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