The Sun-Earth System is a The Sun-Earth System is a Complex Set of Interacting Physical Complex Set of Interacting Physical

Processes Processes

The Sun-Earth System is a The Sun-Earth System is a Complex Set of Interacting Physical Complex Set of Interacting Physical

Processes Processes

Large Scale FlowsLarge Scale FlowsLarge Scale FlowsLarge Scale Flows

ConvectionConvectionConvectionConvection

DynamoDynamoDynamoDynamoEmerging &Emerging &

Evolving Evolving Magnetic FieldsMagnetic Fields

Emerging &Emerging &Evolving Evolving

Magnetic FieldsMagnetic Fields

Spectral Spectral irradianceirradianceSpectral Spectral irradianceirradiance

EarthEarthDynamoDynamo

EarthEarthDynamoDynamo

Earth Earth RotationRotationEarth Earth

RotationRotation

MagnetosphereMagnetosphereMagnetosphereMagnetosphere

FlaresFlares

Coronal MassEjections

Coronal MassEjections

Solar WindSolar Wind

Coronal HeatingCoronal Heating

Interplanetary Interplanetary Energetic ParticlesEnergetic Particles

Interplanetary Interplanetary Energetic ParticlesEnergetic Particles

InterplanetaryInterplanetaryShocksShocks

InterplanetaryInterplanetaryShocksShocks

UltravioletUltravioletX-raysX-rays

UltravioletUltravioletX-raysX-rays

Heliospheric Heliospheric FieldsFields

Heliospheric Heliospheric FieldsFields

Cosmic RaysCosmic RaysCosmic RaysCosmic Rays

Radiation Radiation BeltsBelts

Radiation Radiation BeltsBelts

Density, Density, chemistrychemistry

Upper Atmos.Upper Atmos.

Density, Density, chemistrychemistry

Upper Atmos.Upper Atmos.

MagnetosphereMagnetosphereDynamicsDynamics

MagnetosphereMagnetosphereDynamicsDynamics

Ionosphere Ionosphere variabilityvariability

Ionosphere Ionosphere variabilityvariability

ClimateClimateClimateClimate

AstronautAstronautSafetySafety

AstronautAstronautSafetySafety

2

AIA and HMI Provide Data From the Interior to the Heliosphere

AIA and HMI Provide Data From the Interior to the Heliosphere

Tricolor:171 Å195 ÅYohkoh

3

AIA Science ObjectivesAIA Science Objectives

Energy input, storage, and releaseHow do quiesent and unstable magnetic structures evolve?

Coronal heating and irradiance

What are the physical properties of the irradiance modulating features?

Transients

How are particles accelerated?

Connections to geospaceWhat drives the solar wind and accelerates CME’s?

Coronal SeismologyWhat can waves reveal of the coronal densities, damping mechanisms, and magnetic fields?

Energy input, storage, and releaseHow do quiesent and unstable magnetic structures evolve?

Coronal heating and irradiance

What are the physical properties of the irradiance modulating features?

Transients

How are particles accelerated?

Connections to geospaceWhat drives the solar wind and accelerates CME’s?

Coronal SeismologyWhat can waves reveal of the coronal densities, damping mechanisms, and magnetic fields?

4

Investigation OverviewInvestigation Overview

The AIA investigation goal is to resolve fundamental observational ambiquities in coronal loop evolution that are caused by either density of temperature changes.

To achieve this AIA observes the coronal plasma with arc second spatial resolution, 10 second temporal resolution, over a wide and continuous temperature range.

The AIA investigation goal is to resolve fundamental observational ambiquities in coronal loop evolution that are caused by either density of temperature changes.

To achieve this AIA observes the coronal plasma with arc second spatial resolution, 10 second temporal resolution, over a wide and continuous temperature range.

