J. D., Sheeley, N. R. ,Jr . , Tousey, R., and Van Hoosier, M. E. 1975, Astrophys. J. Lett. - 197, L133.

"'J.'he 1640.4 A Ha Line of He I1 Observed from Skylab", Feldman, U., Doschek, G. A., Van Hoosier, M. E., and Tousey, R. 1975, Astrophys. J. Lett. 199, L67.

1729

-

1-4

1733 "XTJV Emission from Above the West Limb N e a r 20:OO U.T. , January 17, 1974"', Tousey, R. 1975, Astrophys. and Sp. Sci,, 1701. 38, 327. -

11 1741 "ATM Observations of the XUV Emission from Solar Flares, Brueckner, G. E. 1976, 'A Discussion on the Physics of the Solar Atmosphere', Phil. Trans. Roy. SOC. Lond. A 281, 443.

"Spatial Distribution of .XUV Emission i n Solar Flares", Cheng, C. C. and Widing, K. G. 1975, Astrophys. J. - 201, p. 735.

It The Interpretation of Ultraviolet Solar Spectra", Moore-Sitterly, C. E., Proc. Twentieth Liege International Astrophysical Symp. , . 1975, Mem. de la Societe Royale de Liege - 9, p. 59.

Sheeley, N. R. , Jr. , Bohlin, J. D., Brueckner, G. E. , Purcell, J. D., Scherer, V. E., Tousey, R. , Smith, J. B., Jr., Speich, D. M., Tandberg-Hanssen, E. , Wilson, R. M. , de Loach, A. C. , Hoover, R. B., and McGuire, J. P. , Solar Physics - 45, p. 377.

1745

1748

I t Coronal Changes Ass.ociated with a Disappearing Filament, I t 1749

1760 "Absolute Solar Intensities 1750 A-2100 and their Variations with Solar Activity", Brueckner, G. E. , Bartoe, J. -D. F., Moe, 0. K., T;an Eoosier, M. E. 1975, Proc. of the Workshop: The Solar Constant and the Earth's Atmosphere, p. 71.

"Selected Tables of Atomic Spectra, Atomic Energy Levels and Multiplet Tables OI", Moore-Sitterly, C. E. 1976, NSRDS-NBS 3, Sec. 7.

"Limb Brightening Curves of XUV Transit ion Zone Lines i n the Quiet Sun and in a Polar Coronal Hole Observed from Skylab", Doschek, G . A. , Feldman, U. and Tousey, R. Astrophys. J.

"The Intensities and Profiles of XUV Transition'Lines in a Quiet Sun Region Compared to a Polar Coronal Hole", Feldman, U. , Doschek, G . A. andTousey, R. Astrophys. J. Lett. - 202, L151.

"Advances in X-Ray and EUV Spectroscopy of Solar F l a re s and Laboratory Plasmas", Doschek, G. A. 1975, Proc. International Conf. on 'X-Rays i n Space', Vol. I, p. 306.

1762

1765

. Lett. 202, L147. - .

1766

1773

1783 . "The Calculation of Force-Free Fields from Discrete Flux Distributions , It Sheeley, N. R. , Jr., and Harvey, J. W., Solar Physics - 45, p. 275.

Energy Released by the Interaction of Coronal Magnetic Fields, Sheeley, N. R . , Jr., Solar Physics - 47, p. 173.

"Synoptic Maps of Coronal Hole Boundaries Derived from He It 304 A Spectroheliograms from the Manned Skylab Missions, I t

, Bohlin, J. D. and Rubenstein, D. M. 1975, World Center A for Solar-Terrestrial Physics, N O M , Report UAG-51.

II I t 1789

. _

1795

'

1-5

1796 "The Emission Line Spectrum Above the Limb of the Quiet Sun: 1100-1910 Angstroms. I' Doschek, G. A . , Feldman, U. , Van Hoosier, M. E. and Bartoe, J. -D. E'. 1976, Astrophys. J. Supp. Series - 31, 417.

1797

1799 .

1800

1804

1806

1807

1808

1810

1812

The Emission Line Spectrum Above the Limb OE a Solar Coronal Hole: 1100-1 940 Angstroms, Van Hoosier, M. E. and Pu:*cell, J. D. 1976, Astrophys. J. Supp. :izries 31, 445.

"The Lithium-Like 2s S-2p P Transition in Solar Flares,

I 1

I 1 Feldman, U. 8 Doscheck, G. A. 8

. -

I t 2 2

Widing, K.. G. and Purcell, J; D. 1976, Astrophys. J. Lett. - 204, L151. '

I t "High Temperature Flare Lines in the Solar Spectrum 171 -630w, Sandlin, G. D. , Brueckner, G. E., Tousey, R. and Scherrer, V. E. 1976, Astrophys. J. Lett. - 205, L47.

"Space-Resolved Spectra of Laser-Produced Plasmas in the XUV, I' Feldman, U., Doschek, G. A . , Prinz, D. IC. andNagel, D. J. 1976, J. of Appl. Phys. - 47, No. 4, 1341.

"The Profile of the Solar Lyman Beta Line of Hydrogen, K. R. , Moe, 0. K . , Bartoe, J. -D. F. and Tousey, R. 1976, J. of Geophys. Res. - Space Physics - 81, 3465.

"Effects of l'lasma Microfields on Radiative Transients from Atomic Levels Above the Ionization Threshold, Davis, J. and Jacobs, V. L. , Phys. Rev. A 12, 2017.

"High Latitude Observations of Solar Wind Streams and Coronal Holes, Rickett,, B. J. 8 Sime, D. G. , Sheeley, N. R. , Jr., Crockett, W. R. and Tousey, R. 1976, J. of Geophys. Res. - 81, 3845. -.

I 1 Nicolas,

I t

- I t

The Sources of Material Comprising a Mass Ejection Coronal I t

I t .Transient , Hildner, E.., Gosling, Ji T. 9 Hansen, R. T. and Bohlin, J. D. 1975, Solar Physics - 45, 363.

"Doppler Wavelength Shifts of Transition Zone Lines Measured i n Skylab Solar Spectra, " DoSCheCk, G. A. 8 Feldman, U. and Bohlin, m 1 9 7 6 , Astrophys. J. Lett. . - 205, L177.

. . : I t 1813 "Polar Faculae During the Interval 1906-1975, 1976, J. of Geophys. Res. - 81, 3462.

Instabilities and Their Possible Role in a Pre-Flare Energy Build- up, Solar Physics - 47, 127.

Sheeley, N. R., Jr.

._ . . Spectroscopic Far Ultraviolet Observations of Transition Zone

Brueckner, G. E., Patterson, N. P. and Scherrer, V. E.

11 1814 I 1

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1817

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1822

1824

1826

1827

1837

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1845

. _ ' 1850

1851

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1869

Absolute Solar Ultraviolet Intensities and Their Variations with . 11

Solar Activity Part I: The Wavelength Region 1750A - 2100A, I'

Brueckner, G. E., Bartoe, J. -D.. F., Moe, 0. K., and Van Hoosier, M. E., Astrophys. J. - 209, 935.

Observation of a Kink Instability i n a Solar Flare, .I1 Cheng, C. C., 1 1

Astrophys. J. - 213, 558.

"Thin Aluminum Filters for U s e on the Apollo Television Monitor Flown on Skylab, Opt. - 16, 904.

Feldman, U., Davis, J. and Cowan, R. D., .Phys. Rev. A - 12, -980.

Schumacher, R. J. and Hunter, W. R., Appl.

11 . Density Sensitive Lines of Highly Ionized Iron, I' Doschek, G. A.,

"Transitions of Zn XXII, Zn XXTII, ZnxxTv, G e XXIV and Ge 2 K V Observed in Laser-Produced Plasmas, I' Behring, W. E., Cohen, Leonard, Doschek, G. A. and Feldman, U., JOSA. - . 66, 376.

"NRL/ATM Extreme Ultraviolet Solar Image Television Monitor. Flown on Skylab, Crockett, W. R. , Patterson, N. P., Purcell, J. D., Schumacher, R. J. andTousey, R., Appl. Opt. -. 16, 893.

The Emission Line Spectrum of a Sunspot in the Far Ultraviolet," 11

Cheng, C. C., Doschek, G. A. and Feldman, U., Astrophys. J. .210, - 836.

"The XUV Spectrum. of C I Uherved from Skylab During a Solar Flare, Feldman, U., Brown, C. M. 8 Doschek,G. A,, Moore, C. E. andRoseriberg, F. D. 1976, J. Opt. Soc. Am. - 66, 853.

Coronal Holes, Solar Wind Streams and Recurrent Geomagnetic Disturbances: 1973-1976,'' Sheeley, N. R., Jr., Harvey, J. W. and Feldman, W. C., Solar Physics - 49, 271.

."Emission Measures, EJectron Densities and Nonthermal Velocities from Optically Thin UV-Lines Near a Quiet Solar Limb, " Kjeldseth Moe, 0. and Nicolas, K. R., Astrophys. J. - 211, 579.

"The Quiet Sun Chromospheric Network Observed from Skylab, " Feldman, U., Doschek, G. A. and Patterson, N. P. 1 9 r Astrophys. J. - 209, 270.

I t

11

The Influence of Autoionization Accompanied by Excitation on Dielectronic Recombination and 1onization.Equilibrium.. Jacobs, V. L., Davis, J., Kepple, P. C. and Blaha, Me, Asti..,nhys. J. 211, 605.

"The Emission Spectrum of the Hydrogen Balmer Series Observed Above the solar Limb from Skylab I. A Quiet-Sun and Polar Coronal Hole, Astrophys. 3, - 212, 905

I I

11

-

11 Roseir.berg, F: D., Feldman, U. and Doschek, G. A.'

1872

1875

1876

1880

1883

1885

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1899

1900

1901

1904

. 1906

1922

"?'he Profile OF the 977 A Line of C 111, auc! Eartoe, J. -D. F. I>.i:ysical Output of the Sun, 1976, i n press.

Appl. Opt. 16, 825.

"The Solar XUV Grazing Incidence Snectrograph on Skylab, 'I Garrett, D. L. andTousey, R., Appl. Opt. (6 , 898.

"The Emission Spectrum of the Hydrogen Balmer Series Observed

a d Doschek, G. A. , Astrophys. J. 212, 913.

"Exploring the Ear th ' s Atmosphere by Photography from Skylab, 'I

Packer, D. M. and Packer, I. G. , Appl. Opt. 16, 983.

"The Extreme Ultraviolet Spectrograph ATM Experiment SO 82B, 'I Bartoe, J. -D. F., Brueckner, G. E., Purcell, J. D. and Tousey, R., Appl. Opt. - 16, 879.

"The 3s-3p and 3p-3d Lines of Mg I1 Observed Above the Solar Limb f rom Skylab, 'I Feldman, U. and Doschek, G. A., Astrophys. J: Lett. 21.2, L 147. . .

I I CIhservinG and Recording Instanteous Images on ATM Television Monitors, Patterson, N. .,P., Tousey, It. and Delamere., W. A.,

"Experience with Schumann-Type XUV Film on Skylab, Van Hoosier, M. E., Bartoe, J. -D. F., Brueckner, G. E., Pztterson, N. P. and Tousey, R., Appl. Opt. 16, 887.

"The Extreme Ultraviolet Spectroheliograph ATM Experiment. SOSZA," Tousey, R, Bartoe, J. -D. F., Brueckner, G. E. and Purceli, J. D., Appl. Opt. 16, 870.

"Chromospheric Limb Spectra from Skylab: 200 to 3200 8, 'I

Doschek, G. A. and Feldman, U. , Astrophys. J. Supp. Series 33, 101.

"Enhancement of Dielectronic Reombination by Plasma Electrlc Microfields," Jacobs, V.. L., Davis, J. and Kepple, P. C., Phys. Rev. Lett. 37, 1390.

"Electron Impact Excitation Coefficients for Laboratory and Astrophysical Plasmas, 'I Davis, J., Kepple, f. C; and Blaha, M. , J. Quant. Spectrosc. Radiat . Transfer, Vol. 16, 1043.

Moe, 0. K., Nicolas, K. R. Contribution to the NASA Workshop on the

"The Apollo Telescobe Mount of Skylab - An Overview, I t Tousey, R.

- -

AI.)ove the Solar Limb from Skylab Ii. Active Regions, II Feldman, U. -- .

-

-.-

... . . Appl. Opt. 16, 922. . . -

-

-

-

-

-

1-8

11. PROFE3SIONAL PUBLICATIOXS - SUBMITTED

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1886

1887

1894

,1898

1902

1905

1908

1917

1918

A Comment on the Acceleration of Charged Particles i n the 11

I 1 Presence of Micro-Turbulence as R.elated to Solar Flares, Spicer, D. S. Research Note submitted to Solar Physics.

Extreme-Ultraviolet Observations of Coronal Holes: I. Locations, .. . I 1

I 1 Sizes and Evolution of Coronal Holes June 1973 - Januaiy 1974, Bohlin, J. D. Submitted to Solar Physics.

"Emission Measures and Structure of the Transition Region of a .. Sunspot from Emission Lines in the Far Ultraviolet," Cheng, C. C. arid Moe, 0. K. Submitted to Solar Physics. I 1 . Observations of the 0 and Absorption Cross Section in the Vicinity of 13-Lyman Alpha, I '

Prinz, D. I<. and Brueckner, G . E. Submitted to J. of Geoplys. Res.

Mu.ltiple Loop Activations .and Continuous Energy Release in the Solar Flare of 1973 June 15, Submitted to Solar Physics.

Column Density Between 120 km and 70 km

I1

I 1 Widing, K. G . and Dere, K. P.

"Solar XUV Emission Line Profiles of Si I1 and Si 111 and Their Center to Limb Variations, I ' Nicolas, IC. R., Brueckner, G. E., Tousey, R., Tripp, D. A. , . White, 0. R. andRthay, R. G. Submitted to Solar Physics.

I 1 Comparison of Flare Bremsstrahlung Resulting from Energetic Thermal and Non-Thermal Electrons, Davis, J. and Rogerson, J. E.

"The Thermal and Non-Thermal Flare: A Result of Non-Linear Threshold Phenometja During Magnetic Field Line Reconnection, I t

Spicer, D. S .

"Forbidden Lines of the Solar Corona and Transition Zone AX955 A - 3000 A," Sandlin, G . D., Brueckner, G. E. and Tousey, R. Submitted to Astrophys. J.

Observations, Dere, K. P., Horan, D. M. and Kreplin, R. W. Submitted to Astrophys. J.

I 1

Submitted t o Solar Physics.

Submitted to Solar Physics. . - .

Structure and Dynamics of a Solar Flare: X-Ray and XUV I t

1 1

"A Pictorial Comparison of Intetplanetary Magnetic Field Polarity, Solar Wind Speed and Geomagnetic Distrubance Index During the Sunspot Cycle, and Harvey, J. IV. Submitted to Solar Physics.

11 Sheeley, N. R., Jr., Asbridge, J. R.; Bame, S. J.,

"Plasma Diagnostics Using High Resolution Spectroscopic Techniques, It Feldman, U and Doschek, G. A. Submitted J. Opt. SOC. of Am.

11-1

1919 "XUV Spectra of the 15 June 1973 Solar Flare Observed from Skylab I. Allowed Transition in Chromospheric and Transition Zone Ions, ' I Doschek, G. A., Feldman, U. and Rosenberg, F. D. Submitted t o Astrophys. J.

"XUV Spectra of the 15 June 1973 Solar Flare Observed from Skylab 11. Intersystem and Forbidden Transitions i n Transition Zone aiid Coronal Ions, Rosenberg, F. D.

"High Resolution Spectra of the Solar Mg I1 h and k Lines, Doschek, G. A. and Feldman, U. Submitted to Astrophys. J.

1920

I 1 Feldman, U., Doschek, G. A. arid Submitted t o Astrophys. J.

II 1936

Suppl.

A Search for a Turbulent Free Region in the Solar Transition Zone, Feldman U. and Doschek, G.. A. Submitted to Astrophys. J. .

"On the Problem of Density Diagnostics for the EUV Spectrum for the EUV Spectrum of the Solar Transition Zone, I ' Doschek, G . A. and Feldman, U. Submitted to Astronomy and Astrophys. Lett.

I 1 1937

1938

Elec t ros ta t ica l ly Unstable Heat Flow During Solar F la res and 1941 'I

its consequences, Spicer,. D. S. Submitted to Solar Physics.

A Survey' of Coronal Holes and Their Solar l.'.:ind Associations Throughout Sunspot Cycle 20, Jr., Tousey, R. and Underwood, J. H. Submitted .to Solar Physics.

II

' . . 11

I f 1946

Broussard, R. M., Sheeley, N. R. ,

..

11 -2

m. ABSTRACTS

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. .

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1572

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1625

1626

1628

1629

Absii:ln te Intensity of the Continutiin in the Ultraviolet Spectrum II

of ?:!e: Sun Between 1650-1800 A'', Brueckner, G. E. , Mae, 0. K., aI:G .l?.tk., E. , BAAS 3, 260 ( 3 . ')7 1).

iiigi.: Spectral ani[ Spatial Resolution Ultraviolet Spectroscopy of the St:::?. in the R-egion 1.170-1800 w", Brueckner, G. E., BAAS 3, 259 (1971).

- II

-

On the Classification of Some Highly Ionized Iron and Nickel Lines in the 200-400 A Region of the Solar Spectrum", Widing,' K. G.. and, Sandlin, G. D., Cowan, R. D., Sp. Sci. Rev. - 13, 665 (1972).

Extreme Ultraviolet Spectroheliograms of a Solar Flare", Purcell,

I I

. II

J. D. and Tousey, R., BA.AS - 3, 448 (1971).

"Prelimina5y Results of Identifications in the XUV Spectrum of a Solar Flare , Purcell, J. D., Tousey, R., and Widing, K. G., BAAS 3, 448 (1971).

"The Coronal Origin of a Solar Flare", Brueckner, G. E., BAAS 4, 378 (1972).

