Helioseismic and Magnetic Imager hmi.stanford

1. Helioseismic and Magnetic Imagerhttp://hmi.stanford.edu LWS-SDO Workshop 23-26 March 2004 • Philip Scherrer • pscherrer@solar.stanford.edu

2. HMI Investigation Overview • Investigation Overview • Science Objectives • Data Products and Objectives • Data Product Examples • Science Team and Institutional Roles • HMI Instrument • HMI-AIA Joint SOC • HMI EPO

3. Investigation Overview - 1 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.

4. Investigation Overview - 2 The basic HMI measurements must be processed into higher level data products before analysis can proceed HMI produces data products suitable 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 products to enable model estimates of the low and far coronal magnetic field for studies of variability in the extended solar atmosphere.

5. Investigation Overview - 3 The production of HMI high level data products and analysis of HMI data requires the participation of the HMI Team with active collaboration with other SDO instrument teams and the LWS community. HMI observations will enable establishing the relationships between the internal dynamics and magnetic activity in order to understand solar variability and its effects. This is a prerequisite to understanding possible solar activity predictability. HMI data and results will be made available to the scientific community and the public at large through data export, publications, and an Education and Public Outreach program.

6. HMI Science Objectives – Top Level • HMI science objectives are grouped into five broad categories: • Convection-zone dynamics and the solar dynamo; • How does the solar cycle work? • Origin and evolution of sunspots, active regions and complexes of activity; • What drives the evolution of spots and active regions? • Sources and drivers of solar activity and disturbances; • How and why is magnetic complexity expressed as activity? • Links between the internal processes and dynamics of the corona and • heliosphere; • What are the large scale links between the important domains? • Precursors of solar disturbances for space-weather forecasts. • What are the prospects for predictions? • These objectives are divided into 18 sub-objectives each of which needs data from multiple HMI data products. • Progress will require a science team with experience in multiple disciplines.

7. HMI Science Objectives • Convection-zone dynamics and the solar dynamo • Structure and dynamics of the tachocline • Variations in differential rotation • Evolution of meridional circulation • Dynamics in the near surface shear layer • Origin and evolution of sunspots, active regions and complexes of activity • Formation and deep structure of magnetic complexes of activity • Active region source and evolution • Magnetic flux concentration in sunspots • Sources and mechanisms of solar irradiance variations • Sources and drivers of solar activity and disturbances • Origin and dynamics of magnetic sheared structures and d-type sunspots • Magnetic configuration and mechanisms of solar flares • Emergence of magnetic flux and solar transient events • Evolution of small-scale structures and magnetic carpet • Links between the internal processes and dynamics of the corona and heliosphere • Complexity and energetics of the solar corona • Large-scale coronal field estimates • Coronal magnetic structure and solar wind • Precursors of solar disturbances for space-weather forecasts • Far-side imaging and activity index • Predicting emergence of active regions by helioseismic imaging • Determination of magnetic cloud Bs events

8. Internal rotation Ω(r,Θ) (0<r<R) Global Helioseismology Processing Tachocline Meridional Circulation Internal sound speed, cs(r,Θ) (0<r<R) HMI Data Processing Data Product Science Objective Differential Rotation Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Near-Surface Shear Layer Local Helioseismology Processing Filtergrams Activity Complexes Carrington synoptic v and cs maps (0-30Mm) Active Regions Sunspots High-resolution v and cs maps (0-30Mm) Irradiance Variations Doppler Velocity Magnetic Shear Deep-focus v and cs maps (0-200Mm) Observables Flare Magnetic Config. Far-side activity index Flux Emergence Line-of-sight Magnetograms Magnetic Carpet Line-of-Sight Magnetic Field Maps Coronal energetics Vector Magnetograms Vector Magnetic Field Maps Large-scale Coronal Fields Solar Wind Coronal magnetic Field Extrapolations Continuum Brightness Far-side Activity Evolution Predicting A-R Emergence Coronal and Solar wind models IMF Bs Events Brightness Images HMI Data Products and Objectives Version 1.0

9. B – Rotation Variations J – Subsurface flows C – Global Circulation I – Magnetic Connectivity A – Interior Structure D – Irradiance Sources E – Coronal Magnetic Field H – Far-side Imaging F – Solar Subsurface Weather G – Magnetic Fields HMI Data Product Examples • Sound speed variations relative to a standard solar model. • Solar cycle variations in the sub-photospheric rotation rate. • Solar meridional circulation and differential rotation. • Sunspots and plage contribute to solar irradiance variation. • MHD model of the magnetic structure of the corona. • Synoptic map of the subsurface flows at a depth of 7 Mm. • EIT image and magnetic field lines computed from the photospheric field. • Active regions on the far side of the sun detected with helioseismology. • Vector field image showing the magnetic connectivity in sunspots. • Sound speed variations and flows in an emerging active region.