5

Schematic Diagram of the AIA Investigation

Schematic Diagram of the AIA Investigation

ApertureSelector

PM +2M

Entrancefilters

FilterWheel

ShutterCCDSDO

MOC

DDS

JSOC

ScienceInvestigation

Computers Science team, Solar Physics Community, NASA, TaxpayersScience team, Solar Physics

Community, NASA, Taxpayers

6

Methods for Exploring the Outer Atmosphere

Methods for Exploring the Outer Atmosphere

Maps of the Surface Magnetic field

Maps of the Line of Sight Velocity fields

Maps of horizontal flows

Images formed at different temperaturesAtoms and Ions absorb and emitted light in discrete wavelength ranges

In order to create excited atoms and ions relatively well defined temperatures are required

Maps of the Surface Magnetic field

Maps of the Line of Sight Velocity fields

Maps of horizontal flows

Images formed at different temperaturesAtoms and Ions absorb and emitted light in discrete wavelength ranges

In order to create excited atoms and ions relatively well defined temperatures are required

7

Four Telescopes: Provides 41 arc minute FOV center on the Sun with 1.2 arc second spatial resolution.

Active Secondary Mirror and Guide Telescope: Stabilizes the image to better than 0.1 arc second for frequencies < 20 hz.

Normal Incidence EUV Mirors Optics: Isolates 6 to 10 Å spectral bands.

CCD Cameras: Produce solar images with 0.6 arc second pixels to critically sample the solar images.

Four Telescopes: Provides 41 arc minute FOV center on the Sun with 1.2 arc second spatial resolution.

Active Secondary Mirror and Guide Telescope: Stabilizes the image to better than 0.1 arc second for frequencies < 20 hz.

Normal Incidence EUV Mirors Optics: Isolates 6 to 10 Å spectral bands.

CCD Cameras: Produce solar images with 0.6 arc second pixels to critically sample the solar images.

Instrument Functional Components

Instrument Functional Components

8

AIA ImplementationAIA Implementation

Four telescopes, each with two wavelength channels and a guide telescope

Each telescope takes an image every 5 seconds (10 s of 8 λ’s)

Four telescopes, each with two wavelength channels and a guide telescope

Each telescope takes an image every 5 seconds (10 s of 8 λ’s)

304304

9393 171171 193193 133133

335335211211UVUV

He II

Fe XVIII

He II

Fe XVIII

UV

Fe IX

UV

Fe IX

Fe XIV

Fe XII/XXIV

Fe XIV

Fe XII/XXIV

Fe XVI

Fe XX/XXIII

Fe XVI

Fe XX/XXIII

9

AIA Field of ViewAIA Field of View

AIA will observe 96% of x-Ray radiance (based on Yohkoh data)

AIA will observe (~98%) of emission in EVE’s FOV

AIA will observe 96% of x-Ray radiance (based on Yohkoh data)

AIA will observe (~98%) of emission in EVE’s FOV

Composite Trace Image

41 arcmin

10

FOV extends to at least a pressure scale height (~.1R at T ~ 3MK)

FOV extends to at least a pressure scale height (~.1R at T ~ 3MK)ee

☉☉

Temperature CoverageTemperature Coverage

The set of Iron (Fe) lines selected minimize abundance effectsand give a broad spectral coverage. The Helium and Carbonlines extend temperature coverage to the Transition Region and Chromosphere.

The set of Iron (Fe) lines selected minimize abundance effectsand give a broad spectral coverage. The Helium and Carbonlines extend temperature coverage to the Transition Region and Chromosphere.

11

EUV Filter PropertiesEUV Filter Properties

Table FO2-2. AIA telescope coating and filter definitions. Only one telescope requires an aperture selector. Focal Plane Filters

Telescope λ Ion Rpeak Coating Materials

Entrance Filter 1Filter 2Filter

Aperture Selector

1

1600 1700 4500 171

C I /V continuum Continuum Continuum

Fe IX

80% 80% 80% 50%

Al Al Al /Mo Si

Bandpass on

MgF2 , 1500Al Å

Band pass on MgF2

Band pass on fused silica

Band pass on fused silica

, 1500Al Å

, 2500Al Å

No

2 94 304

Fe XVIII He II

40% 18%

/Ru Y /SiC Si

, 2000Zr Å , 1500Al Å

Zr, 2000Å , 1500Al Å

, 3000Zr Å , 2500Al Å No

3 133 335

/Fe XX XXIII Fe XVI

68% 17%

/Mo Si /SiC Si

, 2000Zr Å , 1500Al Å

, 2000Zr Å , 1500Al Å

Zr on Polyim *ide , 2500Al Å No

4 211 193

Fe XIV /Fe XII XXIV

42% 48%

/Mo Si /Mo Si

, 1500Al Å , 1500Al Å

, 1500Al Å , 1500Al Å

, Al 2500Å , 2500Al Å Yes

*3000 4000 Å Zr on Å Polyimide can be used as a neutral density filter during flares SDO_0023

