Helioseismology for HMI

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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

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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

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HMI - SOC Pipeline
Level-0
Level-1
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HMI Science Working Groups
Helioseismology
Magnetic Fields
Modeling Artificial Data
Vector Field Measurements
Magnetic Field Reconstruction
Intercomparison and validation
Time-Distance Helioseismology Holography
Global Helioseismology
Synoptic B and interior Maps and Evolution
Irradiance- Magnetic Field Relations
Ring Diagrams
Interior-Corona Links
Heliosphere Space Weather
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Task samples
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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

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Intercomparision

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

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Global Helioseismology

• Improving precision of medium-l data
• Fitting methods for high-l modes (l300-1500)
• Mode coupling effects

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Time-Distance Helioseismology Holography

• Effects of magnetic field on wave travel times
  and phase shift (shower-glass effect)
• Non-uniform excitation and absorption (Woodards
  effect)
• Sensitivity kernels for sound-speed, flows,
  magnetic field (Born approximation)
• Error analysis (stochastic, distortion, remapping
  etc)
• Diagnostics of deep interior

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Ring-diagram method

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

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Interior Corona Links

• Relationship between internal flows, magnetic
  field dynamics and coronal activity
• MHD models of coronal response
• Synoptic maps and evolution

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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

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