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) http://hmi.stanford.edu HMI Science Objectives

Convection-zone dynamics and the solar dynamo ƒ Structure and dynamics of the tachocline ƒ Variations in differential rotation ƒ Evolution of meridional circulation ƒ Dynamics in the near surface shear layer Origin and evolution of sunspots, active regions and complexes of activity ƒ Formation and deep structure of magnetic complexes of activity ƒ Active region source and evolution ƒ Magnetic flux concentration in sunspots ƒ Sources and mechanisms of solar irradiance variations Sources and drivers of solar activity and disturbances ƒ Origin and dynamics of magnetic sheared structures and d-type sunspots ƒ Magnetic configuration and mechanisms of solar flares ƒ Emergence of magnetic flux and solar transient events ƒ Evolution of small-scale structures and magnetic carpet Links between the internal processes and dynamics of the corona and heliosphere ƒ Complexity and energetics of the solar corona ƒ Large-scale coronal field estimates ƒ Coronal magnetic structure and solar wind Precursors of solar disturbances for space-weather forecasts ƒ Far-side imaging and activity index ƒ Predicting emergence of active regions by helioseismic imaging ƒ Determination of magnetic cloud Bs events urces ulation r c r i he t etic Field lobal C rradiance So n I G ce Wea – 1.D – al Mag 1.C n oro 2 C 200 olar Subsurfa S 2001 1.E – namo 1.F – 2000 Year 1999 olar Dy S 1998 nterior Structure I 1.B – 1997 1.A – 0

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Stokes Line-of-sight Far-side activity index Level-1 I,V Magnetograms Line-of-Sight Magnetic Field Maps Stokes Full-disk 10-min Vector Magnetograms I,Q,U,V Averaged maps Fast algorithm Vector Magnetic Field Maps Vector Magnetograms Tracked Tiles Coronal magnetic Inversion algorithm Field Extrapolations Tracked full-disk Continuum Coronal and 1-hour averaged Solar limb parameters Brightness Solar wind models Continuum maps Brightness feature Brightness Images maps HMI Data Analysis Pipeline HMI Science Working Groups

Helioseismology Magnetic Fields

Modeling & Vector Field Magnetic Field Intercomparison Artificial Data Measurements Reconstruction

Global Time-Distance Heliosphere Synoptic Maps Helioseismology Helioseismology Space Weather and Evolution Holography

Interior-Corona Irradiance- Ring Diagrams Links Magnetic Field Relations HMI Helioseismology Working Groups

Modeling & Intercomparison Artificial Data Komm/Zhao Mansour/Toomre

Global Time-Distance Helioseismology Helioseismology Rhodes/Schou Holography Braun/Kosovichev

Interior-Corona Ring Diagrams Bogart/Haber Links Hurlburt/Kosovichev Task samples 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 Intercomparision

• Ring diagrams – Time-distance helioseismology • Time-distance – Holography • Local – Global Helioseismology • MDI - GONG Global Helioseismology

• Improving precision of medium-l data • Fitting methods for high-l modes (l=300- 1500) • Mode coupling effects 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 Ring-diagram method

• Effects of non-uniform wave excitation and damping • 3D sensitivity kernels and inversions • Magnetic effects • Error analysis Interior – Corona Links

• Relationship between internal flows, magnetic field dynamics and coronal activity • MHD models of coronal response • Synoptic maps and evolution HMI Science meetings ƒ 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 Comments & suggestions