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

1. Flares Large Scale Flows Interplanetary Energetic Particles Earth Dynamo Radiation Belts Astronaut Safety Coronal Mass Ejections Ultraviolet X-rays Magnetosphere Magnetosphere Dynamics Emerging & Evolving Magnetic Fields Dynamo Earth Rotation Heliospheric Fields Ionosphere variability Coronal Heating Solar Wind Density, chemistry Upper Atmos. Interplanetary Shocks Convection Spectral irradiance Climate Cosmic Rays The Sun-Earth System is a Complex Set of Interacting Physical Processes 2

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

3. 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? 4

4. 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. 5

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

6. 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 7

7. Instrument Functional Components • 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. 8

8. 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) 211 335 304 UV 93 171 193 133 He II Fe XVIII UV Fe IX Fe XIV Fe XII/XXIV Fe XVI Fe XX/XXIII 9

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

10. 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. 11

11. EUV Filter Properties Effective Areas Predicted Response Functions 12

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

13. AIA Optics Package on SDO 14

14. Single Telescope 15

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

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

17. Cross Section of Telescope 18

18. Telescope Mechanisms 19

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

20. Flight Telescope Tube 21

21. Optical Parameters 22

22. 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 PZT’s 23

23. Flight Spider Assembly 24

24. Guide Telescopes • AIA has four identical Guide Telescopes • Noise equivalent angle of 0.6 arc second • Linear signal range ± 95 arc seconds 25

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

26. 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. 0s 10s 20s 30s 40s 50s 60s 131 Fe XX 94 Fe XVII 335 Fe XVI 211 Fe XIV 193 Fe XII 304 He II 1600 CIV 1700 UVC 4500 WL 27

27. 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. 0s 10s 20s 30s 40s 50s 60s 70s 80s 90s 131 Fe XX 94 Fe XVII 335 Fe XVI 211 Fe XIV 193 Fe XII 304 He II 1600 CIV 1700 UVC 4500 WL 28

28. Science Coordination is an Essential Part of the SDO Mission Soft x-Ray Images EUV Spectra HiRes Vector Fields FPP Fpp XRT EIS Dopplergrams & Magnetograms HiRes Spectra & Images AIA/HMI/EVE Ground Telecopes GONG++ Coronal Images Energetic Particles Chromospheric Images STEREO WAVES ACE SOLIS x-Ray Images Gamma Ray Images Radio Images GOES MMS RHESSI SOHO FASR Coronal Images Magnetosphere 29 Radio Images Radio Images

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

30. Joint Science Operations Structure 31

31. AIA Data Flow Temp Seq 32

32. AIA Data Flow Map 33