1. LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager http://hmi.stanford.edu Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO Workshop 23-26 March 2004

2. LWS Science Team Meeting, 23 Mar 2004, Boulder2 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. LWS Science Team Meeting, 23 Mar 2004, Boulder3 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. Investigation Overview - 1

4. LWS Science Team Meeting, 23 Mar 2004, Boulder4 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. LWS Science Team Meeting, 23 Mar 2004, Boulder5 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. LWS Science Team Meeting, 23 Mar 2004, Boulder6 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. HMI Science Objectives – Top Level

7. LWS Science Team Meeting, 23 Mar 2004, Boulder7 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. LWS Science Team Meeting, 23 Mar 2004, Boulder8 Version 1.0 HMI Data Products and Objectives

9. LWS Science Team Meeting, 23 Mar 2004, Boulder9 A.Sound speed variations relative to a standard solar model. B.Solar cycle variations in the sub-photospheric rotation rate. C.Solar meridional circulation and differential rotation. D.Sunspots and plage contribute to solar irradiance variation. E.MHD model of the magnetic structure of the corona. F.Synoptic map of the subsurface flows at a depth of 7 Mm. G.EIT image and magnetic field lines computed from the photospheric field. H.Active regions on the far side of the sun detected with helioseismology. I.Vector field image showing the magnetic connectivity in sunspots. J.Sound speed variations and flows in an emerging active region. B – Rotation Variations C – Global Circulation D – Irradiance Sources H – Far-side Imaging F – Solar Subsurface Weather E – Coronal Magnetic Field I – Magnetic Connectivity J – Subsurface flows G – Magnetic Fields A – Interior Structure HMI Data Product Examples

10. LWS Science Team Meeting, 23 Mar 2004, Boulder10 Solar Domain of HMI Helioseismology rotation 2 3 4 5 6 7 Sun Log Size (km) Zonal flow AR spot SG dynamo P-modes Time-Distance Rings Global HS 123 45 6 7 89 min 5min hour day year cycle Log Time (s) 10 polar field Earth HMI resolution granule

11. LWS Science Team Meeting, 23 Mar 2004, Boulder11 Solar Domain of HMI Magnetic Field 2 3 4 5 6 7 Sun Log Size (km) Large-Scale AR spot SG dynamo P-modes 123 45 6 7 89 min 5min hour day rotation year cycle Log Time (s) 10 polar field Earth HMI resolution granule Coronal field estimates Vector Line-of-sight

12. LWS Science Team Meeting, 23 Mar 2004, Boulder12 HMI Co-Investigator Science Team-1 HMI Science Team NameRoleInstitutionPhase B,C,DPhase-E HMI Lead Institutions Philip H. ScherrerPIStanford UniversityHMI InvestigationSolar Science John G. BeckA-IStanford UniversityE/PO Science LiaisonSurface Flows Richard S. BogartCo-IStanford UniversityData Pipeline and AccessNear Surface Flows Rock I. BushCo-IStanford UniversityProgram ManagerIrradiance and Shape Thomas L. Duvall, Jr.Co-INASA Goddard Space Flight CenterTime-Distance CodeHelioseismology Alexander G. KosovichevCo-IStanford UniversityInversion CodeHelioseismology Yang LiuA-IStanford UniversityVector Field Observable CodeActive Region Fields Jesper SchouCo-IStanford UniversityInstrument ScientistHelioseismology Xue Pu ZhaoCo-IStanford UniversityCoronal CodeCoronal Field Models Alan M. TitleCo-ILMSALHMI InstrumentSolar Science Thomas BergerA-ILMSAL* Vector Field CalibrationActive Region Science Thomas R. MetcalfCo-ILMSAL* Vector Field CalibrationActive Region Science Carolus J. SchrijverCo-ILMSAL* Magnetic Field Assimilation ModelsActive Region Science Theodore D. TarbellCo-ILMSALHMI CalibrationActive Region Science Bruce W. LitesA-IHigh Altitude ObservatoryVector Field InversionsActive Region Science Steven TomczykCo-IHigh Altitude ObservatoryVector Field InversionsActive Region Science * Phase D only

