1. Helioseismology for HMI Science objectives and tasks* Data analysis plan* Helioseismology working groups and meetings *HMI Concept Study Report, Appendix A HMI Science Plan (SU-HMI-S014)HMI Concept Study Report, Appendix A HMI Science Plan (SU-HMI-S014) http://hmi.stanford.edu

2. 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

3. HMI Major Science Objectives 1.B – Solar Dynamo 1.C – Global Circulation 1.D – Irradiance Sources 1.H – Far-side Imaging 1.F – Solar Subsurface Weather 1.E – Coronal Magnetic Field 1.I – Magnetic Connectivity 1.J – Sunspot Dynamics 1.G – Magnetic Stresses 1.A – Interior Structure NOAA 9393 Far- side

5. 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

6. HMI Science Working Groups HelioseismologyMagnetic Fields Modeling & Artificial Data Time-Distance Helioseismology Holography Global Helioseismology Ring Diagrams Interior-Corona Links Vector Field Measurements Magnetic Field Reconstruction Synoptic B and interior Maps and Evolution Heliosphere Space Weather Irradiance- Magnetic Field Relations Intercomparison and validation

7. HMI Helioseismology Working Groups Modeling & Artificial Data Mansour/Toomre Time-Distance Helioseismology Holography Braun/Kosovichev Global Helioseismology Rhodes/Schou Ring Diagrams Bogart/Haber Interior-Corona Links Hurlburt/Kosovichev Intercomparison Komm/Zhao

8. Task samples

9. Modeling & Artificial Data Modeling Doppler signal of solar oscillation in magnetic regions 3D compressible solar convection + wave excitation Inelastic large-scale convection, differential rotation and meridional circulation Wave propagation models, local and global Wave interaction with flows and magnetic field

10. Intercomparision Ring diagrams – Time-distance helioseismology Time-distance – Holography Local – Global Helioseismology MDI - GONG

11. Global Helioseismology Improving precision of medium-l data Fitting methods for high-l modes (l=300- 1500) Mode coupling effects

12. Time-Distance Helioseismology & Holography Effects of magnetic field on wave travel times and phase shift (‘shower-glass’ effect) Non-uniform excitation and absorption (Woodard’s effect) Sensitivity kernels for sound-speed, flows, magnetic field (Born approximation) Error analysis (stochastic, distortion, remapping etc) Diagnostics of deep interior

13. Ring-diagram method Effects of non-uniform wave excitation and damping 3D sensitivity kernels and inversions Magnetic effects Error analysis

14. Interior – Corona Links Relationship between internal flows, magnetic field dynamics and coronal activity MHD models of coronal response Synoptic maps and evolution

15. HMI Science meetings  HMI Science Team meeting (Jan. 24-27?, 2005, Stanford) –Helioseismology Modeling & Artificial Data –CTR Summer Program: Solar Interior Dynamics Modeling (Jun.20-Jul.16, 2004,NASA/Ames) Time-Distance Helioseismology & Holography –Time-Distance/Holography Working Group (Aug 18-20, 2004, Stanford) –Magnetic Fields Magnetic Field Reconstruction –Force-Free Field Thinkshop, LMSAL 17-19 May 2004

16. Comments & suggestions