- -

"A Recalibmtion of Spectral Radiance of Mercury and Deuterium Arc Standard Lamps in the Near UV", Bartoe, .J. -D. F. and Ott, W. R., J. Opt. SOC. Am, 62, 1372 (1972).

"The 1175 .%, to 1900 A Ultraviolet Spectrum of Solar Flares", Rrueckner, G. E., Bohlin, J. D., Moe, 0. K., Nicolas, K. R., %.'Lircell, J. D., Scherrer, V. E., Sheeley, N. R., Jr., and 'j.'ousey, R., BAAS - 6, 285 (1974).

"Electron Density from Line Ratios in the XUV Spectrum of .a Solar Flare", Widing, K. G., Purcell, J. D., and Tousey R., BAAS - 6, 297 (1974).

"The Screw Pinch and the Solar Flare", Spicer, D. S. and Cheng,

. . . .._ - .

c. c., BAAS - 6, 294 (1974). A Preliminary Study of Coronal Structures by Means of Time- II

Lapse Photography", Sheeley, N. R., Jr., Bohlin, J. D., Brueckner, G. E., Purcell, J. D., Scherrer, V. E., and Tousey, R., BAAS - 6, 294 (1974).

"Rocket Spectroheliogram Observations of the Heights of Forma- tion and Sizes of Bright Features in the Transit ion Zone", Simon, G. W.8 Seagraves, P, H., and Tousey. R., BAAS - 6, 294 (1974).

Cinematographic Observations for ATM and Their Comparison ? I

with Some ATM Results", Zirin, H., Holt, J., Brueckner, G. E., Bohlin, J. D., Purcell, J. D., Scherrer, V. E., Sheeley, N. R., Jr., and Tousey, R., BAAS - 6, 298 (1974).

111-1

1637

1657

1657

1658

1 6.68

1674

1685

11 Si;iicjj.e..; of Atmospheric Extinction frani Skylab", Brown, C. M. , l'c,:W?;;-, R.. , Tilford, S. G., and Pr i t i z , D. K., EOS 55, 371

I_

(19-;4),

C or.ona1 Extreme Ultraviolet Spectroheliograph and Chromospheric 11

Extreme Ultraviolet Spectrograph", TOUSSY., BAAS 6 , 297 (1 974).

'"The Extreme Ultraviolet Spectrograph", Bartoe, J. -D. F. , Bruecknar, G. E., Purcell, J. D., and Tousey, R., SPIE.. 'Instrumentation in Astronomy - II', 1974, SPIE 44, 153.

"Skylab Observation of the White Light Corona and the He I1 304 A C.'. tiromos phere During the Eruptive Prominence Event of Aigust 2 I , 1973", Bohlin, J. D., Brueckner, G. E., Purcell, '

J. D., Scherrer, V. E., Sheeley, N. R . , Jr., Tousey, R., Poland, A. I . , EOS S5, 409 (1974).

- .

- The Eruptive Prominence of August 21, 1973, Observed from Skylab I I

in the White Light Corona and in the He I1 304 Poland, A. I . , ,Bohlin, J. D., Brueckmr, G. E., Purcell, J. D., ,

Scherrer, V. E., Sheeley, N. R., Jr,, and Tousey, R., BAAS 6 219 (1974).

Chromosphere",

-.

Preliminary Results f rom the Extreme Ultraviolet Spectro- heliograph and Ultraviolet Spectrograph on ATRI", Tousey, R., EOS 55, 408 (1974).

"Skylab Observations of the Sun (170-630 A) with the NRL Objec- tive Grating Spectroheliograph", Widing, K. G., J. Opt. SOC. Am. - 64, 1375 (1974).

NRL Spectrograyh onboard Skyla'l,", Brueckner, G. E., J. Opt. Soc. Am. 64, 1375 (1974).

"ATM Observations on the XUV Emission from Flares", Brueckner, G. E., Astmphys. and Sp. Sci., in press.

? I

-

Spectrophotometry of the Solar Ultraviolet Line Spectrum with the 11

-

Ibid., Stanford Univ. Inst. for Plasma Res. Report No. 594 (19741, - 1695 "A Catalog and Classification of Flares and Flare-Like Events

Observed by the ATNI 'XUV Spectrograph S082A and Spectro- heliograph SO82B",. Scherrer, V. E., Tousey, R., and Sandlin, G. D., BAAS - 7, 356 (1975).

I' Polar Plumes in X W Emission-Line'Corona", Bohlin, J. D., Purcell, J. D., Sheeley, N. R., Jr., and Tousey, R.; BAAS - 7, 356 (1975).

"Macro-Spicules in He I1 304 %i Over the Sun's Polar Cap", Bohlin, J. D., Vogel, S. N. , Purcell, J. D., Sheeley, N. R., Jr., Tousey, R. and Van Hoosier, M. E., BAAS - 7, 354 (1975).

1697

1698

111-2

1699

1700

1701

i703

1705

1706

1707

1712

1716

1718

1726

1750

1751

1752

Flare Mechanisms Based on the Current Liiiiitation Concept", II

Spicer, D. S., BAAS - 7, 352 (1975). "Absolute Solar UV Intensities 1680 Rrueckner, G. E.., Bartoe, J. -D. F., and Van Hoosier, iK. E. ,

On the XUV Emissions in Solar Flares Observed with the ATM/

to 2 100 A", NIoe, 0. K. ,

l.L4.AS 7, 360 (1975). - II

NRL Spectroheliograph", Cheng, c. c. and Widing, K. G. , BAAS - 7, 3-56 (1975).

Observations from Skylab of the Density Dependent C 111 Multiplet at 1175 A in Active and Quiet Regions and Above the Limb", Nicolas, K. and Brueckner, G. E., BAAS - 7, 353 (1975). "The High-Energy Limb Event of January 17, 1974", Tousey, R., Bohlin, J. D., Moe, 0. K., Purcell, J. D. , and Sheeley, N. R. , Jr., BAAS 7, 348 (1975).

Interpreting XUV Spectroheliograms in Terms of Coronal Magnetic Field Structures", Sheeley, N. R. , Jr. , Bohlin, J. D. , Brueckner, G . E., Purcell, J. D., Schemer, V. E., and Tousey, R., BAAS 7, 346 (1975).

"Line ProBles of the F e XXIV Emission at 192 A and 255 ;L i n Solar Flares", BrueCkner, G. E. , Moe, 0. K., and Van Hoosier, M. E. , BAAS 7, 356 (1975).

II

L

II

-

-.. - The Superheating Instability as a Trigger for Solar Flares",

Tidman, D. A. , Spicer, D. S . , and Davis, J., BAAS 7, 352 (1975).

"The XUV Sun as Observed by ATM S082", Tousey, R. , AIAA Bulletin 11, 344 (1974).

"Classification of F lares and Flare-Like Events Observed by the ATM XUV Spectroheliograph S082A and Spectrograph SO 82B During the Skylab Missions", Schemer, V. E. and Tousey, R., ATAA Bulletin 11, 345 (1974).

I t

-

- Structure and Temperature of Solar F l a r e Plasma", Schemer,

V. E. and Sandlin, G. D. , BAPS - 20, 659 (1974).

"A Resistive Screw Instability Model of a Solar Flare", Spicer, D. S., BAAS 7, 397 (1975).

"A 'Time Dependent Study of Conductive Heat F l o w in a Flaring Arch", Kepple, P. C. and Spicer, D. S. , BAAS I 7, 397 (1975)

The Sun's Polar Caps as Coronal Holes; Their Sizes, Evolution, and Phenomenology During the Skylab Mission", Bohlin, J. D., Rubenstein, D. M. , and Sheeley, N. R. , Jr., BAAS - 7, 457 (1 975).

I I

-

I t

. 111-3

1753 I ' Energy &?lease and Thermal Structure i n Solar Flares" Cheng,

"X-Ray '!!:vent of August 13-15, 1973", Scherrer, 17. E., Sandlin, G.. D., Sheeley, N. R., Jr., and Tousey, R . , BAAS 7, 430 (1975).

"Skylab/RTM Observations of Transient Events Having the GRF X-Ray atid Microwave Character", Sheeley, N. R.. , Jr., Bohlin,. J. 3 3 . . Scher re r , V. E., and Tousey, R. , BAAS - 7, 429 (1975)..

"Measured Variation of the XUV Line W.idths and Intensit ies N e a r t h e Solar Limb", R/Ioe, 0. I<. and Nicolas, K. R., BAAS i 7, 460 (1975).

'lEvolutiori o€ XUV Plasmas i n Solar Flares", Widing, K. G. and Cheng, C. C., BAAS - 7, 4 2 4 (1975).

'I Spectroscopic Study of Plasmas Preceding and During. Solar Flares", Scherrer, V. E. andsandl in , G. D., BAPS ---. 1.0: 1325 (1975). .

I t Solar Flare Collision Excitation Rate Coefficients", Tousey, R. , Kepple, P. C., and Davis, J. BAAS - 7, 398 (1975).

Plasma Heating and Flare X-Rays", Davis, J., Kepple, I?., Strickland, D., and Brueckner, G., BAAS - 7, 398 (1975).

"€Iydrcldynami.cs of Electron Beam Deposition in Solar Fl.ares", Eloornberg, J C . , Kepple, P. C,. , Davis, J., Boris, J., Brueckner, G., BAAS I 7, 338 (1 975).

'1ResuZt:4 from the NRL XUV Experiment on Skylab", Tousey, R., 3'. Opt. SOC. Am. - 64, 523 (1974).

' C. C. and Widing., IC. C., BAAS 7, 424 (1975). - 1754

- 1756

1757

1758

1763

1768

I t . 1769

1770

177 1

Maximum Efficiency of Ruled Concave Diffraction Gratings in the I t 1772 Ultraviolet", Mikes, T. L., J. Opt. SOC. Am. - 64, 1371 (1974).

Time Dependent Ionization Equilibrium and Line Emission from I I 1776 Ionized Iron Under Flare.-Like Conditions", Kepple, P. and Davis, J., EOS - 56, 1183 (1974).

Trans ien t Line Emission from Ionized Iron Under F lare-Like .

Conditions", Davis, J . , Kepple, P., and Tousey, R . , BAAS - 7, 357 (1975).

"Absolute Calibrated Solar UV Intensities 1700 - 2100 A'', RIoe, 0. K. ,. J. Opt. SOC. - 64, 1375 (1974).

The Source of Material Comprising a M a s s Ejection Coronal Transient", Hildner, E. , Gosling, J. T., Hansen, R. T., and Bohlin, J. D., BAAS - 7, 473 (1 975).

178 1 "Evidence for Non-Hydrostatic Equilibrium Conditions in the .

Transi t ion Region", Brueckner, G. E., Stanford Univ. Inst . fo r Plasma Res. Report No. 594 (1974).

I t 1777

1778

VI 177.9

.

111-4

1782 I' Evidence for nqagnetic Field Line Reconnection in the Lower Corona", Sheeley, N. R., Jr., EOS Transactions, Vol. 56, 1049.

II 1794 'I Extreme Ultraviolet Spectroheliograph for Plasma Diagnostics, Scherrer, V. E., Purcell, J. D. and Sandlin, G. D. Frist Topical Conference on Diagnostics of High Temperature Plasmas, American Physical Society, 7-9 January 1976, Knoxville, Tennessee.

1796 "The Emission Line Spectrum Above the Limb of the Quiet Sun: 1175-1 940 Angstroms, 'I Doschek, G. A., Feldman, U., Van Hoosier, -M. E. and Bartoe, J. -D. F. Ast rophp. J. -. 206, 964 (1976).

1797 "The Emission Line Spectrum Above the Limb of a Solar. Coronal Hole: 1175-1 940 .Angstroms, I ' Feldman, U., Doschek, G. A., '

Van Hoosier, M. E. and Purcell, J. D. Astrophys. J. - 206, 965 (1976).

I' Diagnostics for Plasma Temperatures in the Spectrum 171 - 630A, 'I

Scherrer, Victor E. and Sandlin, G. .D., 1976 Spring Meeting of APS, 26-29 April 1976, Washington, D. C . , . BAPS - 21, 598 (1976).

"High Spatial Resolution UV Spectr-3- of the Sun: The Dynamics of the Transition Zone, Brueckner, G. E., Bartoe, J. -D. F., Kjeldseth Moe, O., Nicolas,' K. R. and Van Hoosier, M. E., XIX CCl.3 PAR Meeting, 8-1 9 ,Tune 1 976, Philadelphia, PA. '

. .

1825

1829 II

183 1 "Spectrophotometry of the. Photospheric and Chromospheric Granulation in the UV Region 1240-1650A, 'I Bartoe, J. -D.. F., Brueckner, G. E., Kjeldseth Moer O., Nicolas, K. R. and Van Hoosier, ' M. E., XIX COSPAR hqeeting, 8-19 June 1976, Philadelphia,' PA.

Field Line Reconnection, I' Spicer, D. S., Solar Physics Div. of 148th A.A.A.. Meeting, 21-24 June 1976, .Haverford, PA., BAAS - 8, 373 (1976).

"Final Report on Coronagraph Feasibility Studies for a n Out-of- Ecliptic Mission," Bohlin, J. D., Howard, R, A., Koomen, M. J., and Michels, D. J. Out-of-Ecliptic Mission, I ESA Headquarters, 6-7 April 1976, Paris., France.

"Multiple Loop Activations and Continuous Energy .Release in a .

Solar Flare, I' Widing, K. G., Solar Physics Div. of 148th A.A. S. Meeting, 21-24 June 1976, Haverford, PA., BAAS - 8, 375 (1 976).

. .

1836 "Amplitude Instability and Stochastic Behavior During Magnetic '

1839

'Phase A Final Review of a Joint ESA/NASA

1847

1853 "Identification of Ha Macrospicules with E W Macrospicules and with Flares in X-Ray Bright Points, If Moore, R. L., Tang, E'. , Bohlin, J. D. and Golub, L., Solar Physics Div. of 148th. A.A. S. Meeting, 21-24 June 1976, Haverford, PA., BAAS - 8, 333 (1976).

111-5

11 1854 "Observation of a Kink Instability in a Solar Flare, Solar Physics Div. of 148th A.A. S. Meet ing, 21 -24 June 39.76, BAAS 8, 373 (1976).

"Preliminary Analysis of NRL, Skylab Spectroheliograms in Lines of H e I and He 11, Linsky, J. , Solar Physics Div. of 148th A. A. S. Meeting, 2 1-24 June 1976, Haverford, PA., BAAS - 8, 332 (1976).

12474 August 7-9, 1973, Schemer, V., Brueckner, G., Sandlin, G. arid Tousey, R. , Solar Physics Div. of 148th A.A. S. Meeting, 21 -24 June 1776, Haverford, PA., BAAS 8, 373 (1976).

Time Dependent Ionization and Radiation of a Gas Moving through the Solar Transition Zone, I' Kjeldseth Moe, O., Solar Physics Div.

' of 148th A.A. S. Meeting, 21-24 June 1976, Haverford, PA., BAAS - 8, 331 (1976).

"Coronal Lines in ATM Sp.ectra 1100 - 3000 8, It Sandlin, G.. D. , Brueckner, G. E. and Tousey, R., Solar Physics Div.' of 148th A.A.S. Meeting, 21-24 June 1976, Haverford, PA.,'BAAS - 8, 339 (1 976).

Cheng, C. C i,

- 1 855

I I Mango, S., Bohlin, J. D., Glackin, D. and

Pre-flare Observations During the Evolutiion of McMath R.egion I I

II 1636

. - . . I I 1857

1858

Spectrophotometry of the Photospheric 3 n d Chromospheric Gran!.:lation i n the UV Region 1240-1650& Bartoe, J. -D. F., Brueckner, G. E., Kjeldseth Moe, O., Nicolas, K. R. and Van Hoosier, h!l. E. , Solar Physics Div. of 148th A.A. S. Meet- ing, 21-24 June 1976, Haverford, PA., EAAS - 8, 312 (1976).

"The UV Spectrum of a Sunspot (1175 t o 1700 A) Observed with High Spatial and Spectral Resolution, Nicolas, K. R. ; Bartoe, J. -D. F. and Van Hoosier, R'I. -E., Solar Physics Div. of 148th A; A. S. Meeting, 21 -24 June 1976, Haverford, PA., BAAS - 8, 345 (1976).

"Densities i n the Solar Chromosphere above the Quiet Sun and a Coronal Hole Derived f rom the Hydrogen Balmer Lines, F. D., Feldman, U. and Doschek, G. A,, Solar Physics Div. of 14Sth A.A. S. Meeting, 21-24 June 1976, Haverford, PA., BAAS - 8, 338 (1976).

"Preliminary Analysis of NRL Rock::t Spectra of the La Line Wings, Basri, G., Bartoe, J.-D. F., Brueckner, G., Linsky, J. and Van Hoosier, M. E., Solar Physics Div. of 148th A. A. S. Meeting, 21-21 June 1976, Haverford, PA., BAAS - 8, 331 (1976).

"The Presence of Si I Ser ies in the Ultraviolet Solar Spectrum: 3000A - 1200%L11, Moore, C. E., Brown, C . M., Sandlin, G. D., Tilford, S. G. and Tousey, R., Ap. J. - 212, 310 (1977).

I I 1859

1860 11 Brueckner, G. E.,

1861 II Rosenberg,

I I 1865

1868

111-6

1904

I909

1912

1926

1927

1528

1945

Chromospheric Limb Spectra f r o m Skylab: 2000 to 3200A1', Doschek, G. A., Peldman, U. and Cohen, L., Ap. J. 210, 890 (1976).

The Origin of Coronal Holes and a Hypothesis f o r Their Occurrence During the Solar Cycle", Rohlin, J. D. , Topical Conference on Solar and I'titerplanetary Physics, 12-1 5 January 1977, Tucson,' Arizona, to be published in Bull. of A. A. S.