Table FO2-2. AIA telescope coating and filter definitions. Only one telescope requires an aperture selector. Focal Plane Filters

Telescope λ Ion Rpeak Coating Materials

Entrance Filter 1Filter 2Filter

Aperture Selector

1

1600 1700 4500 171

C I /V continuum Continuum Continuum

Fe IX

80% 80% 80% 50%

Al Al Al /Mo Si

Bandpass on

MgF2 , 1500Al Å

Band pass on MgF2

Band pass on fused silica

Band pass on fused silica

, 1500Al Å

, 2500Al Å

No

2 94 304

Fe XVIII He II

40% 18%

/Ru Y /SiC Si

, 2000Zr Å , 1500Al Å

Zr, 2000Å , 1500Al Å

, 3000Zr Å , 2500Al Å No

3 133 335

/Fe XX XXIII Fe XVI

68% 17%

/Mo Si /SiC Si

, 2000Zr Å , 1500Al Å

, 2000Zr Å , 1500Al Å

Zr on Polyim *ide , 2500Al Å No

4 211 193

Fe XIV /Fe XII XXIV

42% 48%

/Mo Si /Mo Si

, 1500Al Å , 1500Al Å

, 1500Al Å , 1500Al Å

, Al 2500Å , 2500Al Å Yes

*3000 4000 Å Zr on Å Polyimide can be used as a neutral density filter during flares SDO_0023

0.001

0.010

10.000

100 150 200 250Wavelength (Å)

1.000

0.100

300 350

171193211335

94133304

0.1

1.0

10.0

10000.0

4.5 5.0 5.5 6.0 6.5log T (K)

1000.0

100.0

7.0 7.5

171193211335

94133

Effective AreasEffective Areas Predicted Response FunctionsPredicted Response Functions

12

AIA Exposure EstimatesAIA Exposure Estimates

Predicted EUV Countrates Photons per pixel per 2.7s exposure, or time to full well (<…>)

Channel Quiet Sun Active Region M flare Microflare

94 Å 35 <0.1s> 170 131Å 22 240 <2.8ms> 3,400 171Å 1,100 <2.1s> <57ms> <0.19s> 193Å 810 <1.6s> <7.1ms> <0.3s> 211Å 250 6,600 <74ms> <1.1s> 304Å 2,500 8,100 <10ms> 335Å 61 2.700 <97ms> 5,200

Assumes thin filter wheel filters From CSR, Appendix A

These estimates provides a dynamic range of 8 in quiet and 20 in active Sun.

These estimates provides a dynamic range of 8 in quiet and 20 in active Sun.

13

AIA Optics Package on SDOAIA Optics Package on SDO

14

Single TelescopeSingle Telescope

Aperture Door

Science Telescope (ST)

GT Pre-Amp

Vent

Guide Telescope (GT)

Camera Electronics Box (CEB)

CEB RadiatorCCD Radiator

PZT straingauge pre-amp

15

AIA Telescope PhantomAIA Telescope Phantom

Secondary BaffleSecondary Baffle

Primary MirrorAssembly

Primary MirrorAssembly

Primary BafflePrimary Baffle

Spider InterfaceSpider Interface

Filter FrameFilter Frame

Primary Secondary Separation 975 mm

Primary Focal Length 1375 mm

Back focalposition 225 mm Secondary Focal Length

604 mm

16

Optical LayoutOptical Layout

Secondary MirrorSecondary Mirror

Wavelength SelectorWavelength Selector

Entrance FilterEntrance Filter

Focus MotorFocus Motor

Image Stabilization SystemImage Stabilization System

Primary MirrorPrimary Mirror

Shutter Shutter

CCDCCD

Filter WheelFilter Wheel

17

Cross Section of TelescopeCross Section of Telescope

Filterwheelassembly

Fiberglassisolator tubeCCD

header

CCDheaters

CCDdetector

Radiationshield/

cold trapShutter

assemblyPrimarymirror

Secondarymirror PZT Active mirror

assemblySpiderframe

Apertureselectormotor

Aperturedoor

Apertureselectorblade

Entrancefilter frame

Rocker arm

Focus motor(behind spider

arm)