13. LWS Science Team Meeting, 23 Mar 2004, Boulder13 HMI Co-Investigator Science Team-2 HMI Science Team – US and International Co-Is NameRoleInstitutionPhase B,C,DPhase-E HMI US Co-Investigator Institutions Sarbani BasuCo-IYale University* Ring Analysis CodeHelioseismology Douglas C. BraunCo IColorado Research Associates* Farside Imaging CodeHelioseismology Philip R. GoodeCo-INJIT, Big Bear Solar Observatory* Magnetic and Helioseismic CodeFields and Helioseismology Frank HillCo-INational Solar Observatory* Ring Analysis CodeHelioseismology Rachel HoweCo-INational Solar Observatory* Internal Rotation Inversion CodeHelioseismology Sylvain KorzennikA-ISmithsonian Astrophysical ObservatoryHelioseismology Jeffrey R. KuhnCo-IUniversity of Hawaii* Limb and Irradiance CodeIrradiance and Shape Charles A. LindseyCo-IColorado Research Associates* Farside Imaging CodeHelioseismology Jon A. LinkerCo-IScience Applications Intnl. Corp.* Coronal MHD Model CodeCoronal Physics N. Nicolas MansourCo-INASA Ames Research Center* Convection Zone MHD Model CodeConvection Physics Edward J. Rhodes, Jr.Co-IUniversity of Southern California* Helioseismic Analysis CodeHelioseismology Juri ToomreCo-IJILA, Univ. of Colorado* Sub-Surface-Weather CodeHelioseismology Roger K. UlrichCo-IUniversity of California, Los Angeles* Magnetic Field Calibration CodeSolar Cycle Alan WrayCo-INASA Ames Research Center* Convection Zone MHD Model CodeConvection Physics HMI International Co-Investigators J. Christensen-DalsgaardCo-ITAC, Aarhus University, DK* Solar Model CodeHelioseismology J. Leonard CulhaneCo-IMSSL, University College London, UKActive Region Science Bernhard FleckCo-IEuropean Space AgencyILWS CoordinationAtmospheric Dynamics Douglas O. GoughCo-IIoA, Cambridge University, UK* Local HS Inversion CodeHelioseismology Richard A. HarrisonCo-IRutherford Appleton Laboratories, UKActive Region Science Takashi SekiiCo-INational Astron. Obs. of Japan, JPHelioseismology Hiromoto ShibahashiCo-IUniversity of Tokyo, JPHelioseismology Sami K. SolankiCo-IMax-Planck-Institut für Aeronomie, DEAR Science Michael J. ThompsonCo-IImperial College, UKHelioseismology * Phase D only

14. LWS Science Team Meeting, 23 Mar 2004, Boulder14 HMI Institutional Roles HMI Instrument HMI-AIA JSOC HMI Science Team SDO Science LWS Science HMI E/PO Stanford LMSAL

15. LWS Science Team Meeting, 23 Mar 2004, Boulder15 HMI Team Organization Alan Title HMI-LMSAL Lead Rock Bush HMI-Stanford Prg. Mgr. Larry Springer LMSAL SDO Prg. Mgr. Jim Aloise Ground System Rasmus Larsen Processing & Analysis Deborah Scherrer Educ. & Public Outreach Rick Bogart Data Export Barbara Fischer HMI Deputy Prg. Mgr. Philip Scherrer HMI Principal Investigator Edgar Thomas Camera Electronics Dexter Duncan CCDs John Miles System Engineering Rose Navarro Thermal Russ Lindgren Electrical Lead Glenn Gradwohl Mechanical Lead Dave Akin Mechanism Lead Rick Rairden Optical Elements Jerry Drake Inst. Software Lead Mike Levay Integration & Test Jesper Schou Instrument Scientist Local Helioseismology - Alexander Kosovichev Global Helioseismology - Jesper Schou Magnetic Fields - Yang Liu HAO Vector Fields team Co-I Science Team Science Team Romeo Durscher HMI Admin Keh-Cheng Chu Ground Sys Hardware

16. LWS Science Team Meeting, 23 Mar 2004, Boulder16 Science Team Coordination Team meetings: May 2003, Mag splinter Oct 2003 Next HMI (+AIA?) September 2004 Leads for Planning Local HelioseismologySasha Kosovichev Global HelioseismologyJesper Schou Modeling & InversionsSasha Kosovichev Mag Field large & smallYang Liu Vector Field InversionsSteve Tomczyk Continuum studiesRock Bush Space Weather Coord.Yang Liu

