GOES fluence in 0.5-4 Å and 1 - 8 Å(1 min data)

GOES fluence in 0.5-4 Å and 1 - 8 Å(1 min data)

Areas in black correspond to times with the data

missing from telemetryor times when HV was OFF

(rad. belt passage)

PHA histogram for a given channel

Time runs horizontally,amplitude bin (0÷31)

vertically. Normalized to maximum in the dump

Channel descriptorCrystal & wavelength band

(software indexes used before 15 Nov. 2002 and

spectroscopic indexeslater on)

“Rubbish” side bins ‘0’ and ‘31’ containing the

signal from particlesmostly. Used in software

to detect rad. belt passage

High Voltage [V] setat the start of the sequence

Strong S XV He-like ion resonannce line at 5.04 Å

seen on the spectrum. λ runs vertically, time-hor.

Spacecraft night period.Orbital background seen

Rad. belt passagesHigh Voltage is OFF

Flare duration & position(from SOHO EIT)

Flare of X-ray class M6The rise phase is entirely

observed by RESIK, during about 30 min.

between auroral crossings

RESIK lightcurve plot (in black) description

Channel #2 (Ar XVII) denoted in ‘software’

notation as #0

Minimum DGI valuefor a given sequece [s]

Maximum DGI valuefor a given sequece [s]

Date of the data period shown.

Time [hours] elapsedfrom initial day start

Inclination Φ [deg]of the dispersion plane

for given day (large)and preceding & following

days (small)

Dump identification (the number of

orbit at which the data presented weresent to the ground)

PHA amplitude histogram(32 bins) for entire periodshown. The peak corre-

sponds to Si fluorescence

Summed spectrum in a given band.

All day & night periodsincluded

Spectra normalized to their maxima.

Orbital background is promptly removed.

Spectral variations seen represent

RELATIVE changes of intensity between lines,NOT the changes due to

solar flux level.

Example size of the Sunon the spectrum. Lines

may be displaced so much

S XV (w, x, y &z) tripletlines and satellites

Si XIII 1s2 - 1s3plines and satellites

S XVI 1s - 2p Lyαline and satellites

Possibly Si (solar induced)fluorescence emission

Solar peak in the range seen below

Only background signalseen on PHA during night

Ar XVII 1s2 - 1s2p wresonance line and satellites

Ar XVII 1s2 - 1s2p zforbidden line and satellites

Detector A ‘standard’HV setting 1480 V

Detector B ‘standard’HV setting 1419 V

‘Control’ Detector AHV readout 1480 V

with readout noise ±17 V

‘Control’ Detector BHV readout 1414 V

with readout noise ±10 V

Upper and bottom plot panels

Orbital position of the CORONAS at

each time

Orbital position of the CORONAS at

each time

Particle (protons) fromPIN detectors due to SAA

passage

Orbital position of the CORONAS at

each time

Orbital position of the CORONAS at

each time

Auroral regions crossings HV OFF due to high energy

electrons

Combined PHA signal in ‘rubbish’ bins, someflare response present.This levels are analysed

onboard in order todetermine rad-belt

intrusion

Earth map in projectionwhere eqal ate longitudezones crossed by S/C in

each DGI - funny

Levels corresponding toparticular GOES

X-ray flare classes, A, B...

ADS settings for aparticulare channel

Ar XVII 1s2 - 1s2ptriplet lines and the

correspondingsatellites

S XV 1s2 - 1s4pline and satellites

K XVIII 1s2 - 1s2ptriplet lines and the

correspondingsatellites

RESIK logonames of people canbe seen on zoomed

PostScript file

Dodac tu powiekszenie stopki logo !

Raw spectrum number for easyaccess from data

Orbit & particles‘electrons PHA’

Spectra normalized to maximum in each

channel 4.96 - 6.09

4.31 - 4.89 Å

3.37 - 3.88 Å

3.82 - 4.33 Å

GOES fluxes Flare positions & dispersion plane

Black - HV off

S/C nightsPHA

PHA

PHA

PHA

spectrum #1 4ADS = 96 - 165

spectrum #3 3ADS = 112 - 165

spectrum #0 2ADS = 80 - 165

spectrum #2 1ADS = 80 - 165

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