"ATM Skylab Observations of Flare Lyman-a, Line Profiles", Canfield, R, C. and Van Hoosier, M. E. , Topical C'onf. on Solar and Interplanetary Physics, 12-15 J a n u a r y 1977, Tucson, Arizona, to be published in Bull. of A. A. S.

"Observations of Coronal Holes Throughout Sunspot Cycle ZO", Eroussard, R. M., Underwood, J. H., Tousey, R., and Sheeley, N. R., Jr..-, 149th A.A.S. Meeting, 16-19 Honolulu, Hawaii, BAAS - 8, 557 (1976).

"Enhancement of Dielectronic R.ecombination by Plasmas". Jacobs, V. L., Davis, J. andKepple, P. C., TopicalConf. onAtomic Processes in High Temperature Plasmas of Am. Physical SOC. , 16-18 February 1977, Knoxville, Tennessee, to be published in Bull. of A. P.S.

II

- II

"The Influence of Metastable Levels on the Oxygen Impurity Radiation

V. L. , Topical Cod. on Atomic Processes in High Temperature Plasmas of Am. Physical SOC. , 16-1 8 February 1977, Knoxville, Tennessee, t o be published in Bull. of A. P. S .

' f rom Flare-like Plasmas", . Rogerson, J. E. , Davis, J. and Jacobs,

Models of Solar Chromosphere Structures Implied by Lyman-cu Rocket

G. E. and Van Hoosier, M. E. , 149 A.A.S. Meeting, 16-19 January,. 1977, Honolulu, Hawaii, BAAS - 8, 534 (1976).

I t

, Spectra", Basri, G., Linsky, J. L. , Bartoe, J. -D. F., Brueckner,

111 -7

IV, P13OFESSIONAL TALKS - INVITED

1514

1515

1518

1522

-1565

1641

1642

1651

1652

1658

"%%e ATM Project", Tousey, R . ,' Symp. on 'Calibration Methods in - i h UV and X-Ray Regions of the Spectrum', Institut f u r extra- t e r r e s t r i s che Pkysik, Max Planck Institut f u r Physik utid Astrophysik, Munich, Germany, 27 -30 May 1968.

Assembly IAU, C :.)mmission 44, University of Sussex, Brighton, England, 20 August 1970.

Identifications in the Solar XUV Spectrum", Tousey, R. , 24th Gen. 1 1

Solar Astronomy, Som9 Highlights of the Past Year" , Tousey, R. ,. 14th Gen. Assembly IAU, IAU Commission 44, University of Sussex, Brighton, England, 20 August 1970.

Survey of New Solar Results", Tousey, R. , IAU Symp. 41, 'New

Solar Spectroscopy f rom Space Vehicles", Tousey, R. , Tenth

. 1 1

1 1

Techniques in Space Astronomy', Munich, Germany, 10-m August 1970.

National Meet ing of the Society for Applied Spectroscopy, St. Louis, Missouri, 18-22 October 1971. ,

"High Angular Observations from Roc.kets: Solar XUV Observations", Tousey, R. , COSPAR XU, Seattle, Washington, 17 June - 2 July 1971.

Madrid, Spa.in, 10-24 May 1972. .

Ibid. , AAS, Solar Phys. Div. , University of bl'aryland, College Park, TGT-ryland, 4-6 April 1972.

I 1

. .

The Coronal Origin of a Solar Flare", Brueckner, G. E. , COSPAR XV, 11

I

The Ext reme Ultraviolet Spectroheliograph and the Extreme Ultra- . violet T V Monitor", Tousey, R. , Bartoe, J. -D. F. , Brueckner, G. E., and Purcell, J. I). , SOC. Photo-Optical Instr . Eng. , 'Instrumentation in Astronomy' - 11'. Tucson, Arizona, 4-6 March 1974.

"The Extreme Ultraviolet Spectrograph", Bartoe, J. -D. F. , Brueckner, G . E., Purcell, J. D. , and Tousey, R., SOC. Photo- Optical Instr. Eng. , 'Instrumentation in Astronomy - II', Tucson, Arizona, 4-6 March 1974.

11

"The Sun as Observed by the ATM XUV Spectroheliograph and Spectrograph, S08ZA and B", Tousey, R. , COSPAR XVII, Sao Paulo, Brazil, 25 June - 1 July 1974.

"Preliminary Results from the NRLIATM Instruments from Skylab Z1', T O U S e y , R., Bartoe, J. -D. F. , Bohlin, 6. D., Brueckner, G . E., Purcell, J. D., Scherrer, V. E., SChUmaCher, Et. J. , Sheeley, N. R. , Jr. 8 and Van Hoosier, M. E., IAU Symp. 57, 'Coronal Disturbances', Surfers Paradise, Queensland, AustraTTa, 19 August - 11 September 1973.

"Preliminary Results from the Extreme Ultraviolet Spectrohelio- graph and Ultraviolet Spectrograph on ATIVI", Tousey, R. , AGU, 55th Annual Meeting, Wa:;hington, D. C. , 8-12 April 1974.

1v-1

I I Results from the NRL Experiments on Skylab",. Tousey, R . , Opt. SOC. Am., Washington, D. C., 22 April 1974.

Some NRL/ATM Observations of a Coronal Hole at the Solar Limb", Sheeley, N. R., Jr., 3rd Solar Wind Conf., Asilomar, California, 25-29 March 1974.

11 1662

1668

167 1

1675

1677

1679

. 1683

1685

1690

1691

1715

"Skylab Observations of the Sun (170-630 A) wi th the NRL Objective Grating Spectroheliograph", Widing, K. G. , Opt. Soc.. Ani. , Houston, Texas, 15-18 October 1974.

"Diffraction Gra t ings f o r the XUV - Conventional vs. Holographic" *

Hunter, W. R., Symp. on 'Diffraction Gratings and Grating Instru- ments', Tokyo, Japan, 31 August 1974.

Ultraviolet Emission Line Profiles of Flares and Active Regions", Brueckner, G. E., IAU/COSPAR Symp. 68, 'Solar Extreme UV, X and Radiation', Buenos Aires, Argexina, 11 -14 June 1974.

"Fe XXIV' Emission in Solar Flares Observed with the NRL/ATA3 XUV Slitless Spectrograph", Widing, K. G.. , IAU/COSPAR Symp. 68, 'Solar Extreme UV, X and Radiation', Buenos Aires, Argent inay 1 1 -14 June 1974.

I I

. . . . .

XUV Observations of Coronal Magnetic Fields", Sheeley, N. R . , Jr., 'I

Bohlin, J. D., Brueckner, G: E., Purcell, J. D., Schemer, V. E.; and Tousey, R., Conf. on IFlare-Related Magnetic Field Dynamics', Boulder, Colorado, 23 September 1974.

"Observations of the Hydrogen Ly-cu (1216 A) Emission Line of Comet Kohoutek (1 973f) by the Skylab/ATM S082B Spectrograph", . Keller, H. U. ,. IJohlin, .J. D., and Tousey, R . , Comet Kohoutek Workshop,. MSFC, Huntsville, Alabama, 13 - 14 June 1974.

"ATM Observations on the XUV 'Emission from Flares", .Brueckner, G. E., IAU Colloq. 27, 'Fourth Conf. on Ultraviolet and X-Ray Spectroscopy of Astrrphysical and Laboratory Plasmas', Harvard University, Cambridge, Massachusetts, 9- 11 'September 1974.

. . . .

- . . ....

Ibid., 'Solar Physics - Plasma Physics Workshop1, Stanford m v e r s i t y , Stanford, California, 17 -20 September 1974.

G. E., Royal Society Discussion Meeting 'The Physics of the Sol.ar Atmosphere', London, England, 14- 15 January 1975.

"Eruptive Prominences Recorded by tfie XUV Spectroheliograph on 'Skylab", Tousey, R. , Royal Society Discussion Meeting, 'The Physics of the Solar Atmosphere', London, England, 14-15 January 1975.

"XUV Results from Skylab", Tousey, R., International Conf. on 'X-Rays in Space', University of Calgary, Calgary, Alberta, Canada,

Ultraviolet Observations of Solar Flares from Skylab", Brueckner, I t

14-21 August 1974.

I v-.2

1733

1734

1748

1749

1760

1774

1778

1781

1784

1786

. "XUV Emission from Abovc! the West Limb Near 2O:OO U. T., Janriary 17, 1974", Tousey, R., TAU Colloq. 27, 'Fourth Conf. c:m i.lltraviolet and X-Ray Spectroscopy of Astrrphysical and Labora- t o ry Plasmas', Cambridge, Massachusetts, 9- 11 September 1974.

"A Review of Skylab/ATn/I Observations and Analyses of Coronal Transients", Gosling, J. T., Rohlin, J. D., Krieger, A. S., Schma.'tII., E. J., Tandberg-Hanssen, E., C.OSPAR XVIII, Varna, Bulgaria, 29 May - 7 June 1975.

The Interpretation of Ultraviolet Solar Spectra", Moore-Sitterly, C. E. Twentieth Liege International Astrophysical Symp., Liege, Belgium, 17-20 June 1975.

Sheeley, N. R., Jr., Bohlin, J. D., Brueckner, G. E., Purcell, J. D., Scherrer , V. E., Tousey, R., Smith, J. B., Jr., Speich, D. IvT., Tandberg-Hanssen, E., Wilson, R. ILL, de Loach, A. C . , Hoover, R. B.', and McGuire, J. P., Annual Meeting of HAO, SPO, KPNO, Santa Fe, New Mexico, 23 May 1975.

I I

Coronal Changes Associated With a Disappearing Filament", . I I

"Absolute Solat' Intensities 1750 8, - 2100 A and Their Variations with Solar Activity", Brueckner, G. E., Bartoe, J. -D. F., Moe, 0. I<. , Van Hoosier, M. E., Workshop on the Solar Con- stant and the Earth 's Atmosphere', Biz Bear Solar Observatory, Big Bear City, California, 19-21 May 1975.

"First Results f rom Skylab", Tousey, R., AAS, Tucson, Arizona, 2-6 December 1973.

"Absolute Calibrated Solar UV Intensities 3700 to 2100 A", R'loe, 0. K., Opt. SOC. Am., Houston, Texas, 15- 18 October 1974.

Evidence for Non-Hydrostatic Equilibrium Conditions in the Transit ion Region", Brueckner, G. E., 'Solar Physics - Plasma Physics Workshop', Stanford University, Stanford, California, 17-20 September 1974.

Spectroscopic Far Ultraviolet Observations of Active Regions Prior to and Dnring Flares", Brueckner, G. E., Patterson, N. P., Scher rer , V. E., 'Flare Build-up Study Workshop', Falmouth, Cape Cod, Massachusetts, 8- 11 September 1975.

Solar Research with Diffraction Gratings in the Far Ultraviolet", Brueckner, G. E., U. S. -Japan Seminar on Diffraction Gratings, . Washington, D. C., 14-17 October 1975;

"Photospheric Magnetic Field and I t s Coronal Extension", Sheeley, N. R . , Jr. , AAS, Solar Physics Div., 20 January 1975.

' I

I I

I '

IV-3

1838

1840

1841

1562

1863

1870

1878

1891

, . 189.5

1907

. ..

1915

11 kIechanisms for Particle Acceleration in Solar Flares, Spicer, I). S., Godd-, ::d Space Flight CenterlUniversity of Maryland High Energy Astrc?j4iysics Seminar, 15 March 1976.

Resistive Kixk Model of a Solar Flare, Spicer, D. S., Bartol Institute, Swarthmore, Pennsylvania, 17 February 1976. .

"The nlorphology and Evolution of Coronal I-Ioles, ' I Bohlin, J. D. . Coll. at Observatoire de Paris, Paris, France, 9 Apri l 1976.

Spectroscopic Ultraviolet Observations of F la re s from Skylab, I '

Brueckner, G. E., U. S. -Japan Cooperative Seminar on "High .

Energy Phenomena in Solar Flares,

I'Skylab Spectroheliograph Observations of the Double Ribbon Flare of 1973 June 15, 'I Widing, K. G., U. S. -Japan Cooperative Seminar on "High Energy Phenomena in Solar Flares, I' 10-13 May 1976, Tokyo, Japan.

I I

I 1 I 1

I 1

10-13 M a y 1976, Tokyo, Japan.

I 1 "The Physical Propert ies of Coronal Holes, Bohlin, J. D., AGU International Sym. on Solar-Terrestr ia l Physics. 7 -1 8 June 1976, Boulder, Colorado.

"The Therma l and Non-Thermal Flare: A Result of Non-Linear Threshold Phenomena, 25 August 1976, Grenohle, France.

Multiple Loop Activations"aiid Continuous Energy Release in a Solar Flare", Widing, K. G. . XVI General Assembl .~, I. A. U., 24 August - 2 September 1976, Grenoble, France.

I I Spicer, D. S. , I. A. U. Commission 8 14, .

I 1

Analyses of Laboratory Spectra of Special Interest for the Inter- pretation of Ultraviolet Stellar Spectra, 'I . Moore-Sitterly, C. and Widing, K., I. A. U. Commission hc 14, 25 August 1976, Grenoble,

"The Prime Energy Release and Subsequent Flare Development", Erueckner, G . E,, I, A, U. Commission # 10, 24 August - 'i. September 1976, Grenoble, France.

11

. France.

"High Spatial Resolution UV Spectroscopy of the Sun", Brueckner, G. E. , I. A.U. Commission #44, 24 August - 2 September 1976, Grenoble, France.

"Detecting Ultraviolet Radiation from and through the Atmosphere", Prinz, D. K., 20th Annual Technical Symposium of the Society of Photo-Optical Instrumentation Engineers, 26 August 1976, .

San Digeo, California.

"A Random Walk Through the Results of the Solar Experiments of the Skylab Mission", Bohlin, J. D., National Capital Section of Opt. SOC. of Am., 25 January 1977, Washington, D. C.

IV -4

1923 "The Phenomenon of 'Overlapping of Resonances' its Applied to. lK;gnetic Rcconnection Problems i n Space", Spicer, D. S. , N. C. Christophiles International Summer School and Conference on Laboratory and Space Plasmas, 20-30 July 1977, Spetses, Greece.

1925 "A Survey of Coronal Holes and. Their Solar Wind Associations Throughout Sunspot Cycle 20"s Sheeley, Ni R. , Jr. , Topical Conf. on Solar and Interplanetary Physics, 12-15 January 1977, Tucson, Arizona.

"An Arch ,Model of a Solar Flare", Spicer, D. S . , High Altitude Observatory., 3 March 1977, Boulder, Colorado.

1929

IV-5

V. PROFESSIONAL TALKS - CONTRIBUTED . .

1420

1469

147 1

1479

1481

1499

1509

1510

1529

1536

1538

1544

Some Recent XUV Spectroheliograms and Heliograms f rom Rockets, " II

Purcell, J . D., Bartoe, J. -D. F., Snider, C. B., and Tousey, R., Second International Conf. on 'Vacuum Ultraviolet and X-Ray Spec- troscopy of Laboratory: and Astrophysical Plasmas', University of Maryland, 24-28 March 1968.

Radiation Light Sources for Stellar Telescope Calibration f rom 700 8, to 7000 A, 'I Hunter, W. R., Workshop on Optical .Telescope Technology, MSFC, Huntsville, Alabama, May 1969.

Planned and Proposed, 'I Tousey, R., Opt. SOC. Am. Symp. on 'Optical Contamination in Space', Aspen, Colorado, 13-15 August 1969.

"A Photographic Spectrum of a Flare in the xuv, " Purcell, J. D. and Tousey, R., International Symp. on Solar Te r re s t r i a l Physics, Leningrad, U. S. S. R., 13 May 1970.

I f

. Some Experiments on the Corona Surrounding a Spacecraft - Past, 1 1

Observations of the Sun in the Ext reme Ultraviolet, 'I Tousey, R., Meeting of the Royal Society, London, England, 2 1-22 Apri l 1970. I'

0bse.rvation of Stark-Effect in a Far UV Flare Spectrum, I' Brueckner, G. E., 14th Gen. Assembly LAU, University of Sussex, Brighton, England, 18-27 August. 1970;

the Sun Between 1650-1800 A, " Brueckner; G. E., Moe, 0. K., Pitz, E., AAS, Solar Phys. Div., Huntsville, Alabama, 17 h'ovember 1970.

If

I' Absolute 1nten.sity of the Continuum i n the Ultraviolet Spectrum of .

"High Spectral and Spatial Resolution Ultraviolet Spectroscopy of the Sun in the Region 11 70 - 1800 A, I' Brueckner, G. E., U S , Solar Phys. Div., Huntsville, Alabama, 17 November 1970 . "On the Classification of Some Highly Ionized Iron and Nickel Lines in the 200-400 A Region of the Solar Spectrum, I' Widing, K. G., Sandlin, G. D., and Cowan, R. D.,ThirdSyrnp. on 'TJltraviolet and X-Ray Spectroscopy of Ast.rophysica1 and' Laboratory Plasmas', Utrecht, The Netherlands, 24-26 August 197 1.

"XUV Television of a Solar Image f r o m a Rocket, 'I Tousey, R., Symp. on 'The Processing of Telescopic. Images', Lava1 University, Quebec, Quebec, Canada, 1-2 October 197 1 .

.

Possibilities for Measuring Atmospheric Extinction and Absorp- 11

tion with the ATM Solar Experiments in Skylab, 'I Tousey, R., Informal Conf. on 'The U s e s of Astronomy in the Stcidy of A i r Pollution' Project, Seattle, Washington, 19 August 197 1.

"Extreme Ultraviolet Spectrohe1,iograms of a Solar Flare, Purcell, J. D. and Tousey, R., AAS, 136th meeting, San Juan, Puerto Rico, 6-8 December 197 1.

?I

v-1

1545

3 572

1606

1623

1624

' 1625

1626

1628

1629

1637

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1643

Prel iminary Results of Identifications in the XUV Spectrum of it . Solar Flare, Purcell, J . D., Tousey, R., and Widing, K. G., AAS, San Juan, Puerto R4c0, 6-8 December 1971.