10. 7 Sun dynamo 6 polar field Rings Global HS Zonal flow 5 AR Time-Distance P-modes spot Earth SG 4 granule 3 Log Size (km) HMI resolution 2 7 1 2 3 6 4 5 8 9 10 min day year hour 5min cycle Log Time (s) Solar Domain of HMI Helioseismology rotation

11. 7 Coronal field estimates Sun dynamo 6 polar field Large-Scale 5 Vector AR P-modes spot Earth SG 4 Line-of-sight granule 3 Log Size (km) HMI resolution 2 7 1 2 3 6 4 5 8 9 10 min day year hour 5min cycle rotation Log Time (s) Solar Domain of HMI Magnetic Field

12. HMI Co-Investigator Science Team-1

13. HMI Co-Investigator Science Team-2

14. HMI Institutional Roles LWS Science SDO Science HMI Instrument HMI Science Team HMI-AIA JSOC Stanford HMI E/PO LMSAL

15. Science Team Local Helioseismology - Alexander Kosovichev Global Helioseismology - Jesper Schou Magnetic Fields - Yang Liu HAO Vector Fields team Co-I Science Team HMI Team Organization Philip Scherrer HMI Principal Investigator Alan Title HMI-LMSAL Lead Jesper Schou Instrument Scientist Rock Bush HMI-Stanford Prg. Mgr. Larry Springer LMSAL SDO Prg. Mgr. Romeo Durscher HMI Admin Deborah Scherrer Educ. & Public Outreach Barbara Fischer HMI Deputy Prg. Mgr. Rick Bogart Data Export Rasmus Larsen Processing & Analysis Jim Aloise Ground System Keh-Cheng Chu Ground Sys Hardware Edgar Thomas Camera Electronics Dexter Duncan CCDs John Miles System Engineering Rose Navarro Thermal Mike Levay Integration & Test Russ Lindgren Electrical Lead Glenn Gradwohl Mechanical Lead Dave Akin Mechanism Lead Rick RairdenOptical Elements Jerry Drake Inst. Software Lead

16. Science Team Coordination • Team meetings: May 2003, Mag splinter Oct 2003 • Next HMI (+AIA?) September 2004 • Leads for Planning • Local Helioseismology Sasha Kosovichev • Global Helioseismology Jesper Schou • Modeling & Inversions Sasha Kosovichev • Mag Field large & small Yang Liu • Vector Field Inversions Steve Tomczyk • Continuum studies Rock Bush • Space Weather Coord. Yang Liu

17. X Y HOP Z HEB HMI S/C Accommodations

18. Instrument Overview – Optical Path Optical Characteristics: Focal Length: 495 cm Focal Ration: f/35.2 Final Image Scale: 24m/arc-sec Re-imaging Lens Magnification: 2 Focus Adjustment Range: 16 steps of 0.4 mm Filter Characteristics: Central Wave Length: 613.7 nm Reject 99% Solar Heat Load Bandwidth: 0.0076 nm Tunable Range: 0.05 nm Free Spectral Range: 0.0688 nm

19. HMI Optics Package (HOP) Connector Panel Z Focal Plane B/S Fold Mirror Shutters Alignment Mech X Limb Sensor Y Oven Structure Detector (Vector) Michelson Interf. Lyot Filter CEBs Detector (Doppler) Vents Limb B/S Front Window Active Mirror Polarization Selector Focus/Calibration Wheels OP Structure Mechanical Characteristics: Box: 0.84 x 0.55 x 0.16 m Over All: 1.19 x 0.83 x 0.29 m Mass: 39.25 kg First Mode: 63 Hz Telescope Support Legs (6) Front Door

