HMI Data Products: Plan and Status

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HMI Data ProductsPlan and Status
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Primary goal origin of solar variability

• 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 Suns interior and the various
  components of magnetic activity.
• HMI produces data to determine the interior
  sources and mechanisms of solar variability and
  how the physical processes inside the Sun are
  related to surface and coronal magnetic fields
  and activity.

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Key Features of HMI Science Plan

• Data analysis pipeline standard helioseismology
  and magnetic field analyses
• Development of new approaches to data analysis
• Targeted theoretical and numerical modeling
• Focused data analysis and science working groups
• Joint investigations with AIA and EVE
• Cooperation with other space- and ground-based
  projects (SOHO, Hinode, PICARD, STEREO, RHESSI,
  GONG, SOLIS, HELAS)

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Primary Science Objectives

• Convection-zone dynamics and 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.
• 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 delta-type sunspots.
• Magnetic configuration and mechanisms of solar
  flares and CME.
• 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 solar corona.
• Large-scale coronal field estimates.

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HMI Science Analysis Plan
Magnetic Shear
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HMI module status and MDI heritage
Intermediate and high level data products
Primary observables
Internal rotation
Heliographic Doppler velocity maps
Spherical Harmonic Time series
Mode frequencies And splitting
Internal sound speed
Full-disk velocity, sound speed, Maps (0-30Mm)
Local wave frequency shifts
Ring diagrams
Doppler Velocity
Carrington synoptic v and cs maps (0-30Mm)
Time-distance Cross-covariance function
Tracked Tiles Of Dopplergrams
Wave travel times
High-resolution v and cs maps (0-30Mm)
Research codes in use by team
Egression and Ingression maps
Wave phase shift maps
Deep-focus v and cs maps (0-200Mm)
Far-side activity index
Stokes I,V
Line-of-sight Magnetograms
Line-of-Sight Magnetic Field Maps
Stokes I,Q,U,V
Full-disk 10-min Averaged maps
Vector Magnetograms Fast algorithm
Vector Magnetic Field Maps
Vector Magnetograms Inversion algorithm
Coronal magnetic Field Extrapolations
Tracked Tiles
Tracked full-disk 1-hour averaged Continuum maps
Coronal and Solar wind models
Continuum Brightness
Solar limb parameters
Brightness feature maps
Brightness Images
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JSOC - HMI Pipeline
Data Product
Processing
HMI Data
Internal rotation O(r,T) (0ltrltR)
Spherical Harmonic Time series To l1000
Heliographic Doppler velocity maps
Filtergrams
Mode frequencies And splitting
Internal sound speed, cs(r,T) (0ltrltR)
Full-disk velocity, v(r,T,F), And sound speed,
cs(r,T,F), Maps (0-30Mm)
Local wave frequency shifts
Ring diagrams
Doppler Velocity
Level-0
Carrington synoptic v and cs maps (0-30Mm)
Time-distance Cross-covariance function
Tracked Tiles Of Dopplergrams
Wave travel times
High-resolution v and cs maps (0-30Mm)
Egression and Ingression maps
Wave phase shift maps
Deep-focus v and cs maps (0-200Mm)
Far-side activity index
Stokes I,V
Line-of-sight Magnetograms
Level-1
Line-of-Sight Magnetic Field Maps
Stokes I,Q,U,V
Full-disk 10-min Averaged maps
Vector Magnetograms Fast algorithm
Vector Magnetic Field Maps
Vector Magnetograms Inversion algorithm
Coronal magnetic Field Extrapolations
Tracked Tiles
Tracked full-disk 1-hour averaged Continuum maps
Coronal and Solar wind models
Continuum Brightness
Solar limb parameters
Brightness Images
Brightness feature maps
HMI Data Analysis Pipeline
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Helioseismology
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Global helioseismology
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Ring Diagrams
Need
Need
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Time-Distance Helioseismology
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Acoustic Holography
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Magnetic Fields
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Line-of Sight Magnetic Field
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Vector Magnetic Field
Need
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Intensity
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Detail Example Time-Distance Helioseismology
Products

• Full-disk synoptic flow maps
• Area from -60 to 60 deg in longitude and
  latitude (30x30 deg tracked regions, sampling
  TBD)
• Depth 0-30 Mm ( 20 distances)
• Cadence 3 per day
• Resolution 0.2 deg per pixel
• Comment systematic errors for sound-speed maps
  may be too large usefulness is unclear
  suggestion descope
• Carrington synoptic maps
• Central meridian flow maps made from the
  full-disk maps
• High-resolution flow and sound-speed maps of
  tracked AR
• Area 30x30 deg
• Depth 0-30 Mm
• Cadence 8 hours (with a 2-hour shift? Need to
  study this option)
• Resolution 0.06 deg/pixel
• Track areas of all AR in NOAA from -60 to 60
  longitude (including periods prior flux emergence
  and after disappearance)
• Need matching vector magnetograms
• High-resolution flow and sound-speed maps of
  flaring AR
• Area 30x30 deg
• Depth 0-30 Mm
• Cadence 4 hours (with a 1-hour shift)

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Organization of TD data analysis

• Two parallel techniques
• Gabor wavelet fitting for phase and group travel
  times ray-path inversions
• Cross-correlation measurement of reference travel
  times Born inversions
• Two data analysis options
• Standard pipeline processing with standard
  fitting and inversion parameters
• Interactive processing (Junweis IDL widgets)
  should be able to import intermediate data from
  pipeline processing (e.g. travel times for
  experimental inversions)

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Summary

• HMI will provide key data to study the Suns
  dynamics and magnetism subsurface flow maps and
  photospheric vector magnetic fields.
• The HMI data analysis plan includes a standard
  pipeline processing and interactive data analysis
  tools.
• The analysis pipeline is being developed by the
  Co-I team, using existing techniques and
  software.
• However, to fully utilize the science potential
  of HMI additional funding is necessary for Co-Is
  teams (in particular, for helioseismic imaging of
  the deep interior/tachocline, and
  coronal/heliospheric magnetic field analysis and
  models).