I t

II

A .&calibration of Spectral Radiance of Mercury and Deuterium Arc Stantlard Lamps in the near UV, Bartoe, J. -D. E'. and Ott, W. R., Opt. SOC. Am., San Francisco, California, 17 -20 October 1972.

The Increase in Tra:.: -;mittance of Unbacked Aluininurn Filters Exposed to R F and DC Discharge in Oxygen, Steele, G. N., and Gillette, R. B., Opt. SOC. Am., Rochester, New York, 9-12 October 1973.

"The. 1175 to 1900 A Ultraviolet Spectrum of Solar Flares, I' Brueckner, G. E., Bohlin, 5. D., Moe, C. IC., Nicolas, K. R., Purcell, J. D., Scherrer , V. E. , Sheeleyv, N. R., Jr., and Tousey, R., AAS, Solar Phys. Div., Honolulu, Hawaii, 9- 11 January 1974.

1'131.c?ctron Density from Line Ratios in the XUV Spectrum of a Solar Flare, Widing, K. G., Purcell, J. D., and Tousey, R., AAS, Solar Phys. Div., Honolulu, Hawaii, 9- 11 January 1974.

I I

l l

I 1

I t Hunter, W. R. ,

? I

I I "The Screw Pinch and the Solar Flare, Spicer, D. S. and CIieng, C. C., AAS, Solar Phys. Div., 9-1 1 January 1974.

"A Prel iminary Studj of Coronal Structures by Means of Time- Lapse Photography, Sheeley, N. R., Jr., Bohlin, J. D., Brueckner, G. E., Purcell, J. D., Scherrer, V. E., and Tousey, R., AAS, Solar Phys. Div., 9- 11 January 1974.

"Rocket S pectroheliograrn Observations of the Heights of Forma - tion and Sizes of Bright Features in the Transition Zone, Simon, G. W., Seagraves, P. H., and Tousey, R., AAS, Solar Phys. 3>iv., Honolulu, Hawaii, 9 - 1 1 January 1974.

-

I I

Cinematographic Observations for AT31 and their Comparison 11

11 with some ATM Results, Zirin, H., Holt, J., Brueckner, G. E., Bohlin, J. D., Purcell, J. D., Scherrer, V. E., Sheeley, N. R., Jr., .

and Tousey, R., AAS, Solar Phys. Div., H.onolulu, Hawaii, 9- 11 January 1974.

"Studies of Atmospheric Extinction from Skylab, Tousey, R., Tilford, S. G., and Prinz, D. K., AGU, 55th Annual Meeting, Washington, D. C., 8- 12 April 1974.

Coronal Extreme Ultraviolet Spectroheliograph and Chromospheric Ext reme Ultraviolet Spectrograph, 'I Tousey, R., AAS, Solar Phys. Div. , Honolulu, Hawaii, 9-3 1 January 1974.

"Oxygen Densities a t Altitudes. Between 70 and 129 kin, 'I Brueckner, G. E., Bartoe, J. -Do F. , Brown, C. M., Prinz, D. K., Tilford, $3. G., and Van Hoosier, M. E., COSPARXVII, Sao Paulo, Brazil, 25 June - 1 July 1974.

I I Brown, C. M.,

I ?

V-2

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. .

1655

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1657

1666

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1678

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Ultraviolet Emission Line Profiles of Flares and Flare-Like I 1

I I Events Observed from Skylab, , Bruecliner, G . E. , hloe, 0. K. , and Nicolas, I<. R. , COSPAR XVII,, Sao Paulo, Brazil, 25 June 1 July 1974.

I I . . On the F e XXW Emission in the Solar F la re of June 15, 1973, I I

Widitig, K. G. and Cheng, C. C., COSPAR XVII, Sao Paulo, Brazil, 25 June - 1 July 1974.

"Structure of the Sun's Polar Cap i n the Wavelengths 240-600 A, Bohlin, J. D., Sheeley, N. R., Jr., and Tousey, R.., COSPAR. XVII, Sao Paulo, Brazil, 25 June - 1 July 1974.

I I

Implications of NRL/ATR/I Solar F la re Observations on Flare I 1

I I Theories, Cheng, C. C. and Spicer, D. S., IAU/COSPAR Symp. 68, 'Solar Extreme UV, X and y Radiation', Buenos Aires, Argentina, 11-14 June 1974.

"Skylab Observation of the White Light Corona and the He I1 304 Chromosphere During the Eruptive Prominence Event of August 21, 1973, Bohlin, J. D. , Brueckner, G. E. , Purcell, J. D., Scherrer, V. E., Sheeley, N. R., Jr., Tousey, R., and Poland, A. I. , AGU, 55th Annual Meeting, Washington, D. C. , 8-12 April 1974.

in the White Light Corona and i n the He I1 304 .& Chromosphere, Poland, A. I . , Bohlin, J. D. , Brueckner, G. E, , Purcell, J. D. , Scherrer, V. E., Sheeley, N. R., Jr., and Tousey, R., AAS, Lincoln, Nebraska, 26-29 March 1974.

Some Reflections on the U s e of Conventional and Holographic Diffraction Gratings in the Vacuum Ultraviolet Spectral Region, Hunter, W; 11. , IV Internatiorial Conf. on Vacuum-Ult.raviolet Radiation Physics, Hamburg, Germany, 22-26 July 1974.

G. E., IAU/COSPAR Symp. 68, 'Solar Extreme UV, X and y Radiation', Buenos Aires, Argentina, 11 - 14 June 1974.

"Flares Observed by the NRL/ATR/I Spectrograph and Spectro- heliograph During the Skylab Missions, Scherrer, V. E. and Tousey, R. , International Conf. on .IX-Rays in Space', University of Calgary, Calgary, Alberta, Canada, 14-21 August 1974.

11

The Eruptive Prominence of August 21, 1973, Observed from Skylab I I

II

' 1

I I

I I Flare-Like Ultraviolet Spectra of Active Regions, Brueckner, 11

I 1

"The Impact of ATM/NRL Flare Data on Flare Theory, ' I Spicer, D. S., Cheng, C. C., Widing, K. G., and Tousey, R., Second European Conf. on Cosmic Plasma Physics, Culham, England, 1 July 1974.

''Diffraction Gratings in Space Research - Problems and Accom- plishments, I ' Hunter, W. R., Informal meeting on Diffraction 'Gratings, Kyoto, Japan, 6 September 1974.

v-3

1684

1683

1696

1697

1698

1699

1700

1701

1703

1705

1706

!:[igli R.esolu tioii Ly-cr Observations of Comet Kohoutelc by Skylab and Coperniciis, Bohl.in, J. D., Drake, J. F., Jenkins, E. B., . and Keller, '9. U., 'IAU Colloq. ?.5, Goddard Space Flight Center, Greenbelt, ldaryland, 28 Octobe.i.:'-r 1 November 1974.

I 1

I I

Ultraviolet Solar Identifications Based. on Extended Absorption I I

I I S e r i e s Observed i n the Laboratory Spectra of Si I, To.!sey, R., Sandlin, G. D., Brown, C. M., G i n t e r , M. L., and Ti':.;'x-d, S. G. , IAU Colloq. 27, 'Fourth Conf. on Ultraviolet and X-i izty Spectroscopy of Rstrc)*ysic.al and Laboratory Plasmas', EIarvard University, Cambridge, Massachusetts, 9 - 1 1 September 1974.

Moore, C. E.,

A Catalog and Classification of Flares and Flare-Like Events Observed by the ATM XUV Spectrograph S082A and Spectro- heliograph S082B, Scherrer, V. E., T.ousey, R., and Sandlin, G. D., AAS, Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

I 1

I I

l l Polar Plumes in XUV Emission-Line Corona, Bohlin, J. D., I t

Purcell, J. D., Sheeley, N. R., Jr., and Tousey, R. , AAS, Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

I I Macro-Spicules in He I1 304 A Over the Sun's Polar Cap, I' Bohlin, J. D., Vogel, S. N., Purcell, J. D., Sheeley, N. R., Jr., Tousey, R., and Van Hoosier, 14. E., AAS, Solar Phys. Div., Boulder, Colorado, 20 -22 January 1975.

I I Flare Mechanisms Based on the Current Limitation Concept, I I

Spicer, D. S., U S , Solar Phys. Div., Boulder, Colorado, -20-22 January 1975.

"Absolute Solar UV Intensities 1680 A to 2100 A, Bruecltner, G. E., Bartoe, J. -D. F., and Van Hoosier, M. E., U S , Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

"On the XUV Emissions in Solar Flares Observed with the ATM/NRL Spectroheliograph, I' Cheng, C. C. and Widing, I<. G., U S , Solar Phys . Div., Boulder, Colorado, 20 -22 January 197 5 . "Observationos from Skylab of the Density Dependent C 111 n W t i - II plet at 1175 A in Active and Quiet Regions and Above the Limb, Nicolas, K. and Brueckner, G. E., AAS, Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

The High-Energy Limb Event of January 17, 1974, " Tousey, R., Bohlin, J. D., Moe, 0. K., Purcell, J. D., and Sheeley, N. R., Jr., U S , Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

Moe, 0. K.,

I 1

"Interpreting XUV Spectroheliograms in Terms of Coronal Mag- netic Field Structures, Sheeley, N. R., Jr., 'Bohlin, J. D., Brueckner, G. E., Purcell, J. D., Scherrer, V. E., and Tousey, R. , AAS, Solar Phys. Div., Boulder, Colorado, 20-22 Jatiuary . 1975.

I I

v-4

1707

17 12

17 14

17 16

17 18

1726

. 1731

1738

1739

1750

Line Profiles of the Fe XXIV Emission at 192 a and 255 A in II

I I Solar Flares , Brueckner, G. E., Moe, 0. IC. , and Van Hoosier, M. E., AAS, Solar Phys. Div., Boulder; Colorado, 20-22 January 1975. I' The S L I ~ ~ T Heating Instability as a Trigger for Solar Flares, I' Tidman, D. A . , Spicer, D. S. ' , and Davis, J., AAS, Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

"Forbidden Lines of Highly Ionized Iron in Solar Flare Spectra, 'I Doschek, G. A., Sandlin, G. D., Brueckner, G. E., Van Hoosier,." .&'I. E., and Tousey, R., IAU Colloq. 2'7, 'Fourth Conf. on Ultra- - violet 2nd X-Ray Spectroscopy of A s t r m y s i c a l and Laboratory Plasma', Harvard University, cambridge, Massachusetts, 9- 11 September 1974.

"The XUV Sun as Observed by ATIvI S082, I' Tousey, R., 'AIAA/AGU Space Science Conf. on 'Scientific Experiments of Project Skylab!, MSFC, Huntsville, Alabama, 30 October- 1 November 1974.

"Classification of F l a r e s and Flare-Like Events 0bserved.by the .

ATM XUV Spectroheliograph SO 82A and Spectrograph SO 82B During the Skylab Missions, Schemer, V. E. and Tousey, R., AIAA/AGU Space Science Conf. on 'Scientific Experiments of .Project Skylab', MSFC, Huntsville, Alabama, 30 October - 1 November 1974. .

II

. .- Structure and Temperature of Solar F l a re Plasma, " Scherrer,

V. E. and Sandlin, G. D., Am. Phys, SOC., Washington, D. C., 28 April - 1 May 1975.

11

The Character and Temperature of a Coronal'Transient: I. The 11

I' Event of 25-27 August 1973, Hansen, R.. T., COSPAR XVIII, Varna, Bulgaria, 29 May - 7 June 1975.

Bohlin, J. D., Hildner, E., and

I1 "Experience with Schumann Type UV Film on Skylab, M. E., Bartoe, J.-D. F., Brueckner, G. E., Moe, 0. K., Nicolas, K. R., and Tousey, R., Topical' Meeting on 'Imaging in Astronomy', Harvard University, Cambridge, Massachusetts, 18-20 June 1975.

Van Hoosier,

Limitations of Imaging Capabilities of Schumann Type UV Film, I' I'

Bartoe, J.-D., Brueckner, G. E., andVanHoosier, M. E., Topical Meeting on 'Imaging in Astronomy', Harvard University, Cambridge, Massachusetts, 18-20 June 1975.

"A Resistive Screw Instability Model df a Solar Flare, D. S., AAS, San Diego, California, 17-20 August 1975.

I? Spicer,

v-5

1752

1.7 53

1754

1756

17 57

1758

1768

1769

1770

1771

1772

1776

1777

T h e Sunts Polar Caps as Coronal Holes; Their Sizes, Evolution, I t

and Phenomenology During the Skylab Mission, I ' Bohlin, J. D., Rubenstein, D. FA., and Sheeley, N. E., Jr., U S , San Diego, California, 17 -20 August 1975.

r i "Energy R.elease and Thermal Structure in 'Solar Flares, Cheng, C. C. and Widing, K. G., AAS, San Diego, California,

"X-Itay Event of August 13-15, 1973, Schemer, V. E., Sandlin, G. D., Sheeley, N. R., Jr., and Tousey, R., AAS, San Diego, California, 17 -20 August 1975.

"Skylab/ATM Observatins of Transient Events Having the GRF X-Ray and Microwave Character, 3. U., Schemer, V. E., and Tousey, R., AAS, San Diego, California, 17 -20 August 1975.

"Measured Variation of the XUV Line Widths and Intensities N e a r the Solar Limb, Moe, 0. K. and Nicolas, K. R., AAS, San Diego, ,

California, 17 -20 August 197 5.

17-20 August 1975.

I 1

I t Sheeley, N. R., Jr., Bohlin,

t I

I t Evolution of XUV Plasmas in Solar Flares, Widing, IC. G. 1111

a!id Cheng, C. C., AAS, San Diego,: California, 17-20 August 1975.

Kepple, P. C., and Davis, J., AAS, San Diego, California, I I Solar Flare Collisional Excitation Rate Coefficients, Tousey, R., I 1

17-20 August 1975. I t Plasma Heating and Flare X-Rays, Davis, J., Kepple, P., I t

Strickland, D., and Brueckner, G., AAS, San Diego, California, 17 -20 August 197 5.

I I Hydrodynamics of Electron Beam Deposition in Solar Flares, I1

Bloomberg, H., Kepple, P. C., Davis, J., Boris, J. and Brueckner, G., U S , San Diego, California, 17-20 August 1975.

Resul t s from t h e NRL XUV Experiments on Skylab, It Tousey, R.,

Maximum Efficiency of Ruled Concave Diffraction Gratings in the

I I

Opt. SOC. Am., Washington, D. C., 21-25 Apri l 1974.

Ultraviolet, 15- 18 October 1974.

I t

I t Mikes, T. L., Opt. SOC. Am., Houston, Texas,

Time Dependent Ionization Equilibrium and Line Emission from I t

I t Ionized I ron Under Flare-Like Conditions, Kepple, P. and Davis, J., AGU, San Francisco, California, December 1974.

Trans ien t Line Emission from Ionized Iron Under Flare-Like I I

I1 Conditions, Davis, J., Kepple,' P., and Tousey, Re, AAS, Solar Phys. Div., Boulder, Colorado, 20-22 January 1975.

VI. COLLOQUIA

'1465

1635

' 1661

1708

1728

1737

1767

Apollo Telescope Mount Project", Winter, T. C. , , National. Eureau of Standards, Washington, D. C., 27 February 1969.

The Sun in Lyman-Alpha", Prinz, D. K., Nat ional Capitol Section of the Amateur Astronomers of America', 2 February 1974.

"NR.L/ATM Observations with the XUV Spectroheliograph", Sheeley, N. R., Jr., Sacramento Peak Observatory, Sunspot, New Mexico, 15 March 1974.

II

II

"Observations of the Sun in XUV with ATM", Tousey, R., Goddard Space Flight Center, Greenbelt, Maryland, 6 December 1974.

"Observations of the Sun in XUV with ATM", Tousey, R., University of Michigan, Ann Arbor, Michigan, 12 February 1975.

"Preliminary Resul t s from the NRL XUV Spectroheliograph and Spectrograph", Bohlin, J. D. , University of Maryland,. College Park, Maryland, 26 February 1975.

"Behavior of Coronal Magnetic Fields as Deduced from Skylab Obswvations", Sheeley, .N. R;' , Jr. High Altitude. Observatory, Boulder, Colorado, 14 March 1975.

Macrospicules, Polar Plumes, Coronal Holes, and Other Assorted Phenomena of. the Sun's Polar Cap", Bohlin, J. D., National Capital Astronomers, Washington, D. C. , 6 September 1975..

"The Structure and Development of Coronal Magnetic Fields as Deduced from Skylab Observations", Sheeley, N. R., Jr., Los Alamos Scientific Laboratory, Los Alamos,.' New Mexico, 2 1 F.Tarch 1 975.

I t

V I - 1

VII. OTHER PUBLICATIONS

1438

. .

1455

1469

' 1476

1500

. _

1504

1764

182.3

1690

1896

1903

Effects of High-Energy Protons on Photographic Film", Winter,

DOD Solar Experiments in NASA Prototype Space Station",

I I

T. C., Jr. and Brueckner, G. E. 1969, NRL ReportNo. 6797. I 1 .

Winter, T. C., Jr. 1970, Military Review, February, p. 58.

. "Radiation Light Sources for Stellar Telescope Calibration f rom 700 A to 7000 A", Hunter, W.R. 1969, ISRL Progress Report, .. September, p. 1. . "Spectroscopy i n the Space Science Division of the Naval Research Laboratory", Hunter, W. R. and Winter, T. C., Jr. 1969, ONR ILeviews.

"Schumann-Type Photographic Film: Preliminary Environment Test Results", Winter, T. C. and Van Hoosier, M. E. 1970, Rep.ort of NRL Progress, May.

Results", Winter, T. C. and V:.Ii Hoosier, M. E. 1970, NRL Report No. 7072.

"The NRL Solar Experiments i n the Apollo Telescope Mount of. Skylab", Tousey, R.. 1975, Report of NRL Progress, April, p. 1.