Baffletubes

Graphite epoxymetering tube

1341 mm

319 mm 244 mm

18

Telescope MechanismsTelescope Mechanisms

Aperture Selector(one telescope only)

Focus Mechanism

Shutter

Filterwheel

Light from Sun

CCD

19

AIA-TelescopeAIA-TelescopeGuide Telescope (GT)Guide Telescope (GT)

Front ApertureAssembly (FPA)Front Aperture

Assembly (FPA)Telescope TubeTelescope Tube

Camera Electronics Box (CEB)

Camera Electronics Box (CEB)

Focal PlaneAssembly (FPA)

Focal PlaneAssembly (FPA)Focus MechanismFocus Mechanism

Front DoorFront Door

20

Flight Telescope TubeFlight Telescope Tube

21

Optical ParametersOptical Parameters

ParameterParameter mmmmMirror separation 975

Back focal distance 230

Pupil OD 188

Pupil ID 90.2

Beam diameter secondary 68

Beam diameter primary 188

Primary mirror OD 200

Primary mirror ID 65

Primary mirror radius -2755.0

Primary mirror conic constant (concave) -1.0916

Secondary mirror OD 79.8

Secondary mirror radius (convex) 1208.57

Secondary mirror conic constant -5.077

22

Image Stabilization SystemImage Stabilization System

GT analog signals are used by the ISS of the associated Science Telescope

Photo diodes and preamp circuits are redundant

Secondary is moved by three PZT’s

Error signal provided by GT

GT analog signals are used by the ISS of the associated Science Telescope

Photo diodes and preamp circuits are redundant

Secondary is moved by three PZT’s

Error signal provided by GT

PZT’sPZT’s

23

Flight Spider AssemblyFlight Spider Assembly

24

Guide TelescopesGuide TelescopesAIA has four identical Guide Telescopes

Noise equivalent angle of 0.6 arc second

Linear signal range ± 95 arc seconds

AIA has four identical Guide Telescopes

Noise equivalent angle of 0.6 arc second

Linear signal range ± 95 arc seconds

25

E2V Packaged CCDE2V Packaged CCD

AIA Thinned Front Illuminated 4096

AIA Thinned Front Illuminated 4096 22

Probe Image Room Temperature

Probe Image Room Temperature

26

Normal OperationsNormal Operations

A regular cadence of 10 seconds for 8 wavelengths allows observations of most phenomena, guaranteed coverage, and standardized software. It also has the advantage of being compatible with the HMI and EVE science needs.

A regular cadence of 10 seconds for 8 wavelengths allows observations of most phenomena, guaranteed coverage, and standardized software. It also has the advantage of being compatible with the HMI and EVE science needs.

131 Fe XX94 Fe XVII131 Fe XX94 Fe XVII

0s0s 10s10s 20s20s 30s30s 40s40s 50s50s 60s60s

335 Fe XVI211 Fe XIV335 Fe XVI211 Fe XIV

193 Fe XII304 He II

193 Fe XII304 He II1600 CIV1700 UVC4500 WL

1600 CIV1700 UVC4500 WL

27

Special OperationsSpecial Operations

Fast reconnection, flares, filament eruptions, and high frequency wave require a higher cadence. Partial readouts in a limited set of wavelenghts embedded in a slowed baseline program that is infrequently used, will broaden discovery potential without adverse effects on the overall mission goals.

Fast reconnection, flares, filament eruptions, and high frequency wave require a higher cadence. Partial readouts in a limited set of wavelenghts embedded in a slowed baseline program that is infrequently used, will broaden discovery potential without adverse effects on the overall mission goals.

