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 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 HMI Major Science Objectives 1.B – Solar Dynamo 1.J – Sunspot Dynamics 60 1.C – Global Circulation 30 0 Latitude -30 -60 1997 1998 1999 2000 2001 2002 Year 1.I – Magnetic Connectivity -1 1.A – Interior Structure v (km s ) 1.4 -1.4 1.D – Irradiance Sources B (kG) 2.0 -2.0 Flux (kG) 1.0 -1.5 Ic to disk center 10Mm 1.E – Coronal Magnetic Field 1.H – Far-side Imaging NOAA 9393 Far- side 1.G – Magnetic Stresses 1.F – Solar Subsurface Weather HMI - SOC Pipeline Processing Data Product HMI Data Spherical Internal rotation Ω(r,Θ) Heliographic Harmonic Mode frequencies (0<r<R) Doppler velocity Time series And splitting Internal sound speed, Filtergrams maps To l=1000 cs(r,Θ) (0<r<R) Full-disk velocity, v(r,Θ,Φ), Local wave And sound speed, c (r,Θ,Φ), Ring diagrams s frequency shifts Maps (0-30Mm) Level-0 Doppler Velocity Carrington synoptic v and c Time-distance s Tracked Tiles maps (0-30Mm) Cross-covariance Wave travel times Of Dopplergrams function High-resolution v and cs maps (0-30Mm) Egression and Wave phase Ingression maps shift maps Deep-focus v and cs maps (0-200Mm) 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 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.