Electron Impact Excitation Rate Coefficients f o r Ions of Solar Interest", Kepple, P. C., Davis, .J. and Blaha, M. 1'975, NRL Memorandum Report 3171, Nov.

"A Spectral Atlas of the Sun Between 1175w and ZlOOA, 'I Kjeldseth Moe, O., Van Hoosier, M. E., Bartoe, J. -D. F. and Brueckner, G. E. 1976, NRLRepor tNo. 8057.

Schumann-Type Photographic Film: Preliminary Environment Test I I

I I

' . . . . .

"Holes in the Corona", Bohlin, J. D. 1976, Natural History 85,

"An Unstable Arch Model of a Solar Flare", ,Spicer, D. S. 1976, NRL Report No. 8036.

- pp. 69-70.

"NRL/ATM User 's Guide t o Experiment S082A", Packer, I. G. Patterson, N. P. , Mango, S. A. and Tousey, R. NRL Memorandum. Report No'. 3410, Nov. 1976.

"Flare Atlas. and U s e r ' s Instruction Guide for NRL.Flare Data of 15'June; 5 and 7 September 1973", Scherrer, V. E. and Sandlin, G. D., NRL Instruction Book No. 161, 'May-1 976.

'

. .

VI1 - 1

1711. OTI-IER PUBLICATIONS

1438

. .

1455

1469

1476

1500

. -

'1504

,1764

1823

1890

1896

1903

Effects of High-Energy Protons on Photographic Film", Winter, II

T. C., Jr. and Brueckner, G. E. 1963,. N R L ReporkNo; 6797. ' "DOD Solar Experiments in NASA Prototype Space Station",

Wi.nt:?.r, T. C . , Jr. 1970, Military Review, February, p. 58. .

700 A t o 7000 A'', Hunter, 151. It. 1969, NRL Progr.ess:Beport, .

",3pectroscopy in' the Space Science Division of the Naval Research : Laboratory!', Hunter, W. R. and Winter, T. C., Jr. 1969, ONR fleviews.

Radiation Lig4;lt Sources €or Stellar Telescope Calibration from . I I

September, p. 1. - c

"Schumann-Type Photographic Film:. Preliminary Environment Test Results", Winter, T. C. and Van Hoosier,, M. E,' 1970, Report of NRL Progress, May.

I I Schumann-Type Photographic Film: Preliminary Environment Tes t Results", Winter, T. C. and T7an Hoosier, hL E. 1970, NRL' Report No. 7072.

'"'J?ie NRL Solar Exp,eriments in the Apollo Telescope Mount of Skylah", Tousey, R: 1975, Report of NRL Progress, April, p. 1..

E:lectron Impact Excitation Rate Coefficients for Ions of Solar . II

Interest", Kepple, P. C., Davis, -J. and Blaha, M. 1975, NRL Memorandum Report 3171, Nov.

"A Spectral Atlas of the Sun Between 11758 and 2100A, I' Kjeldseth Moe, O., Van Hoosier, M. E., Bartoe, J. -D. F, and Brueckner, G. E. 1976, NRL Report No. 8057.

8 .

I-Ioles in the Corona", BOhh , J. D. 1976, Natural History 85,. II - pp. 69-70..

"An Unstable Arch R!todel of a Solar Flare", Spicer, D. S. 1976, NRL Report No. 8036.

"MRL/ATM User 's Guide to Experiment SO82A", Packer, I. G. Patterson, N. P., Mango, S. A. and Tousey, R. NRL Memorandum Keport No; 3410, Nov. 1976.

"Flare Atlas. and User's. Instruction 'Guide for NRL. Flare Data of 15'June; 5 and 7 September 197-3", Scherrer, V. E. and Sancllin, G. D., NRL Instruction Book No. 161, .May 1976.

VI1 - 1

Appendix E. L i n e L i s t s f o r S082B Data

The f o l l o w i n g t a b l e s have been e x t r a c t e d from t h e r e f e r e n c e s g i v e n . A d d i t i o n a l d a t a c o n c e r n i n g t h e measurements or t h e o r e t i c a l t e c h n i q u e s i n v o l v e d may be o b t a i n e d from t h e p u b l i s h e d p a p e r s . R e f e r e n c e s t o s t u d i e s of specif ic i o n s or solar phenomena may be found i n t h e B i b l i o g r a p h y , Appendix D.

E . 1 . 1 (DFVB)

"The Emiss ion L i n e Spectrum Above t h e Limb of t h e Q u i e t Sun: 1175-1940 Angstroms," G. A. Doschek, U. Feldman, M. E. VanHoosier"' and J.-D. F. B a r t o e . A p . J. Supp. Ser ies 31, p. 417 (1976.). . --

TABLE 2 < D F v R ) STRONG SOLAR LINES 4 A R C SECONDS ABOVE THE LIMB

Ion h (A) (Lab) h (A) (Solar) ht .*

c 111 ............ c 111 ............ c 111 ............ c I l l ............ c 111 ............ c 111 ............ s 111 ............ s 111 ............ s Ill ............ Fe 11 ............ s I l l ............ s 111 ............ Si 111 ............ La ............. o v ............ N v ............ Nv ............ c 111 ............ s 11 ............. s 11 ............. c1 ............. SI1 ..... i ....... Si 11 ............ Si II ............ Si II ............ c1 ............. CI ............. Si 111 ............ Si 111 ............ Si 111 ............

Si 111 ............. 0 1 ............. Si 111 ............ Si 11 ............. 0 1 ............. Si 11 ............ 0 1 ............. Si II ............ C I ............. Si 111 ............ Ni 11 ............ c 11 ............ CI ............. C I ............. C l ............. C.11. ........... Ni 11 ............ c I1 ............ P 111 ............

. O r ............. CI ............. 0 1 ............. Fe 11 ............ Fe 11 ............ Fe 11 ............ Ni 11 ............ o v ............ Fe 11 ............ Ni 11 ............ Fe 11 ............ Fe 11 ............ Ni 11 ............ Si iv ............ 0 1 v ............ 0 I V ............ 0 IV ............ Si iv ............

1 174.933 1175.263 1175.590 1175.711 1175.987 1176.370 1190.17

1194.02 1194.40 1.194.66

1200.97 1201.71 .

1206.51 0 1215.67 121 8.406 1238.821 1242.804 1247.383 1250.50 1253.79 1256.498 1259.53 1260.421 1264.737 1265.001 1274.984 1288.422 1294.543 1296.726

Et:%} 1301.146 1302.169 1303.320 1304.372 1304.S57 1305.590 1306.029 1309.277 1311.363 131 2.590 1317.220 1323.93 1328.833 1329.10 1329.59 1334.532 1335.203 1335.707 1344.34 1355.598 1355.844 1358.512 1360.1 8 1361.372 1368.098 1370.136 1371.292 1379.60 1381.295 1387.22 1392.82 1393.330 1393.755 1397.20 1399.774 1401 . 156 1402.770

1174.94 1175.27 1175.64 1175.73 1175.99 1176.37 1 190.20t 1190.49 1194.07t 1194.39 1194.63** 1199.17 1200.97 1201.73 1204.31# 120632 121 5.64 '1218.350 1238.82 1242.81 1247.38 1250.58t 1253.81 1256.47 1259.52 1260.41 1264.74 1265.08 1274.98 1288.42 1294.55 1296.73 1298.94 1300.90 1301.15 1302.17 1303.32 1304.37 1304.86 1305.58 1306.03 1309.29 1311.35 1312.58 1317.21 1323.92 1328.81 1329.14 1329.55 1334.53 1335.21 1335.71 1344.3211 1355.58 1355.83 1358.49 1360.16** 1361.36 1368.07 1370.12 1371.29 1379.60** 1381.28 1387.20 1392.80 1393.33 1393.76 1397.20 1399.77 1401.16 1402.78

1.1 0.90

B2.0 B2.0 B0.83 0.95 0.088 0.046 0.12 0.063 0.063 0.28 0.43 0.056 0.17

2.9 3.6 2.0 0.14 0.18 0.35 0.034 0.43 0.13 0.33 B0.16 0.041 0.041 0.40 0.28 1.2 0.046 0.11 1.24 0.35 0.24 1.3 0.063 1.3 0.27 0.046 0.16 0.25 B0.25 0.038 B0.035 B0.048 4.0 BO . 16 5.0 0.051 0.78 0.069 0.18 0.12 0.15 0.075 0.21 0.70 0.059 0.1 1 0.046 0.094

2.5 . 42

B 15.6 0.24 0.68 4.6 10.8

Ion h (A) (Lab) h (A) (Solar) 1nt.l

S l V ............ O l V ............ S I V ............ 0 IV ............ Ni 11 ............ Fe 11 ............ S I V ............ Fe II ............ Fe 11 ............ Fe 11 ............ Si 111 ............ Ni 11 ............ C I ............. CI ............. Ni 11 ............ Cr ............. Ni 11 ............ S I ............. SI ............. C I ............. N IV ............ N I ............. Ni 11 ............ Ni 11 ............ Ni 11 ............ Si II ............ Si 11 ............ Ni 11 ............ P I1 ............. c IV ............ Fe 11 ............ c I V ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ c1 ............. C I ............. C I ............. Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Feii ........... r Fe 11 ............ Fe 11 ............ Fe II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............

1406.00 1407.386 141 1.071 1412.834 1416.94

1424.716 1434.994 1442.746 1447.196 1454.852 1459.032 1463.336 1467.265 1467.402 1467.762 1472.972 1473.995 1481.763 1486.496 1492.625 1500.437

1502.150 1510.859 1526.708 1533.432 1536.746 1542.29 1548.1 85 1550.260. 1550.774 1551.933 1558.690 1559.084 1560.309 1560.69 1561.438 1563.788 1565.374 1566.819 1568.016 1569.674 1570.242 1573.825 1574.03 1574.768 1574.923

1577.1 66 1578.497 1580.625 1584.949

1588.286 1600.02 1602.51 1605.3 18 1608.456 161 0.921 1611.21 1612.802 1616.65 16 18.470 1621.24 1621.685 1621.85 1623.091 1623.71 5 1625.520

1401.79 1406.04t 1407.38 141 1.05 1412.83 1416.92 1423.86 1424.71 1434.98 1442.75 M47.23 1454.84 1459.03 1463.34 1467.27 1467.40 1467.75 1472.96 1473.99 1481.76 1486.51 '

1492.63 1500.44 1501.81 1502.15 151 0.86 1526.71 1533.44 1536.74 1542.3111 1548.19 1550.29 1550.79 1551.93 1558.62 1559.09 1560.30 1560.69 1561.42 1563.79 1565.35 1566.82 1568.02 1569.67 1570.24 1573.83 1574.02**. 1574.78 1574.91 1576.65 1577.16 1578.49. 1580.62 1584.95 ' 1586.53 1588.29 1600.01 1602.51 ** 1605.32 1608.46 1610.92 1611.19 1612.81 1616.65 1618.47 1621.25- 1621.69 1621.83** 1623.09 1623.71 1625.52

1.8 0.73 0.66 0.14 0.14 0.36 0.088 0.13 0.10 0.051 0.056 '

0.20 0.036 0.11 0.094 0.075 0.11 0.069 0.059 0.10 1.54 0.069 0.16 0.094 0.094 . 0.11 0.58 0.58 0.081 0.056 21.6 B

14.1 0.088

b0.40 1.3 0.34 B0.35 0.39 1.2 0.088 '

0.81 0.31 0.61 0.88 0.35 0.23 B 1.1 0.15 0.28 0.088 0.77 0.81 . 0.088 0.58 0.088

0.063 0.39 0.61 '

0.28 1.0 0.069 0.28 0.081 0.21 B 0.49 0.094 1.12

0.19,

434

Ion A (A) (Lab) A (A) (Solar) Int.*

Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe II ............ Fe I I ............ Fe 11 ............ Fe II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ He 11 ........... Fe 11 ............ Fe 11 ............ c 111 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ c1 ............. C I ............. CI ............. C I ............. Cr ............. CI ............. Fe II ............ Fe 11 ............ 0 111 ............ Fe 11 ............ Fe 11 ............ 0 111 ............ Fe II ............ Fe 11 ............ AI II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............. Fe II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe II ............ Fe II ............ Fe 11 ............ Fe II ............ Fe 11 ............ Fe I I ............ Ni I I i ? .......... Fe 11 ............ Fe 11 ............ Fe 11 ............ Fc I I ............ Fe 11 ............ Fe II ............ Fe II ............ Ni 11 ............ Fc I I ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Ni 11 ............ Fe 11 ............ Fe 11 ............

1625.909 1627.401 1629.154 1629.376 163 1.1 20 1632.668 1633.908 1634.345 1635.398 1636.321 1637.397 1639.403 1640.150 1640.4 1641.759 1643.576 1645.03 1649.423 1654.26 1654.476 1656.267 1656.928 1657.008) 1657.380 1657.907 1658.122 1658.771 1659.483 1660.803 1661.347 1663.221 1666.1 53 1669.68 1670.742 1670.787 1671.010 1673.462 1674.254 1674.716 1676.853 1679.381 1681 . 12 1685.954 1686.455 1686.692 1688.401 1689.828 1690.759 1691.271

1693.936 1694.68 1696.794 1698.190 1699.1 90 1702.043 1703.408 1704.652 1706.142 1707.399 1707.66 1708.250 1708.621 1709.598 1712.997 17 1 5.503

}

:E:; a)

1625.90 1627.37 1 629.1 6 1629.36 1631.12 1632.66 1633.90 1634.34 1635.39 1636.34 1637.40 1639.40 1640.14 1640.39# 1641.77 1643.58 1645.01 1649.42 1654.26** 1654.47 1656.27 1656.99 1657.39 1657.92 1658.13 1658.77 1659.48 1660.81 1661.32 1663.22 1666.15 1669.66**

1670.80

1673.46 1674.25 1674.71 1676.85 1679.39 ' 1681.10 1685.95 1686.45 1686.68 1688.39 1689.83 1690.77 1691.27 1692.52 1693.93 1694.67** 1696.78 1698.1 3 1699.19 1702.04 1703.41 1704.63 1706.14 1707.40 1707.66** 1708.25 1708.62 1709.59 17 13.00 1715.50

0.081 0.16 0.18

B0.075 . 0.15

0.32 0.82 0.094 0.10 0.12 1 . 0 0.10 0.8 4.8 0.059 0.79 0.088 0.49 0.19 0.39 0.44 0.43 0.42

B0.41 0.43 0.81 1.5 1.2 0.091 0.76 2.94 0.18

1.24

0.31 0.44 0.37 0.30 0.28 0.41 0.40 0.40 0.47 0.17 0.073 0.069 0.47 0.059 0.16 0.071 0.65 0.05 0.059 1.65 0.084 0.25 0.26 0.069 0.071 0.05 0.59 0.52 1.65 0.12

A (A) (Lab) A (A) (Solar) ht.* Ion

Fe 11 ............ Fe 11 ............ N IV ............ Fe 11 ............ Fe 11 ............ AI I I ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Ni 11 ............ Fe 11 ............ N 111 ............ Ni II ............ N 111 ............ Fe €1 ............ N 111 ............ Ni 11 ............ Nru ............ N 111 ............ Ni 11 ............ Fe 11 ............ AI II ............ Fe 11 ............. Fe 11 ............ Ni 11 ............ Fe 11 ............ Fe 11 ............ Ni 11 ............ Fe 11 ............ Fe 11 ............ Ni 11 ............ Si 11 ............ Si u ............ Si 11 ............ Fe 11 ............ Fe II ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ Fe 11 ............ AI 111 ........... Fe II . Fe II . AI 111 Fe II . Fe II . Fe II . Fe I I . Fe II . Si 111 . Fe 111

.......... .......... .......... .......... .......... .......... .......... .......... .......... .......... Fe 11 ............ Fe 11 ............ Fe 11 ............ c 111 ............ Fe 111 ........... Fe 111 ........... Fe 11 ............ Fe 11 ............ Fe 111 ........... C I ............. Fe 11. ........... Fe 11 ............

171 6.577 17 18.123 171 8.551 1720.042 1720.616 1721.26 1722.425 1724.854 1726.391

1731.038 1741.547

;E:%} 1748.285 1748.61 1749.136 1 749.674 175 1.91 1 1752.16P 1753.986 1754.808 1761.379 1763.952 1764.117 1772.509 ' 1773.949 1785.262 1788.072 1788.485 1793.367 1798.1 56 1804.473 1808.012 181 6.928 1817.451 1818.509 1822.150 1823.888 1835.874 1841.701 1846.573 1848.77 1 1854.7 16 1859.741 1860.055 1862.790 1864.743 1876.838. 1877.467 1880.976 1888.733 1892.030 1895.457 1898.538 1901.76 1904.784 1908.734P 1914.071 1915.095. 1917.337 1925.983 1926.3 23 1930.905 1935.296 1936.799

17 16.57 1718.09 1718.56 1720.03 1720.61 1721.27 1722.42 1724.87 . 1726.39 1728.94 1731.05 1741.55 1746.82 1748.28 1748.63 1749.12 1749.67 1751.91 1752.1 2 1753.98 1754.80 1761.36 1763.95 1764.07 1772.50 1773.94 1785.27 1788.04

1793.36 1798.15 1804.48 1808.01 1816.93 1817.44 1818.51 1822.13 1823.89 1835.86 1841.65 1846.57 1848.76 1854.72 1859.74 1860.04 1862.79 1864.72 1876.83 1877.46 1880.97 1888.73 1892.04 1895.48 1898.54 1901.76** 1904.79 1908.74 191 4.07tt 191 5.09tt 1917.31 1925.99 1926.31 tt 1930.91 1935.30 1936.80

1788.48.