20. HMI Requirements - Driving

21. Z Y X HMI Overview – HEB Key Features • Power all HMI sub-systems • Processing for decoding and execution of commands and acquiring and formatting of housekeeping telemetry • Contains: • Processor Board (2) • PCI to Local Bus Bridge and 1553 Interface board (2) • Mechanism and Heater Controller Board (4) • Housekeeping Data Acquisition Board (2?) • CCD Camera Interface Board (2) • Data Compressor/High Rate Interface Board (2) • ISS Limb Tracker Board • ISS PZT Driver Board • Power Converter Subsystem with redundant power converters • HEB dimensions: 254 X 424 X 320 mm, Mass 19.3 kg • Oven Controller and Limb Sensor Pre-Amp are in HOP Data Section Power Section

22. GSFC LMSAL White Sands housekeeping MOC House- keeping Database DDS HMI & AIA Operations Stanford HMI JSOC Pipeline Processing System Redundant Data Capture System Quicklook Viewing Primary Archive 30-Day Archive LM-Local Archive AIA Analysis System Catalog High-Level Data Import Offline Archive Data Export & Web Service World Offsite Archive HMI & AIA JSOC Architecture Science Team Forecast Centers EPO Public

23. Internal rotation Ω(r,Θ) (0<r<R) Processing Data Product Internal sound speed, cs(r,Θ) (0<r<R) HMI Data Spherical Harmonic Time series To l=1000 Heliographic Doppler velocity maps Filtergrams Mode frequencies And splitting Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Carrington synoptic v and cs maps (0-30Mm) Local wave frequency shifts Ring diagrams Doppler Velocity High-resolution v and cs maps (0-30Mm) Time-distance Cross-covariance function Tracked Tiles Of Dopplergrams Wave travel times Deep-focus v and cs maps (0-200Mm) Egression and Ingression maps Wave phase shift maps Far-side activity index Stokes I,V Line-of-sight Magnetograms Line-of-Sight Magnetic Field Maps Stokes I,Q,U,V Full-disk 10-min Averaged maps Vector Magnetograms Fast algorithm Vector Magnetic Field Maps Coronal magnetic Field Extrapolations Vector Magnetograms Inversion algorithm Tracked Tiles Tracked full-disk 1-hour averaged Continuum maps Coronal and Solar wind models Continuum Brightness Solar limb parameters Brightness feature maps Brightness Images HMI Data Analysis Pipeline HMI - SOC Pipeline Level-0 Level-1

24. HMI - SOC Processing and Data Flow LMSAL secure host Dataflow (GB/day) 0.04 Joint Ops Quick Look Hk 1610 1210 Level 0 (HMI & AIA) 1230 Level 1 (HMI) Data Capture 1230 HMI High Level Processing 2 processors each HMI & AIA Science 2 processors 16 processors c. 200 processors 1210 75 1610 1200 30d cache 40TB each Online Data LMSAL Link (AIA Level 0, HMI Magnetograms) 325TB+50TB/yr rarely needed 240 1820 Redundant data capture system Data Exports 2 processors Science Archive 440TB/yr (Offsite) HMI Science Analysis Archive 650TB/yr 1230 SDO Scientist & User Interface

25. JSOC Development Strategy • SOC Ops system developed at LMSAL as evolution of MDI, TRACE, SXI, etc. programs. • During instrument build, used with EGSE for I&T • During operations hour/day for health check and day/week for command loads • SOC Data system developed at Stanford as evolution of existing MDI data system. • 2004 - 2005: First 2 Years • Procure development system with most likely components (e.g. tape type, cluster vs SMP, SAN vs NAS, etc) • Modify pipeline and catalog infrastructure and implement on prototype system. • Modify analysis module API for greater simplicity and compliance with pipeline. • Develop calibration software modules. • 2006 - 2007: Two years prior to launch • Complete Level-1 analysis development, verify with HMI test data. • Populate prototype system with MDI data to verify performance. • Procure, install, verify computer hardware. • Implement higher-level pipeline processing modules with Co-I support • During Phase-E • Add media and disk farm capacity in staged plan, half-year or yearly increments • First two years of mission continue Co-I pipeline testing support

26. HMI E/PO Education / Public Outreach • HMI E/PO Plans: • Development of a model Science Fellow Program: a science-outreach, community service student training program implemented and tested in a collection of underserved environments • Solar Planetarium Program for small, interactive planetaria (joint with LWS, Lawrence Hall of Science, & AIA) • Solar Sudden Ionospheric Disturbance Monitor (Solar SID) Program developed and established in high schools throughout the nation (collaborative effort with NSF CISM) • Information Resources – Posters, Web, Press, etc. • Partnerships with AIA instrument team, other NASA entities, science museums and planetaria