17. LWS Science Team Meeting, 23 Mar 2004, Boulder17 HMI S/C Accommodations HOP HEB X Y Z

18. LWS Science Team Meeting, 23 Mar 2004, Boulder18 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. LWS Science Team Meeting, 23 Mar 2004, Boulder19 HMI Optics Package (HOP) OP Structure Telescope Front Window Front Door Vents Support Legs (6) Polarization Selector Focus/Calibration Wheels Active Mirror Limb B/S Alignment Mech Oven Structure Michelson Interf. Lyot Filter Shutters Connector Panel CEBs Detector (Vector) Fold Mirror Focal Plane B/S 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 Y X Detector (Doppler) Limb Sensor Z

20. LWS Science Team Meeting, 23 Mar 2004, Boulder20 HMI Requirements - Driving ParameterRequirement Central wavelength6173.3 Å ± 0.1 Å (Fe I line) Filter bandwidth76 mÅ ± 10 mÅ fwhm Filter tuning range680 mÅ ± 68 mÅ Central wavelength drift< 10 mÅ during any 1 hour period Field of view> 2000 arc-seconds Angular resolutionbetter than 1.5 arc-seconds Focus adjustment range± 4 depths of focus Pointing jitter reduction factor> 40db with servo bandwidth > 30 Hz Image stabilization offset range> ± 14 arc-seconds in pitch and yaw Pointing adjustment range> ± 200 arc-seconds in pitch and yaw Pointing adjustment step size< 2 arc-seconds in pitch and yaw Dopplergram cadence< 50 seconds Image cadence for each camera< 4 seconds Full image readout rate< 3.2 seconds Exposure knowledge< 5 microseconds Timing accuracy< 0.1 seconds of ground reference time Detector format> 4000 x 4000 pixels Detector resolution0.50 ± 0.01 arc-second / pixel Science telemetry compressionTo fit without loss in allocated telemetry Eclipse recovery< 60 minutes after eclipse end Instrument design lifetime5 years at geosynchronous orbit

21. LWS Science Team Meeting, 23 Mar 2004, Boulder21 Data Section 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 X Y Z Power Section

22. LWS Science Team Meeting, 23 Mar 2004, Boulder22 HMI & AIA JSOC Architecture Science Team Forecast Centers EPO Public Catalog Primary Archive HMI & AIA Operations House- keeping Database MOC DDS Redundant Data Capture System 30-Day Archive Offsite Archiv e Offline Archiv e HMI JSOC Pipeline Processing System Data Export & Web Service Stanford LMSAL High-Level Data Import AIA Analysis System LM-Local Archive Quicklook Viewing housekeeping GSFC White Sands World

23. LWS Science Team Meeting, 23 Mar 2004, Boulder23 HMI - SOC Pipeline HMI Data Analysis Pipeline Doppler Velocity Heliographic Doppler velocity maps Tracked Tiles Of Dopplergrams Stokes I,V Filtergrams Continuum Brightness Tracked full-disk 1-hour averaged Continuum maps Brightness feature maps Solar limb parameters Stokes I,Q,U,V Full-disk 10-min Averaged maps Tracked Tiles Line-of-sight Magnetograms Vector Magnetograms Fast algorithm Vector Magnetograms Inversion algorithm Egression and Ingression maps Time-distance Cross-covariance function Ring diagrams Wave phase shift maps Wave travel times Local wave frequency shifts Spherical Harmonic Time series To l=1000 Mode frequencies And splitting Brightness Images Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Internal sound speed, c s (r,Θ) (0<r<R) Internal rotation Ω(r,Θ) (0<r<R) Vector Magnetic Field Maps HMI Data Data ProductProcessing Level-0 Level-1

24. LWS Science Team Meeting, 23 Mar 2004, Boulder24 HMI - SOC Processing and Data Flow Dataflow (GB/day) Joint Ops Science Archive 440TB/yr (Offsite) Data Capture 2 processors each 1230 1610 HMI & AIA Science Hk 0.04 30d cache 40TB each Quick Look LMSAL secure host Level 0 (HMI & AIA) 2 processors 75 Level 1 (HMI) 16 processors Online Data 325TB+50TB/yr HMI High Level Processing c. 200 processors HMI Science Analysis Archive 650TB/yr Redundant data capture system 1210 Data Exports 1200 LMSAL Link (AIA Level 0, HMI Magnetograms) 240 1610 1820 1230 rarely needed 1230 2 processors SDO Scientist & User Interface

25. LWS Science Team Meeting, 23 Mar 2004, Boulder25 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. LWS Science Team Meeting, 23 Mar 2004, Boulder26 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