0.55 0.25 O.OG? 0.0813 1.37 0.091 0.055 0.89 1.0 0.39 0.m 0.71. 0.20 0.44 0.15 0.045 0.70 0.52

b0a1 0.15 0.10 0.21 0.10

B 0.34 0.11 0.059 0.094 0.26 0.21 0.12 0.069 5 . 6 . 9.5 0.92 0.10 0.063 0.056 0.12 0.081 0.063 . 0.056 1.4 0.14 0.36 0.70 0.16 0.25 0.11 0.081 0.12

0.34 0.050 0.088 0.045 4.05 0.29 0.088 0.053 0.13 0.22 0.55 0.081 0.069

15.2

N a TO TABLE 2 NoTE.-B = blend .

Peak intensity of the line . The units are the same as used in Table 1 . P = predicted wavelength .

435

Notes t o Table 2 (DFUE)

* The d i f f e r e n c e s between o u r measured wavelengths a n d t h e

, wavelengths . g i v e n i n K e l l y and Palumbo '(1973) for these' . .

l i n e s are c o n s i d e r a b l e . We feel t h a t t h e 1.aboratory wave-

l e n g t h s ' are i n error. . .

. + Burton a n d Ridgeley (1970) i d e n t i f y t h i s l i n e .as S V . .

3 . . '; (3s2 'S0.--:3s3p .P1). ' However, t h e l i m b b r i g h t e n i n g c u r v e

for ' . t h i s ' l i n e is s u g g e s t i v e of a lower t empera tu re i o n .

. .

'**The wavelength d i f f e r e n c e between t h e laboratory a n d solar

wavelength is considerable, a n d t h e d i f f e r e n c e is .unexpla ined .

*+We t e n t a t i v e l y i d e n t i f y these weak l i n e s as t r a n s i t i o n s . i n

. ' . phosphorus i o n s .

" 0

++The '1640.39 A H e . 1 1 l i n e is a c t u a l l y composed'of s e v e n

components, e .g. , see Feldman et a l . (1975b).

+ I n t 3 photographic

- .. n e a r 90 c o r r e s p o n d

d e n s i t y measured by a dens i tometer . Va lues

t o s a t u r a t e d l i n e s .

B = b l e n d .

E.2 The Long Wavelength Spectra

E . 2 . 1 ( D F C ) “Chromospheric L imb S p e c t r a from Skylab: 2000 to 3200 A , ” G . A. D o s c h e k , U . Feldrnan and L . C o h e n . A p . J. Supp. Series -- 3 3 , 1 0 1 , 1 9 7 7 .

TABLE 1 (DFC) THE SOLAR SPECTRUM 4' ABOVE THE WHITE LIGHT LIMB: 2000-3200 A

Fluxt A (A) Solar A (A) n(photons cm-l

(air) Lab Ion Mul* s-' sr-')

1986.88 ..... 0.907 Fe rrr 1991.03. .... 0.016 Fe 111 2000.36 ..... 0.368 Fe II 2010.69 ..... 0.688 Feir 2015.48 ..... 0.500 Felt 2018.78 ..... 0.772 Ferr 2020.75 ..... 0.739 Fen 2025.53 ..... 0.58 Cr I I 2029.20 ..... 0.182 Fe 11 2032.40 ..... 0.407 Fe II 2036.44 ..... 0.435 Feir 2039.90 ..... 0.90 Cr I I 2040.68 ..... 0.687 Fe II 2051.04 ..... 0.028 Fer1 2055.59 ..... 0.59 Cr I I 2057.34. .... 0.332 Fen 2061.58 ..... ::I ....... ~-~~ 2062.00 ..... 0.00 Fen$ 2063.69 ..... 0.672 Fen 2065.50. i ... 0.460 Cr II 2067.96 ..... 0.917 Ferr 2068.24 ..... 0.243 Fenr

. 2079.00 ..... 0.989 Fe 111 2080.25 ..... 0.246 Fen 2087.56 ..... 0.527 Fen 2090.14 ..... 0.14 Ni 11 2093.53 ..... 0.55 Ni II 2097.10 ..... 0.08 Nilr 2097.57 ..... 0.512 Ferr 2103.85 ..... 0.799 Fe III 2107.41 ..... 0.324 Fe 111

2108.00 ..... 2110.74 ..... 0.724 Fen 2118.17 ..... 0.195 Feir 2119.03 ..... 0.050 Fen 2125.14 ..... 0.12 Ni II 2128.58 ..... 0.57 Ni II 2130.24 ..... 0.259 Fen 2131.28 ..... 0.27 Nin 2132.67 ..... 0.72 Cr II 2133.50 ..... 0.49 Cr II

052 C r r r

2135.37 ..... 0.34 C r r r 2137.71 ..... 0.735 Ferr 2138.61 ..... 0.60 Niri 2139.01 ..... 2142.77 ..... 2147.68 ..... 8 .719 Fe I I

0.618 Fen 0.762 Fe 11 2150.65.

0.373 Fe II 0.488 Fe II 2152.38

2158.75. .... 0.73 Ni I I 0 161 Fen .

2162.01 ..... 0.023 Fen 2164.34 ..... 0.339 Ferr

0555 Fen

2169.10 ..... 0.10 N i n 2172.95 ..... 0.989 Fen 2174.68 ..... 0.67 Ni II 2175.15. .... 0.16 Nix1 2175.42 ..... 0.445 Fen

2134.56 ..... (0162 cr II

21 39.62. .... 0.676 Fe'ir

2146.05 ..... 0.058 Fk'iI

.... 2151.10 ..... {OB95 Fe 11

.....

2161.21 ..... {0:21 Ni II

2165.55 ..... {&5 ~i

... 7.4ii3) 4.1(13) 4.3(13) 1.0(14) 5.5(13) 3.7(13) 2.2(13) 8.8(13) 3.2(13) 2.4(13) 1.9(14) 1.1 (14) 1.8(14) 2.0(13) 1.5(14)

6.5(13) 1.2(14) 3.0( 13) 1.9( 13) 2.6(13) 4.6(13) 2.1 13) 7.9i12) 9.7( 1 2) 1.1(13) 1.6(13)

2.iii3)

. . . . . i . oii3j i . i 'i3) 8.3112) l.O(l3) 1 . O( 13) 2.0( 13) 1.2( 13) 7.9( 12) 7.9( 12) 1.6( 13) 1.6(13)

7.4( 12) 1.2(13) 2.6(13 1.1(13] 6.0( 13) 1.2(13)

I . i i i3)

~ $ 3 )

i . i i is)

i.jii3) 2.iii3)

1.4(13)

1.3(14) 7.9( 13)

7.4( 1 3) 7.4(13)

Fluxt A (A) Solar A (A) n(photons cm-'

(air) Lab Ion MuP sml sr-l)

2177.06 ..... 0.080 Nir r 2179.37 ..... 0.36 Nirr 2180.48 ..... 0.46 Nirr 2184.60 ..... 0.61 Nia 2185.51 ..... 0.51 Niri 2186.84 ..... 0.89 . Fell# 2187.71 ..... 0.678 Ferr? 2188.02 ..... 0.05 Nia 2189.03 ..... 8.999 Con 2192.31 ..... 0.26 CUII 2201.41 ..... 0.41 Niii 2206.71 ..... 0.71 Niir 2210.38 ..... 0.38 Niir . 952 Ferr

0.112 Fer1 2211.08 ..... 2213.22 ... 2213.65 ... 2216.48 ... 2219.90. .. 2220.38 ... 2221.16 ... 2222.96 ... 2223.48. < . 2224.40. .. 2224.86. .. 2226.33 ... 2227.22. .. 2229.88 ... 2232.08 ... 2233.91 ... 2236.66. .. 2240.34. .. 2241.78. .. 2243.59 ...

.. 0.19 . . 0.679 . . 0.479 . . 0.889

. . 0.160

. . 0.948 . . 0.481 .. 0.351 . . 0.88 . . 0.34 .. 0.18 . . 0.85 .. 0.05 .. 0.917 .. 0.680 .. 0.33 . . 0.81 .. 0.578

. . {x:g8

Ni II Fe II Ni II Fe II Fe u Ni II Fe II Ni II Fe II Ni II Ni II Ni II Fe rr# Ni rri co II Fe II Fe II Fe rr# Fe II# Fe II

2244.03 . . . . . . . . ... -~ 2244.65 ..... 0.60 Feu# 2245.13 ..... 0.11 Coir 2246.93 ..... 0.995 Cu II 2249.17 ..... 0.18 Fer1 2250.17 ..... 0.171 Fen ....

2250.93 ..... 0.937 Feu 2251.55 ..... 0.556 Ferr 2253.13 ..... 0.119 Fen

2255.14 ... 2255.77 ... 2255.94. .. 2256.43 ... 2257.91 ...

2268.58. .. 2268.76. .. 2270.21 ... 2274.73. .. 2275.68 ... 2276.03 ... 2277.28 ... 2278.76. .. 2279.91 ...

2254.37 ..... 0.401 Fen .. 0.16 Fen# . . 0.759 Fe II . . 0.979 Fe II . . 0.43 Fen#

2260.1 1 ...... f:z;8 0.228 F~ F i n II

2260.85 ..... 0.853 Fe II 2262.68 ..... 0.686 Feu 2263.21 ..... 0.224 Fe 11 2264.47 ..... 0.456 Nin 2265.99. .. Fe II 2267.58. .. Fe II 2268.1 1 ... Fe II#

Fe II Fe II Ni II Ni II Ni II Fe II# Ni xrfl Ni II Fe II

...... ~ . . 0.991 . . 0.584 . . 0.14 . . '0.562 . =. 0.844 . . 0.209 . . 0.75

. . 0.70 .. 0.02

. . 0.282 . . 0.771 . . 0.918

1.3(13) 9.7(12) IS( 13) 6.9(13) 2.2(13) 9.7(12) 1a13 6.9(12) ... 1.1 (1 3) 9.2(12) '

5.5(13) 8.3(13) 5.1(13)

6.9(12)

1.3( 14) 2.8(13) 1.1(14) 2.2(13) 9.7(13) 2.1( 1 3) 1.7(13) 1 . 1( 14) 8.8( 13) 7.9( 12)

2.3( 1 3)

7.9tl2)

8.3(12)

8;3 13)

Kit$ i.iii3) 1.8(13) 4.2(13)

9.2(13) 3.8( 13) 1.4(14)

BL 2.2 13) 7.4i12) 2.0(14)

a.iii3) 4.6(13) 1.2(13) 1.2(14) 4.3(13)

1.5( 1 3) 1.2(14) 6.9( 12) 1.1(13) 1.4( 13) 3.6( 1 3) 1.4(14) 2.6(14)

TABLE 1-Continued (DFc)

Fluxt A (A) Solar A (A) rr(photons cm-l

(air) Lab Ion Mul+ s-l sr-l)

2283.99. .... 2286.14 ..... 2287.08. .... 2287.61 ..... 2293.76. .... 2294.60. .... 2296.58 ..... 2297.12 ..... 2297.44. .... 2298.26. .... 2298.91 ..... 2299.64. .... 2300.07 ..... 2301.38 ..... 2302.48. .... 2302.99. .... 2303.23 ..... 2304.75 ..... 2304.95. .... 2307.15 ..... 2307.84. .... 2311.23 ..... 2311.61 ..... 2312.02 ..... 2312.91 ..... 2314.04 .....

. 2314.75 ..... 2314.93 ..... 2316.04 ..... 2318.52 .....

. 2319.36 ..... 2319.74 ..... 2320.06. .... 2321.68 ..... .2322.3 4 . .... 2323.52 ..... 2324.39. .... 2324.72. .... 2325.40. .... 2326.16. .... 2326.46. ....

2314.75 ..... 2314.93 ..... 2316.04 ..... 2318.52 ..... 2319.36 ..... 2319.74 ..... 2320.06. .... ~~ ~~~~ .

2321.68 ..... ,2322.34. .... 2323.52 ..... 2324.39. .... 2324.72. .... 2325.40. .... 2326.16. .... 2326.46. .... 2326.98 ..... 2327.39. .... 2328.14 .... 2330.35 ..... 2331.30 ..... ~~

2332.81 ..... . 2334.55 .....

2335.44. .... 2336.21 ..... 2336.70 ..... 2338.01 ..... 2339.40. .... 2340.46. .... 2341.12 ..... 2342.22. .... 2343.41 ..... 2343.90. .... 2344.24 ..... 2345.34 ..... 2347.40. .... 2348.21 ..... 2350.17 ..... 2351.19 ..... 2352.09 .....

0.991 0.165 0.08 0.66 0.765 0.605 0.55

0.486

0.95 0.65 0.10 0.424 0.465 0.98 0.238 0.736 5.001 0.19 0.84 0.224 0.602 0.028 0.91 0.036

0.97 0.034 0.534 0.38 0.73 0.08 0.687 0.326 0.500 0.317 0.689 0.398 0.15

0.930 . 0.391 0.122 0.37 0.308 0.798

Go G:%

e:;;

c:z3

$:E 0.42 0.246 0.70 0.005 0.408

0.238 0.495 0.958 0.278 0.327 0.406

0.174 0.198

E:: ...

Fe II c o 11 Ni I I Ni II Fe II Fe II Ni II Ni II Cr II N ~ I I Fe II Ni II Mn 11 Ni II Ni II Fe II Ni II Ni II v I!? Fe II Mu 11 Cr II co 11 Fe II co 11 Fe II Ni II co 11 Cr 11 Cr II co I1 Ni 11 Fe I I Cr 117 Ni I I Cr II Fe I I Fe I I c I15 co I1 c 115 c 115 co 11 Ni 11 co 11 c 115 Fe II c 118 co 11 Fe 11 Fe II Ni II si 11 Fe II$ co 11 Ni II Fe II Fe I I Fe II Fe II Ni II Fe 11 Fe II Fe II Fe II Fe II co 11 Fe II Fe II Si II Fe II ...

4.0( 1 3) 4.6 13) 6.9tl3)

1.7(14) 2.3(14)

i.iii4)

8.8ii3) 9.2( 12) 2.6( 13) 3.0(13) 8.3(12) 1.4(13) . 2.1 (14) BL 1 . 5(I 3)

5.1(13) 1.1(13) 4.6(13) 4.6(13) 2.4(13) 2.1(13 1.8(13]

2.8ii3) 3.3(14) 3.3(13) 1.8(13) 9.2(12) 1.4( 13) 1.3( 13)

1.9ii4)

4 5 3 )

5.jii3)

3.8( 14)

4.6( 14) 2.2(14)

5.jii4)

I . iii3) 1.7(13) 5.1 (1 4) 7.4(13) 3.9(13)

2.iii3) 3.0(13)

5.5( 14) 1.2(14) 2.0( 13) 6.5(14) .

2.iii4) 1.0(14) ...

Fluxt n(photons cm-z A (A) Solar A (A)

(air) Lab Ion Mul* s-* 5r-l)

2352.69 ..... 2353.42 ..... 2354.50 ..... 2354.90. ... ; 2356.40. .... 2357.00 .....

.... 0.446 0.473 0.884 0.41 0.005

2359.12 ..... 0.111 2359.97 ..... 0.999 2360.28 ..... 0.287 2362.00 ..... 0.014 2363.80 ..... 0.838 2364.83 ..... 0.825 2366.61 ..... 0.591 2367.38 ..... 0.395 2368.60 ..... 0.593

... co 11 Fe II Fe I I Ni I I Fe II Fe II

Fe II

Fe I I Fe II Co I1 Fe II Fe II Ni II Fe II

369.19 ..... 0.232 Fe II 2370.50 ..... 0.494 Fen 2372.63 ..... 0.631 Feir 2373.74 ..... 0.733 Fen 2375.23 ..... 0.192 Fe II 2378.61 ..... 0.636 Co II 2379.26 ..... 0.275 Feu 2380.77 ..... 0.757 Fe II 2382.08 ..... 0.034 Fea

2387.77.- ... 2388.58 ..... 2389.53 .....

2383.15 ..... 2384.40 ..... 0.386 . Fen 2384.99 ..... 0.999 Fen 2386.35 ..... 0.367 Con 2387.43 ..... 0.424 Fen

0.77 Ni II 0.629 Fe II 0.565 Co II

2391.47 ..... 0.475 Fen 2394.53 ..... 0.518 Niir 2394.85 0.892 Fe 11

0.627 Fe I I 2395.59. 2395.71 ..... 0.714 'Feu 239i.39. .... 0.423 Con? 2399.25 ..... 0.237 Fe II

..... ....

0.255 0.597 0.430 0.882 0.660 0.940 0.770 0.377 0.708 0.52 I 0.062 0.308

0.068 0.134 0.705 0.85.9 0.735

G:E

2421.92 ..... 0.898 Fe II

2400.33 ..... 2402.28. .... 2402.59 ..... 2404.40. .... 2404.90 ..... 2406.68. .... 2407.92. .... 2408.73 ..... 2409.37 ..... 2409.70. .... 2410.54 ..... 2411.05 ..... 2413.32 ..... 2414.08 ..... 2415.06 ..... 2416.14 ..... 2416.82 ..... 2417.85 ..... 2420.74. ....

Fe II Fe II Fe 11 Fe 11 Fe II Fe 11 Fe 11 Fe II co I1 Fe II Fe II Fe 11 Fe II Fe II co I1 Fe II Fe II Ni 11 Fe 11 Fe II co I1

.....

2422.70 ..... 0.688 Pe II 2423.20 ..... 0.204 Fe 11 2424.16 ..... B.141 Fen

0.380 Pe II 0.585 Fen 2424.47

2425.36 ...... 0.362 Fe 11

.....

