1. 8:30-9:10 AM: Philip Scherrer, What Can We Hope to Learn from SDO Overview of SDO HMI Investigation HMI Instrument

2. MDI Status Excellent Condition Half Way

8. Solar-Heliospheric Activity Research and Prediction Program

11. SDO EVE Science Overview The EVE program has 4 primary science objectives. 1.Advance current understanding of how and why the solar EUV spectral irradiance varies 2.Specify the solar EUV spectral irradiance and its variability on multiple time scales 3.Improve the capability to predict the EUV spectral irradiance variability 4.Understand the response of the geospace environment to variations in the solar EUV spectral irradiance and the impact on human endeavors

13. SDO-EVE MEGS - Multiple Euv Grating Spectrograph ESP - Euv SpectrophotometerOFS - Optics Free Spectrometer

17. The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study the origin of solar variability and to characterize and understand the Sun’s interior and the various components of magnetic activity. The HMI investigation is based on measurements obtained with the HMI instrument as part of the Solar Dynamics Observatory (SDO) mission. HMI makes measurements of the motion of the solar photosphere to study solar oscillations and measurements of the polarization in a spectral line to study all three components of the photospheric magnetic field.

18. HMI produces data to determine the interior sources and mechanisms of solar variability and how the physical processes inside the Sun are related to surface magnetic field and activity. It also produces data to enable estimates of the coronal magnetic field for studies of variability in the extended solar atmosphere. HMI observations will enable establishing the relationships between the internal dynamics and magnetic activity in order to understand solar variability and its effects, leading to reliable predictive capability, one of the key elements of the Living With a Star (LWS) program.

19. The broad goals described above will be addressed in a coordinated investigation in a number of parallel studies. These segments of the HMI investigation are to observe and understand these interlinked processes: Convection-zone dynamics and the solar dynamo; Origin and evolution of sunspots, active regions and complexes of activity; Sources and drivers of solar activity and disturbances; Links between the internal processes and dynamics of the corona and heliosphere; Precursors of solar disturbances for space-weather forecasts. These goals address long-standing problems that can be studied by a number of immediate tasks. The description of these tasks reflects our current level of understanding and will obviously evolve in the course of the investigation.

20. HMI Major Science Objectives B – Solar Dynamo C – Global Circulation D – Irradiance Sources H – Far-side Imaging F – Solar Subsurface Weather E – Coronal Magnetic Field I – Magnetic Connectivity J – Sunspot Dynamics G – Magnetic Stresses A – Interior Structure NOAA 9393 Far-side

24. The HMI instrument will produce filtergrams in a set of polarizations and spectral line positions at a regular cadence for the duration of the mission. These are combined on the ground to produce: 1-arc-second resolution full-disk Doppler velocity and line-of-sight magnetic flux images at least every 50 seconds 1-arc-second resolution full-disk vector-magnetic images of the longitudinal solar magnetic field at least every 90 seconds

28. FeI 6173Å instead of NiI 6768Å

29. HMI Filter Profiles

30. HMI Observing Sequence

31. Sample MDI Filtergrams

32. Sample MDI Observables

33. The HMI investigation will provide sufficient computing capability to convert these raw filtergram measurements into a set of observables and derived data products that satisfy the HMI science objectives The primary observables (Dopplergrams, longitudinal and vector magnetograms, and continuum intensity images) will be available at full resolution and cadence. Other derived products such as subsurface flow maps, far side activity maps, and coronal and solar wind models that require longer sequences of observations will be produced. Open data policy: ALL data products will be freely available as soon as they are created.

34. Lev.DescriptionExamples Rate [GB/day] Rate [TB/yr] Cache [day] Archived [%] RawTelemetry- 60020030100 0Filtergrams- 1000400100 1Observables V LOS, B LOS, I c, Vector Field Parameters 40016060030 2 Reorganized data Spatial/temporal Samples, Averages; Synoptic Maps 1033000100 3Inferences Global Modes, Analysis Maps, Farside Images, Coronal Fields <1 2000100 HMI Data Archive

35. Online Data Telemetry Net Access Ops Analysis Archive Telem Archive HMI SDO 30d cache ReOrg Data Data CaptureLev 1Inferences 600100040010 HMI Dataflow Concept (Gigabytes/day) 0.02 30d Cache <1

37. HMI Education/Public Outreach Partnerships InstitutionStudent Involve ment K-14 Curric- ulum Develop ment Teacher Work- shops Assess ment Support Multi- media Develop ment Distance Learning Support Distri- bution of Materials Access to Under- served Public/ infomal education StanfordXXXXXXXXX LMSALXXXXXX Stanford-HaasXXXXX The Tech MuseumXXXXX Chabot SSCXXXXX Morrison Planetarium /CA Academy of Sciences XXXX Lawrence Hall of Science XXXXX IIISEXX NASA-COREX

38. First HMI Science Team meeting in spring 2003

39. For continuing HMI information see: http://hmi.stanford.edu