1. The Atmospheric Imaging Assembly Measuring the Sun’s Surface, Chomosphere, Transition Region, and Corona using visible and extreme Ultra- violet light.

2. The Sun-Earth System is a Complex Set of Interacting Physical Processes The Sun-Earth System is a Complex Set of Interacting Physical Processes Large Scale Flows ConvectionConvection DynamoDynamo Emerging & Evolving Magnetic Fields Emerging & Evolving Magnetic Fields SpectralirradianceSpectralirradiance EarthDynamoEarthDynamoEarthRotationEarthRotation MagnetosphereMagnetosphere Flares Coronal Mass Ejections Coronal Mass Ejections Solar Wind Coronal Heating Interplanetary Energetic Particles Interplanetary InterplanetaryShocksInterplanetaryShocks UltravioletX-raysUltravioletX-rays HeliosphericFieldsHeliosphericFields Cosmic Rays RadiationBeltsRadiationBeltsDensity,chemistry Upper Atmos. Density,chemistry MagnetosphereDynamicsMagnetosphereDynamics IonospherevariabilityIonospherevariability ClimateClimateAstronautSafetyAstronautSafety 2

3. AIA and HMI Provide Data From the Interior to the Heliosphere 3

4. AIA Science Objectives Energy input, storage, and release How 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 geospace What drives the solar wind and accelerates CME’s? Coronal Seismology What can waves reveal of the coronal densities, damping mechanisms, and magnetic fields? Energy input, storage, and release How 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 geospace What drives the solar wind and accelerates CME’s? Coronal Seismology What can waves reveal of the coronal densities, damping mechanisms, and magnetic fields? 4

5. Investigation 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

6. Schematic Diagram of the AIA Investigation Science team, Solar Physics Community, NASA, Taxpayers 6

7. 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 temperatures Atoms 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 temperatures Atoms 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

8. 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 8

9. AIA 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) 304 93 171 193 133 335 211 UV 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

10. AIA 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 10 FOV extends to at least a pressure scale height (~.1R at T ~ 3MK) e e ☉ ☉

11. Temperature Coverage The set of Iron (Fe) lines selected minimize abundance effects and give a broad spectral coverage. The Helium and Carbon lines extend temperature coverage to the Transition Region and Chromosphere. The set of Iron (Fe) lines selected minimize abundance effects and give a broad spectral coverage. The Helium and Carbon lines extend temperature coverage to the Transition Region and Chromosphere. 11

12. EUV Filter Properties Effective Areas Predicted Response Functions 12

13. AIA Exposure Estimates These estimates provides a dynamic range of 8 in quiet and 20 in active Sun. 13

14. AIA Optics Package on SDO 14

15. Single Telescope 15

16. AIA Telescope Phantom Secondary Baffle Primary Mirror Assembly Primary Mirror Assembly Primary Baffle Spider Interface Filter Frame 16

17. Optical Layout Secondary Mirror Wavelength Selector Entrance Filter Focus Motor Image Stabilization System Primary Mirror Shutter CCD Filter Wheel 17

18. Cross Section of Telescope 18

19. Telescope Mechanisms 19

20. AIA-Telescope Guide Telescope (GT) Front Aperture Assembly (FPA) Front Aperture Assembly (FPA) Telescope Tube Camera Electronics Box (CEB) Camera Electronics Box (CEB) Focal Plane Assembly (FPA ) Focal Plane Assembly (FPA ) Focus Mechanism Front Door 20

21. Flight Telescope Tube 21

22. Optical Parameters Parametermm Mirror separation975 Back focal distance230 Pupil OD188 Pupil ID90.2 Beam diameter secondary68 Beam diameter primary188 Primary mirror OD200 Primary mirror ID65 Primary mirror radius-2755.0 Primary mirror conic constant (concave)-1.0916 Secondary mirror OD79.8 Secondary mirror radius (convex)1208.57 Secondary mirror conic constant-5.077 22

23. Image 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’s 23

24. Flight Spider Assembly 24

25. Guide Telescopes AIA 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

26. E2V Packaged CCD AIA Thinned Front Illuminated 4096 2 2 Probe Image Room Temperature Probe Image Room Temperature 26

27. Normal 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. 131 Fe XX 94 Fe XVI I 131 Fe XX 94 Fe XVI I 0s 10s 20s 30s 40s 50s 60s 335 Fe XVI 211 Fe XIV 335 Fe XVI 211 Fe XIV 193 Fe XII 304 He II 193 Fe XII 304 He II 1600 CIV 1700 UVC 4500 WL 1600 CIV 1700 UVC 4500 WL 27

28. Special 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. 131 Fe XX 94 Fe XVI I 131 Fe XX 94 Fe XVI I 0s 10s 20s 30s 40s 50s 60s 335 Fe XVI 211 Fe XIV 335 Fe XVI 211 Fe XIV 193 Fe XII 304 He II 193 Fe XII 304 He II 1600 CIV 1700 UVC 4500 WL 1600 CIV 1700 UVC 4500 WL 70s 80s 90s 28

29. Science Coordination is an Essential Part of the SDO Mission AIA/HMI/ EVE GONG+ + Ground Telecope s FPP Fpp Fpp STERE O WAVESACESOLIS GOES XRTEIS RHES SI FASR HiRes Vector Fields Soft x-Ray Images EUV Spectra Coronal ImagesChromospheric Images x-Ray ImagesGamma Ray ImagesRadio Images HiRes Spectra & Images Dopplergrams & Magnetograms Dopplergrams & Magnetograms SOHOMMS Coronal Images Radio Images Magnetosphere Energetic Particles 29

30. Instrument Capabilities in Space and Time 0.1 1 1 10 0.1 Pore SOHO/EIT 30

31. Joint Science Operations Structure 31

32. AIA Data Flow Temp Seq Temp Seq 32

33. AIA Data Flow Map 33