2.iii3) 1.0(14) 3.9( 14) 2.5(13) 1.6( 13) 4.8(14) 6.5(14)

3.3(14) 5.9( 13) 5.2( 14) 2.8(14) 2.7(13) 5.2(14) 2.5(13) 3.1(14) 1.8( 13) 4.8(14) 5.2(14) 4.8( 13) 4.3(14) 3.7(14) 1.0(15)

6.y1q

9.6(14) 4.8(14) 1.4(14) . 3.2(13) 1.6( 13) 2.2(13) 4.2( 14) 1.6(13) 2.2(14) 1.8(14) 8.6(13) BL 5.2(14)BL 5.2(14) 4.4(13) 2.1( 13) 4.3(14)

1.7(14)

i .qi4) 2.8(14) 4.7( 14) 4.7(14) 5.0(13) 1.8(13) . 1.3( 13) 1.5( 13) 4.3(14) 4.0(14) 4.3(14) 2.4(13) 5.3(13) 2.5(14) 1.5( 13) 22(14)

1.3( 13) 5.0(13) 3.3(13)

1.1(13)

2.6(14)

1.7(13)

104

TABLE l-Confinued( f)

Fluxt . x (A) Solar A (A) =(photons cm-'

(air) Lab Ion Mul* s-I sr-')

2425.72 ..... 2427.18 ..... 2428.34. .... 2429.40. .... 2430.09. .... 2432.26 ..... 2433.50. .... 2434.85 ..... 2435.80 ..... 236.20 ..... 2437.18 ..... 2437.89 ..... 2439.30 ..... 2440.42. .... 2444.52 ..... 2445.58 ..... 2446.16 ..... 2446.47. .... 2447.25. ....

0.677 0.197 0.367

0.073 0.259

$2; $:F {E;

0.816 0.222 0.157 0.892 0.301 0.416 0.515 0.569 0.203 0.462

{::E

Fe 11 Fe 11 Fe II Fe 11 Fe II Fe 11 Fe I I Fe XI Ni 11 Fe XI Fe II Fe 11 Fe II Fe 11 Ni 11 Fe II Fe II Fe II Fe II Fe II Fe 11 Fe 11 Fe 11

2447.74 ..... -0.753 Fen 2449.20 ..... 0.185 Fe II 2449.75 ..... 0.739 Fe 11

2451.14 ..... 2453.79 ..... 2454.57 ..... 2456.81 ...... 2458.79. ....

. 9.961 Fe 11

0.208 Fe 11 0.794 Fen 0.574 Fe II 0.816 Fen

2450.04 .....

2458.99.- ... 2461.29 ..... 0.282 Fen .... ~

2461.83 ..... 0.855 Fe 11 2463.29 ..... 0.280 Fe 11 2464.01 ..... 0.007 Fen 2464.96 ..... 0.903 Fe 11 2465.15. .... 0.194 Fe II .........

2465.91. .... {0.911 Fe 11 0.670 Fe 11 0.811 Fe 11 2466.76. ....

2468.29 ..... 0.292 Fen 2469.49. .. 2470.47. .. 2470.68. .. 2472.10 ... 2472.42 ... 2472.91 ... 2473.30. .. 2474.75. .. 2476.26 ... 2476.66. .. 2477.35 ... 2478.19 ... 2478.56. .. 2479.86 ... 2480.15 ... 2481.04 ... 2482.12 ... 2482.64. .. 2483.25 ... 2483.73 ... 2484.23 ... 2485.04. ..

.. ..

..

.. .. .. .. .. .. .. ..

..

..

.. .. .. .. .. .. .. .. ..

0.512 0.406

0.075 0.426 0.910 0.314 0.762 0.264

0.342

C:%

... ("0:::; C:%

0.775 0.155 0.044 0.1 17 0.654 0.270 0.721 0.243 0.076

Fe II Fe II Fe II Fe 11 Fe II Fe 11 Fe I Fe II Fe 11 Fe II

Fe II Fe II Fe II Fe 11 Fe II Fe I Fe II Fe II Fe II Fe 11 Fe I Fe II Fe 11 Fe II

...

2.4(13) 1.6( 13) 7.9(13) 7.2(13) 2.8(14) 2.3(14) 1.1(14)

1.51 3) 1.8(13) 2.0 13) 8.6t13) 3.0(14) 4.2( 1 3) 4.0(14) 3.3(14) 2.0(14)

... i . 4 'i4)

4.4(13) 4.0( 13) 1.3 1 3)

6.0(13)

5.7( 1 3)

5.7 13) 1.9t13)

2.9(14)

I . 9(14) 2.6(14) 8.1 (1 3) 1 . O( 14) 1.1 (1 4) 1.2( 14) 1.0(14) 1.6(14) 9.0(13)

8.6ii3)

s.iii3)

2.3(14)

2.1(13) 6.0( 13)

7.1 (I 3) 8.2(13) 4.8( 13) 6.0( I 3)

1.8(14)

2.6( 14) 3.5(13) 2.8(14) 1.4(14) 3.2( 13)

2.0( 13)

8.jii3)

Flux? X (A) Solar X (A) n(photpns cm-a

(air) Lab Ion Mul* . s- s r l )

2486.35 ..... 0.343 2488.14 ..... 0.143 2489.51 ..... 0.485 2489.81 ..... 0.826 2490.84 ..... 0.856 2491.38 ..... 0.392 2492.35 ..... 0.341

0.174 { 0.269 2493.25

2494.11 ..... 0.111

2497.80 .....

.....

2498.90. .... 2500.93 ..... 2502.39. .... 2503.38 ..... 2503.82. .... 2505.21 ..... 2506.09 ..... 2506.38 ..... 2506.94. .... 2509.12 ..... 2510.88 ..... 2511 .44 ..... 2511.77 ..... 2512.52 ..... 2514.38 ..... 2514.91 ..... 2516.10. 2517.13. 2518.08. 2519.05. 25 19.80. 2520.67. 2521.09. 2521 .82 . 2522.18 . 2522.86. 2524.1 5 . 2525.41. 2526.22. 2527.1 1 . 2527.43. 2528.59. 2529.24.

.... .... .... .... .... .... .... .... .... .... .... ....

....

.... .... .... ....

-0.897 0.919 0.388

(0.323 0.560 0.870 0.217 0.091 0.429 0.896 0.117 0.87 0.375 0.759 0.513 0.383 0.912 0.108 . 0.124 0.100 0.044 0.829 0.669 0.089 0.810 0.189 0.848 0.108 0.386

0.107 0.433 0.51 0.22 I

g;;;

Fe II Fe I Fe II Fe 11 Fe 11 Fe II Fe II

Fe II

Fe II Fe 11 Fe II

Fe II Fe II Fe 11 Fe II Fe II

Fe II

Fe II Fe II Fe 11 Fe 11 Si I Fe II Ni 11 Fe 11 Fe 11 Fe II Fe II

Fe II

Si I Fe II Fe I Fe 11 co XI? Fe 11 Fe 11 Fe II Fe II Fe I Si I Fe IJ F e . 1 1 Fc 11 Fe II Fe I Si I Fe II

2529.55 ..... 0.545 Fe 11

2530.09 ..... 0.103 Fen 0.082 Fe 11 0.266 Ti XI? ..... 2531.20 {

2532.68 ..... 2533.41 ..... 0.413 Fen 2533.64 ..... 0.626 Fk'iI ............ 2535.47 ..... 0;480 Fe 11 2535.75 ..... 2536.81 ..... 2538.32 ......

0.794 Fe 11 2538.95 ..... 0.898 Fe II

9.003 Fen 2540.67 ..... 0.669 Fe 11

2541.08 ..... 0.094 Fen 2541.83 ..... 0.831 Fe 11

1.8(14) 3.4(13) 1.8( 1 4) 2.8 14) 1.7[14) 9.6(13) 4.0(13)

8.5(14) . . .

2.5(13) . 1.4(14) 4.5(14) 2.7(13) 1.3(14) W14)

...

... 1.2(14) 4 6 13) 1&4) 3.4(13) . 1.8(13)

El::; 6.iii4) 2.4(13) 8.8(13) 5.0(13)

z.iii3) 2.0(14) 1.4(13) 1.1 (1 4) 1 . 8( 13) 2.1 13) 7.411 3) 4.8(13) 3.5(13) 5.7(13) 1.3(13) 5.1 (1 4)

1.4(14) 6.7( 13) 3.2( 13)

5.3(14) 2.3(14) 4.5(13)

7.5(14) 6.0(14) 2.6(14)

3.iii4)

...

1 . qi i)

a.qi4)

2.iii4)

6.5(14)

9.0(13) 1.6(14) 3.3(14)

1 05

TABLE I-Continued (De) Fluxt

x (A) Solar A (A) =(photons cm-' (air) Lab Ion Mu]* s-' sr-')

2542.74. .... 2543.38 ..... 2545.15 ..... 2545.87 ..... 2546.67 ..... 2547.32. .... 2548.37. .... 2548.72 ..... 2549.40. .... 2550.02 ..... 2550.67 ..... 2553.71 ..... 2555.06. .... 2555.42. .... 2555.96 ..... 2557.52. ..... 2558.60. .... 2559.80 ..... 2560.26 ..... 2562.16 ... : . 2562.54. .... 2563.48 ..... 2566.26 ..... 2566.91 ..... 2567.51 ..... 2568.39 ..... 2569.76 ..... 2570.84. .... 2571.50 ..... 2571.90 ..... 2572.58 ..... 2573.20 ..... 2574.36 ..... 2576.1 1 ...... 2576.87 .. ._. . 2577.92. .... 2579.42. ..... 2580.30 ..... 2581.32 ..... 2582.59. .... 2585.88. .... 2587.19 ..... 2587.94. .... 2590.59. .... 2591 .55 ..... 2592.77. .... 2593.72. .... 2595.21 ..... 2598.39 ..... 2599.40 ..... 2605.63 ..... 2606.56. .... 2607.01 ..... 2608.86. .... 2609.07 ..... 2609.87 .... 2610.16 ..... 2611.08 ..... 261 1.88 ..... 2613.83 ..... 2617.62 ..... 2619.07 ..... 2620.45 ..... 2621.66 ..... 2623.11 .... '.

0.733

{E 6:;;:

G:E 6::;:

0.903 0.667 0.330 0.325 0.741

0.023

0.738 0.066 0.447 0.988 0.500 0.605 0.774 0.278 0.094 0.535 0.472

0.908

0.405 0.775 0.843 0.542 0.78

0.206 0.363 0.107 0.859 0.920 0.406 0.372

. 0.582 0.876 0.225 0.945 0.548 0.542 0.781

...

...

...

...

{E; 0.285 0.369 0.395 0.697 0.514 0.084 0.852 0.122 0.859 0.202 0.075 0.873 0.820 0.618 0.071

0.669 0.129

6:Z

Fe I I Fe 11 Fe II Fe II Fe II Ni 11 Fe II Fe 11 Fe 11 Fe 11 Fe 11 Fe II Fe 11 Fe II Fe 11 Fe 11 Fe 11 Fe 11 Ti rr? Fe 11 Mn II Fe II Fe 11 Fe 11 Fe II Fe II

Fe I I

Fe II Fe II Fe 11 Fe II? Cr 11

Fe I I Fe II Mn II Fe 11 Fe 11 Fe I I co r r ?

Fe u Fe I I co 11 Fe 11 Fe 11 Fe II Fe II Fe I I Mn II Fe 11 Fe II Fe I I Mn II Fe 11 Fe II Fe 11 Fe I I Fe II Mn 11 Fe 11 Fe 11 Fe 11 Fe II Fe 11 Fe II Fe II Fe II Fe II

...

...

...

...

5.4(13) 3.8(14) .

3.2(14)

2.8(14) 6.6( 13) 8.7(13) 2.3( 14) 3.1(14) 4.0(14)

2.7( 13) 8.5(13) 5.6(13) 2.2(13) 9.9(13) 4.6(13) 1.1 (14) 2.5(14).

1.2(15) 5.6(13)

2.2(13) 1.0(14) 2.3( 13) 1.5(14) 3.1 (I 3) 2.4(13) ,1.6(13) 8.6(13) 6.0( 14) 6.5(14) 7.5(13) 1 . O( 15) 4.4(13) 9.5(13) 2.6(13) 9.4(14) 2.5(15) 3.0(13) 8.5(13) 4.7(13) 1.2(15) 4.4(14) 8.8(14)

...

3.5( 1 3)

3.4ii4)

I . 9(15)

1.2(15)

>;:% > 2 3 1 5)

6.5(14)

> 2.5ii5)

3.9ii3) 7.1( 13) 7.5(13) 3.0 14)

> 2.5tI 5) > 2 3 1 5) >2.5(15)

a.qi4)

!:%{ 2.6( 13)

2623.74 ..... 2625.66. .... 2626.46. .... 2628.30 ..... 2629.58 ..... 2630.05 ..... 2631.21 ..... ,2632.31 ..... _.__ ~ ~ ~

2633.20. .... 2637.62 ..... 2638.13 ..... 2639.60. .... 2641.98 .... i 2653.56 ..... 2658.58. .... 2661.70 ..... 2663.49. .... 2664.66. .... 2666.00 ..... 2666.63 ..... 2668.70. .... 2669.14 ..... 2671.78 ..... 2672.80 ..... 2677.15 ..... 2678.77. .... 2684.73 ..... 2687.06. .... 2687.94. .... 2688.20. .... 2689.15 ..... 2691.02 ..... 2692.63 ..... 2697.44 ..... 2698.52 ..... 2701.67 ..... 2703.98 ..... 2705.70 ..... 2708.40. .... 2709.06. .... 2710.28 ..... . ~~~~~~~~~~

2711.84 ..... 2712.31 ..... 2714.41 ..... 2716.21 ..... 2717.51 ..... 2718.99 ..... 2722.72 .... 2724.86 .... 2726.47 2727.50 2730.72 2732.41

....

....

.... .... 2736.96 .... 2739.56 .... 2741.37 .... 2742.00. .... 2743.22 ..... 2746.42 ..... 2747.03 ..... 2749.30. .... 2750.70. ....

0.721

0.499 0.291 0.590

{:::E

f:: 0.321 0.353 0.200 0.643 0.173 0.560 2.015 0.57 0.59 0.73 0.42 0.665 0.02 0.631 0.71 0.17 0.80 0.83

0.79 0.752 0.09 0.960 0.28 0.20 0.03 0.601

0.40 0.693 0.988 0.727 0.442 0.051 0.332 0.842 0.300 0.414 0.216

9.027 0.74 0.879 0.509

0.735 0.441 0.968 0.545

0.02 0.196 0.487 6.978

G:fi

c::::

G%3

GE

0.395

p::;: 0.482

0.72

Fe 11 Fe 11 Fe II Fe 11 Fe II Fe II Fe II

Fe II

Fe 11 Mn 11 Fe 11 Fe 11 Mn II Fe 11 Fe 11 Cr 11 Crn Cr II Cr II

. Fe 11 Cr II . Fe 11 'Cr 11 AI II Cr II Cr II Cr 11 Cr 11 cr 11 Fe 11 Cr 11 v II? Cr II Cr II Cr II Fe II Fe 11 Fe 11 Cr 11 Mn II Fe II Mn 11 Mn II Fe II Mn u Fe II Cr II Fe 11 Fe 11 cr I1 Fe 11 Fe II cr 11 Fe 11 Fe II Fe II Fe II Fe II Fe 11 Fe II Fe II Fe II Cr 11 Fe II Fe 11 Fe II Fe II Fe 11 Fe II Cr I!

8.0(13)

1.5[14) 1.5(15) 2.4(14) 1.8(14)

3.9(15)

4.7(13) 3.2( 1 3) 1.1 (I 4)

4.3(13)

7.4 13) 1.6t14 7.0(14{ 2.8(14) 5.(?(14) 2.9( 14) 7.1 (14) 3.9(14) 2.8(14) 7.6(14) 4.3(14)

5.3(13) 4.9(13) 3.2(13) 1.6(14) 3.2( 14) 5.5( 13) 3.6(14) 1.1 (14) 4.3(14)

1. ii 'is,

l.l(L5) 3.2(14) 8.1(13) 4.2(13 1.6(14{ 3.8(14) ... 1 .%is) 5.9(14) 7.6(13) 1.1(15) 2.3( 15) 4.3(13) 6.6( 13) 1.9(15) 1 . 9( 15) 1.7(15)

2.0(15)

1.8(14)

CHROMOSPHERIC LIMB SPECTRA FROM SKYLAB

TABLE I-continued (J Fiz> 1 07

FIuxt x (A) Solar A (A) =(photons cm-l

(air) Lab Ion MuP s-’ sr-l)

2751.07 ..... 2751.85 ..... 2753.27 ..... 2755.74. .... 2756.97 ..... 2757.69. .... 2759.29 ..... 2761.79 ..... 2762.56 ..... 2766.52. .... 2767.50. .... 2768.93 ..... 2769.26. .... 2774.62. .... 2779.29. .... 2779.78. .... 2783.68 ..... 2790.75. .... 2793.90. .... 2795.55. .... 2797.96. .... 2799.29. .... 2802.72. .... 2818.30 ..... 2822.34 ..... 2828.60 ..... 2830.45. .... 2831.54 ..... 2835.64. .... 2839.99. .... 2840.64. .... 2843.24 ..... 2848.03. .... 2849.81 ..... 2852.11 ..... 2855.67. .... 2856.74. .... 2857.37. .... 2858.36 ..... 2858.88 ..... 2860.92. ..... 2862.55. .... 2865.10 ..... 2866.73. .... 2867.63 ..... ~~~~ .......

2868.81 ..... 2870.43. ....

0.121 0.85 0.289 0.733 7.029 0.72 0.336 0.813 0.58 0.55 0.50 0.940

0.686 0.302 0.832 0.690

0.887 0.523

G:E

%E

{::E 0.292 0.698

0.38 0.622 0.46 0.562 0.630 4.01 0.644 0.24 0.016 0.83 0.120

C:f36 0.77 0.40 0.340 0.910 0.92 0.57 0.10 0.72 0.65 0.874 0.430

...

Fe II cr 11 Fe II Fe II Fe II Cr II Fe II Fe II Cr II Cr II Fe 11 Fe II Fe II Fe 11 Fe II Fe II Mg I? Fe II Mg 11 Fe II? Fe II M g II Fe II Mg II Fe II Mg II

Cr II Fe II cr I1 Fe II cr I1 Cr 11 Fe II Cr 11 Fe II Cr 11 Me I Cr II Fe II cr I1 cr 11 Fe II

Cr II Cr II cr 11 Cr 11 Cr II cr I1 Fe II Cr II

...