131 Fe XX94 Fe XVII131 Fe XX94 Fe XVII

0s0s 10s10s 20s20s 30s30s 40s40s 50s50s 60s60s

335 Fe XVI211 Fe XIV335 Fe XVI211 Fe XIV

193 Fe XII304 He II

193 Fe XII304 He II1600 CIV1700 UVC4500 WL

1600 CIV1700 UVC4500 WL

70s70s 80s80s 90s90s

28

Science Coordination is an Essential Part of the SDO Mission

Science Coordination is an Essential Part of the SDO Mission

AIA/AIA/HMI/EVEHMI/EVE GONG+GONG+

++

Ground Ground TelecopTelecop

eses

FPPFPP FppFpp

STERESTEREOO

WAVESWAVESACEACE

SOLISSOLIS

GOESGOES

XRTXRT EISEIS

RHESSRHESSII

FASRFASR

HiRes Vector Fields Soft x-Ray Images EUV Spectra

Coronal Images Chromospheric Images

x-Ray Images Gamma Ray Images Radio Images

HiRes Spectra & Images

HiRes Spectra & Images

Dopplergrams & Magnetograms

Dopplergrams & Magnetograms

SOHOSOHOMMSMMS

Coronal Images

Radio ImagesRadio ImagesMagnetosphere

Energetic Particles

29

Instrument Capabilities in Space and Time

Instrument Capabilities in Space and Time

Spatial range (arcsec)

STEREO SECCHI

1 10 100 1000

SOLAR B XRT

Solar Diameter

Granulation

Chromospheric Thickness

Moss Layer

Sunspot Diameter

FilamentsCMEs

AIA

TRACE

Temperature Coverage (MK)

12 8 0.9

40,000 K 0.1

1.2

3 4

2 4000 K

AR Loop Length0.10.1

11

1010

0.10.1

PorePore

SOHO/EITSOHO/EIT

30

Joint Science Operations StructureJoint Science Operations Structure

Catalog

PrimaryArchive

HMI & AIAOperations

House-keeping

Database

MOCDDS

RedundantData

CaptureSystem

30-DayArchive

OffsiteArchive

OfflineArchive

HMI-AIA JSOC PipelineProcessing System

DataExport& WebService

Stanford

LMSAL

High-LevelData Import

AIAAnalysisSystem

LocalArchive

QuicklookViewing

GSFCWhite Sands

World

Science TeamForecast Centers

EPOPublic

31

AIA Data FlowAIA Data Flow

Data ProductsLow-Resolution (10242)

Summary Movies

Full-ResolutionAR Extract Movies

Full-Resolution ExtractEvent/Feature Movies

Irradiance Curves

CoronalField-Line Models

ReconstructedTemperature Maps

Level1a

Level2

On-Line CatalogsCatalog of

Events/Features

Catalog ofDescriptive Entries

Catalog ofDaily Summaries

AIA Level 0 Archive

HMI Magnetograms(from HMI pipeline)

Loop Outlines

Field LineExtrapolation

Web Services“The Sun Today”

Web Service

User Requests

VisualizationCenter

EventDetection

FeatureRecognition

LoopTracing

DEMInversion

MovieMaker

IrradianceMonitoring

Incoming AIA Data(from HMI pipeline)

TempSeq

TempSeq

32

AIA Data Flow MapAIA Data Flow Map

Quick Look Movies(Level 1a)Browser CatalogIndexCalibrated Selected Regions (Level 1a)Calibrated Level 0 (Level 1)Temperature Maps (Level 2)Field Line Models (Level 2)1.18 Tb/Day

Quick Look MoviesBrowser CatalogIndex

1.1 Tb/ Day

On-LineSurvey Data for PublicOutreach, SomeForecasting

Total Cache 100 TB

Data from Stanford PipelineAIA Level 0 decompressed imagesHMI Level 1a Magnetograms

AIA Level 0 +HMI Magnetograms Archive / Backup

1.4 Tb / Day, Life

Basic Data for Science Analysis

Near Real time Tape

AIA Science Data Production

Public & UserCommunityOpen WebConnection

SDO Science TeamControlled Web

Connection

1.1 Tb/ Day

AIA Level 0 +HMI Magnetograms

33