1.0(14)

2.3( 1 5) 4.0(13) 1.3(14) 6.4(13) 4.0( 14) 2.1(14) 3.4(14) 9.9(14) 2.1 (14)

4.7( 1 3) 3.9(14) 7.7( 1 3) 5.8(14) 1.5(14) 5.1 (1 3) S 2.4(14) 5.4( 13) S 3.7(13) 7.9(13) 4.9( 1 3) 8.5(13) 2.9(14) 4.5(14) . 7.1 (1 3) 1.5(14) 4.8(14) 4.9(13) 4.0( 14) 3.4(14) 3.8(14)

:::I:$

i.iii4)

:::I::{ 1.3(14) 1.9( 14) 2.1 ( I 4) 2.5(14) 3.9(14)

5.0(13) 1.6(14)

Et::;

H u t X (A) Solar A (A) n(photons cm-a

(air) Lab Ion Mull s-l sr-’)

2873.41 ... 2873.74. .. 2875.35. .. 2876.00. .. 2877.95. .. 2880.79 ... 2889.1 8 ... 2889.52. .. 2898.58 ... 2926.56. .. 2933.06 ... 2936.49. .. 2939.31 ... 2944.39 ... 2947.65. .. 2949.22 ... 2953.74. .. 2984.84. .. -~ ~ ....... 2985.54 ... 3002.63 ... 3066.26. .. 3072.96. .. ......

3075.22 ... 3078.66 ... 3088.04 ... 3095.57. .. 3100.68 ... . . . . . .

3102.32 ... 3110.67 ... 3118.61 ... 3120.36 ... 3124.98 ... 3128.70 ... 3132.07 ... 3136.70 ... 3147.98 ... 3154.20 ... 3161.18 ... 3161.75 ... 3162.59 ... 3168.51 ... 3179.32 ... 3180.68 ... 3186.72 ... 31 87.76. .. 3190.87 ... 3192.93 ... 3193.78 ...

. . 0.81 . . 0.342

. . 0.97

.. 0.190

.. {E

. * G:iE

. . . . . . . . . . .. 0.584 . . 0.051 . . 0.496 . . 0.302 . . 0.399 . . 0.658 . . 0.201 . . 0.774

. . 0.831 ....... .. 0.545 . . 0.650

. . 0.971

.. {::E:

.. . . 0;225 . . 0.645 . . 0.027 . . . . . .. . . 0.295 . . 0.703 . . 0.652 . . 0.371 . . 0.978 . . 0.699 . . 0.058 . . 0.680 . . 8.033 . . 0.195 . . 0.205 . . 0.775 .. 0.570 . . 0.519 . . 0.332 . . 0.73 . . 0.740 . . 0.743 . . Oi874 . . 0.917 . . 0.809

Fe II Cr II Cr II Fe II Cr II Cr II Cr II Fe II Fe II Cr II

Fe II Mu II Mg II Mn II Fe II Fe II Mn II Fe II Fe II Fe II Fe II Ti II Ti II Ti II Ti 11 Ti II Ti n OH v 11 v I1 Cr II Cr II Cr II Cr II Cr II cr I1 Ti 11 Ti II Ti II Ti II Ti 11 Ti II ca I1 cr I1 Fe II He I Ti 11 Fe II Fe II

... ...

...

1.7(14)

6.9(13) 2.4(14) 6.0(13) 1.6(14) ..

7.jii3)

1.2(14) 1.7(14) 1.7(14) 2.1(14) 3.0(14) 3.3(14)

2.iii4)

;::!::I 2 8 14) 3.5114) 1.3(14) 6.7(14) 1.2(14) 1.2(14) 1.6(14) 1.3(14) 1.3(14) 1.8(14) 2.3(14) 1.2(14) 2.3(14) 1.7( 1 4)

1.1(14) 1.ql4)

.:.it$

NOTES rn TABLE 1 Nm.-BL = blend. S = very strong line . Slightly more accurate wavelengths for the Ni II lines are given by Shenstone (1970) .

Multiplet from cited references to Moore’s compilations . t Fluxes are values at the Sun . True intensities in photons cm-l s-I sr-’ are obtained by dividing the numbers in the table by

# Identification was suggested tous by Johaasson (1975) based on his work or on the work of Dobbie (1938) . 0 Identification was suggested to us by Kelly (1976) .

n/1.7 (see text for discussion) .

108 DOSCHEK, FELDMAN, A N D COHEN Vel. 33

.

0 - C I I (11.26eV,4.2(-4)) ), 0 -01 (6 .9 ( -4 ) ) x - SilI (8.15eV,4.5 ( -5 ) ) v - C r I I (6.77eV,5.1(-7)) 8 - M ~ I I ( 7 . 4 3 e V , 2 . 6 ( - 7 ) ) A - Fe II (7.87eV,3.2(-5)) + - Fe m 6 . 2 eV,3.2(-5)) o - CoII ' (7.86eV,7.9(-8)) + - Ni II (7 .64eV, 1.9 (-611 Y

2" 4 " 6" 8 10" 12" 0.001

ARC SECONDS ABOVE WHITE LIGHT LIMB RQ. 2.-The intensity behavior of chromospheric ions above the limb. The data in parentheses are the ionization potential of

the next lower stage of ionization (Kelly and Palumbo 1973) and the element abundance relative to hydrogen (Ross and AIler 1976). The Upper hln 11 curve is derived from the 7S_7P lines (see text).

The solar wavelengths were obtained by a standard polynomial fitting procedure. The wavelength accuracy was found to . be 20.04 A. The wavelength standards used to calibrate the spectra were lines of Fe II and Cr 11. The laboratory wavelengths were obtained from the sources from which identifications were made. Most of the identifications were based on the compilations of Moore. These are the Ultra- violet Multiplet Tables (NBS Circular488), the Selected Tables of Atomic Spectra (NSRDS-NBS 3), and A Multiplet Table of Astrophysical Interest (NBS Tech- nical Note 36). A few identifications have been obtained from other unpublished sources. These are marked in the table. Moore's multiplet numbers are also given, as well as intensities derived as described above. In obtaining the line intensities, it was necessary to

perform the integration in equation (3). If a line is optically thin and has a Gaussian profile, 1: in equation (3) is given by

(4)

where I,,' is the peak line intensity, RA is the instrumental response at line center, and W is the full width at half-maximum'intensity. Most of the lines in Table 1 have some opacity, and therefore equation (4) does not strictly apply. However, at +4" above the limb, the position for which we give intensities, the opacity of most of the lines is small and the line profiles are approximately Gaussian. We found empirically that W = 9.4 x 10-6h for most of the singly ionized

,

E.2.2 (FD) "The Emission Spectrum of a.Hydrogen Balmer Series Observed Above the Solar Limb frorn Skylab 11. Active Regions," U. Feldman and G. A. Doschek. Submitted to Ap. j.

TABLE 1

Active Regions Observed - ---- --- - -

Active Region Plage No. Time (UT)

d (31 May 1973) 357 16h55. 2m - 18h20. 8m B (11 Aug 1973) 174 18h43 i 5m - 20h-16. 4m

hI c Bla t h

-

C (29 Aug. 1973) 488 201’36. 2m - 221213. 6m

TABLE 2 (?ED) PROPERTIES OF HYDROOEN BALMER LINES IN ACTIVE REOXONS ABOVE THE SOLAR LIMn

A m i m RE~ION A A ~ I V E REGION B ACTIVE R~~GXON C ~~ + 2" + 4' + 6' + 2' + 4' + 6' + 2" + 4' + 6'

rn A(A) Int.+ AAt(A) Ipt. AA(A) Int. AA(A) h t . AA(A) Int. AA(A) Int. AA(A) Int. ANA) Int. ANA) Int. AA(A)

9 ...... 3835.38 . . . . . . 22.0 0.39 . . . . . . . . . . . . 16.3 0.42 3.0 0.47 . . . . . . 17.1 0.42 3.8 0.50 10.. .... 3797.90 . . . . . . 16.0 0.39 . . . . . . . . . . . . 11.0 0.41 2.0 0.47 . . . . . . 12.6 0.42 2.7 0.46 I1 ...... 3770.63 . . . . . . . . . . . . . . . . . . . . . . . . 6.6 0.37 1.3 0.37 . . . . . . 10.0 0.42 1.8 0.46 12, ..... 3750.15 ... ... 8.6 0.41 5.5 0.36 1.0 0.39 7.5 0.39 1.5 0.44

14 ...... 3721.94 ... ... 5.2 0.42 . . . . . . . . . . . . . 3.7 0.42 ... ... 15.. .... 3711.97 ... 3.5 0.37 . . . . . . . . . 3.0 0.42 49.0 0.33 4.5 0.41 ... 16 ...... 3703.85 j j . i 0.39 2.4 0.34 . . . . . . 22.6 0.iO 1.8 0.37 . . . . . . 37.8 0.36 3.1 0.37 ... ... 17 ...... 3697.15 28.7 0.36 2.1 0.34 . . . . . . 20.2 0.32 1.9 0.36 . . . . . . 32.3 0.37 2.9 0.37 ... ... 18 ...... 3691.55 24.7 0.36 2.1 0.39 . . . . . . 16.2 0.29 2.0 0.47 ... 27.7 0.41 3.4 0.50 ... 19 ...... 3686.83 19.5 0.36 2.1 0.44 . . . . . . 15.0 0.32 1.5 0.41 . . . . . . 24.4 0.41 2.5 0.51 ... 20 ...... 3682.81 16.3 0.32 1.6 0.46 . . . . . . 12.0 0.33 1.2 0.37 . . . . . . 20.7 0.41 1.8 0.37 ... 21.. .... 3679.35 13.6 0.32 1.5 0.47 . . . . . . 12.0 0.36 1.0 0.37 . . . . . . 19.2 0.45 1.8 0.44 ... ... 22 ...... 3676.36 12.2 0.37 . . . . . . . . . . . . 10.3 0.44BLz ... 17.2 0.48 ... ... 23 ...... 3673.76 9.9 0.34 . . . . . . . . . ... 7.9 0.39 ... . . . . . . 24 ...... 3671.48 9.9 0.38BL . . . . . . 8.9 0.47BL 14.8 OSSBL ... 25.. .... 26G9.46 8.1 0.37 . . . . . . ... 6.7 0.43 11.9 0.50 26 ...... 3667.68 5.6 0.40 . . . . . . . . . . . . 5.8 0.44 ... ... . . . . . . 10.9 0.51 . . . . . . ... ... 27 ...... 3666.10 . 5.5 0.42 . . . . . . . . . . . . 5.3 0.46 . . . . . . 28 ...... 3664.68 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7.6 0.55 . . . . . . ... ... 29 ...... 3663.40 4.9 0.52 . . . . . . . . . . . . 5.2 0.55 ... 8.3 0.64 ... 30...... 3662.26 ... . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ... . . . . . . . . . . . . . . . 4.2 0.56 ... 31 ...... 3661.22 ...

. . . . . . . . . . . . . . . . . . 13.. .... 3734.37 . . . . . . 6.3 0.41 . . . . . . . . . . . . 4.1 0.37 0.9 0.42 . . . . . . 6.4 0.41 ... 1.5 0.48 . . . . . . ... 5.2 0.41 . . . . . . ...

... ... ... ... . . . . . . . . . . . . . . . . ... . . . . . . . . . . ... 14.5 0.50 . . . . . . . . . . . . . . . . . . . . . . . . . . . ... . . . . . . . . . . . . ... ... ... ...

... . . . . . . ... ... . a . 8.4 0.53

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

Intensity in units 105 ergs - s-l - s r X at the Sun. t AA P <FWHM> of the line after correcting for instrumental width. ! BL = blend.

E . 3 Forbidden Lines

E . 3 . 1 (SBT) "Forbidden L i n e s of t h e Solar Corona and T r a n s i t i o n Zone 9 7 5 A - 3000 A , " G . D . S a n d l i n , G . E . Brueckner and R . Tousey. Submitted to Ap. J.

TABLE I c$i3 T) FORBIDDEN LINES OF 5 X IO' - 3 x IO@ K PLASMA**

' Int. FWHM h ( R ) 0 class Idcntification 4" 40" 4" 40"

974.86 .06 997.1 .1 999.2 * .1

1005.7 .1 1010.2 .1 1118.07 .06 1136.61 .02 I1 1146.61 .02 II 1174.72# .05 >IV 1189.83 .01 IV 1190.07 .01 I11 1191.62 .02 111 1196.24 .01 V 1199.18 .01 I1 1212.96 .01 V 1213.90 .05 11+ 1216.43 .01 VI 1218.36 .02 11+ 1232.62 1242.00 1271.62 1277.23 1307.66 1322.2 # 1324.44 1331.62 1349.40 1361.92 1354.08 1359.06 1369.67 1368.83 1370.62 1375.96 1392.12 1397.22 1399.78 1401.17 1404.80

1406.06 1407.39 1408.66 1409.4s 1416.83 1423.89 1428.71

1440.60 .01 IV 1446.71 . .Ol IP 1460.49 .OS 1463.49 .01 V- 1467.06 .01 'V

i440.01# .oa

-02 v -01 VI- .02 >v .01 VI -02

.01 111

.03

.01 w-

.01

.05

.01

.'in v

.02 . >v

.02 >v

.03 VI

.01 VI

.02 I1

.01 11

.01 I1

.02 I1

.01 I1

.02 I1

.OS V

.01 v+ .01 .01 .01 >v

MnXII 3s23p2 MgV' 2s22p4

FeXn 3s23p3 FIW 2a22p2 FeXXI 2s22p1 F lW 2s22p2 MnXI 3s23p3

Ar XIIIt 2s22pl

0.24 2.5 1.9 .18

3.8 .18 0.75 .18 0.45 .I 7

18. 0.11 .24 .12 4.8 1.4 .26 .I7

6.0 5.8 36. '1.2 .22 .I5

0.29 .17 10.0 10.0 .19 .17

0.61 0.12 .21 .I8 0.03

0.02 0.01 0.09 .PO

5.1 6.7 .19 .17

0.06 -19 0.04 .17 0.04 .19 0.04 0.10 2 2

6.6 0.06 -23 -15

13. 0.18 .23 .15

2.0 0.02 2 3

28. 0.44 .23 .I5

6.0 0.03 .23 6.8 0.05 .23 0.28 0.07 .17 0.37 0.19 .I9 3.4 0.02 0.28 0.86 0.84 .21 .16

0.03 0.18 .22

1.1 3.70 .24 .22

2.3 0.72 .16 .I7 4.3 2.2 .17 .16

A(;) 0 CIasa lden tification Int. FWHM

4" 40" 4" 40"

1467.44 1486.52 1489.04 1510.51 1564.30 1574.9 1582.56 1601.5. .I 1603.21 1611.70 1614.51 1623.54 1639.78 1640.65 1660.81 1666.16 1666.95 1696.26 1715.44 1717.42 1746.81 1748.63 1749.67 1752.14 1753.98 1756.82 1757.64 1805.94 1826.21 1841.57 1847.25 1866.75 1892.03 1908.73 1917.21 191825 1984.88 2000.4 0 2042.35 2085.51 2125.50 2146.64 2149.26 2169.08 2184.26 2406.68 2497.5 2665.93 2670.14 2578.77 2622d6 2648.71

.03

.02

.03 V

.03 >V

.02 >v I11

.04 >V I1

.01 IV

.05 V

.03 VI

.04 IV-VI

.03 IV-VI

.03

.01 I

.01 I .01 .05 .01 IV+ .02 v .02 I .02 I .01 I .01 I .01 I .03 1- .03 I- .03 .02 VI .02 IV .02 VI .01 VI

1-

.02 IV

.01 v-

.02 1v+

.01 1v

.05 VI

.02 VI-

.04 111

.05 IV+

.02 VI-

.05 VI

.01 VI-

.oi I-

Ni XIV Si Ill c 111 Fe IX Fe Xt Si IX Ni X1 Fe IX Ni XV Ni XI11 Si VI1 Si IX Fe XI1 Ni XIV Fe XI1

' FelX .OB VI- FeXII .02 .01 VI FeXlII .os .02 V FeXI

11. 0.12 .23 .19 0.09 .20 0.04 0.05 0.05 0.36 .22

0.5 1.5 .34 0.4 0.26 .27 0.4 0.74 .26 0.4 0.25 1.0 0.68

0.21 16. .21 41. .21

0.08 .23 0.08

1.2 0.50 .26 0.1s .21

10. .23 4.4

18. 0.02 .23 2.7 5.4 .23

0.06 2.8 0.28 .21 .28

0.23 -27 1.7 0.20 .29 1.3 0.35 .29

440. 2.1 .08 71. 0.67 .I9

0.48 .28 2.7 1.1 .2,4 6.6 .38

12. .38 6.7 .40

12. .35 2.0 .36

11. .43 29. .33 14. .32

160. .37 -10.

43. .3B 28. .38

160. .40 19. .42 97. .38

Notes to Table I (3.fT c)

* Observed in the NRL rocket spectrum of 1966 July 27.

t Tentative identification.

k' Observed only in the 36-minute exposure of F igure 3.

6 Blended with Fe I1 2000.3 -&. Wavelengths above 2000 8, are i n air.

** Three flare l ines of higher temperature are included for completeness.

Ionization Class Log T e

I 4.7 - 5.0

I1

' I11

,'5.0 - 5.3 5.3 - 5.6

IV 5 . 6 - 5 . 9

V

VI

5 . 9 - 6.1

6 .1

The columns INT. and FWHM refer, respectively, t o observations . .

.above AR 121 14 at 4" above the limb, and above AR 12300 at 40" above

t h e limb.

. \ . .

19

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of - United States Navylouis14.nrl.navy.mil/skylab/spectral/skylab/docs/pdf/S082B_Manual.pdf4.0 5.0 6.0 7.0 Table of Contents ... and short-time roll stability was excellent. ... S052: