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HMI Data Products: Plan and Status

HMI Data Products: Plan and Status. Primary goal: origin of solar variability.

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HMI Data Products: Plan and Status

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  1. HMI Data Products:Plan and Status

  2. 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 Sun’s 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.

  3. 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)

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

  5. 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. • 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.

  6. Global Helioseismology Processing HMI Data Processing Data Product Science Objective Tachocline Internal rotation Ω(r,Θ) (0<r<R) Meridional Circulation Local Helioseismology Processing Filtergrams Internal sound speed, cs(r,Θ) (0<r<R) Differential Rotation Near-Surface Shear Layer Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Activity Complexes Active Regions Carrington synoptic v and cs maps (0-30Mm) Sunspots Doppler Velocity Irradiance Variations High-resolution v and cs maps (0-30Mm) Observables Deep-focus v and cs maps (0-200Mm) Flare Magnetic Configuration Line-of-sight Magnetograms Flux Emergence Far-side activity index Magnetic Carpet Line-of-Sight Magnetic Field Maps Vector Magnetograms Coronal energetics Large-scale Coronal Fields Vector Magnetic Field Maps Solar Wind Continuum Brightness Coronal magnetic Field Extrapolations Far-side Activity Evolution Predicting A-R Emergence Coronal and Solar wind models IMF Bs Events Version 1.0w Brightness Images HMI Science Analysis Plan Magnetic Shear

  7. Codes to be developed at Stanford Codes being developed in the community Codes to be developed at HAO Standalone production codes in use at Stanford MDI pipeline modules exist 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

  8. JSOC - HMI Pipeline Processing Data Product HMI Data Internal rotation Ω(r,Θ) (0<r<R) Spherical Harmonic Time series To l=1000 Heliographic Doppler velocity maps Filtergrams Mode frequencies And splitting Internal sound speed, cs(r,Θ) (0<r<R) Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), 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

  9. Internal rotation Ω(r,Θ) (0<r<R) Spherical Harmonic Time series To l=1000 Heliographic Doppler velocity maps Mode frequencies And splitting Internal sound speed, cs(r,Θ) (0<r<R) Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Local wave frequency shifts Filtergrams Ring diagrams Doppler Velocity Carrington synoptic v and cs maps (0-30Mm) Time-distance Cross-covariance function Tracked Tiles Of Dopplergrams Wave travel times Code: artificial data N. Mansour A. Wray R. Stein Status: in development Code: Doppler velocity, Lev1 J.Schou S.Tomczyk Status: needs improvements 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 Helioseismology

  10. Internal rotation Ω(r,Θ) (0<r<R) Spherical Harmonic Time series To l=1000 Filtergrams Heliographic Doppler velocity maps Mode frequencies And splitting Doppler Velocity Internal sound speed, cs(r,Θ) (0<r<R) Code: project J. Schou Status: ready to port Code: qdotprod J.Schou Status: ready to port Code: med-l peakbagging J.Schou High-l ridge fitting, E. Rhodes Status: needs improvements Code: sound-speed inversions A.Kosovichev Status: ready to port Code: rotation inversion J.Schou R. Howe Status: ready to port Global helioseismology

  11. Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Local wave frequency shifts Filtergrams Ring diagrams Tracked Tiles Of Dopplergrams Doppler Velocity Carrington synoptic v and cs maps (0-30Mm) Code: fastrack R.Bogart, J.Toomre D. Haber B. Hindman Status: needs improvements Code: power spectrum R.Bogart Status: ready to port Code: sensitivity kernels A.Birch Status: in development Code: inversions J.Toomre, D.Haber, B.Hindman Status: needs improvements Code: ring fitting S.Basu, F.Hill, J.Toomre, D.Haber, B.Hindman Status: needs improvements Ring Diagrams Need $$ Need $$

  12. Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Filtergrams Carrington synoptic v and cs maps (0-30Mm) Time-distance Cross-covariance function Doppler Velocity Tracked Tiles Of Dopplergrams Wave travel times High-resolution v and cs maps (0-30Mm) Deep-focus v and cs maps (0-200Mm) Code: fastrack R.Bogart, T.Duvall J.Zhao Status: needs improvements (remapping issues) Code: cross-covariance T.Duvall J.Zhao Status: needs improvements Code: travel time fitting T.Duvall J.Zhao S.Couvidat Status: needs improvements Code: sensitivity kernels A.Kosovichev J.Zhao A.Birch Status: needs improvements Code: inversions A.Kosovichev J.Zhao, A.Birch S.Couvidat J.Toomre B.Hindman Status: needs improvements Code: deep-focus maps T.Duvall A.Kosovichev J.Zhao Status: needs substantial development Time-Distance Helioseismology

  13. High-resolution v and cs maps (0-30Mm) Filtergrams Doppler Velocity Tracked Tiles Of Dopplergrams Egression and Ingression maps Wave phase shift maps Inversions Far-side activity index Code: fastrack R.Bogart D.Braun C.Lindsay Status: needs improvements (field-effect corrections) Code: egression-ingression D.Braun C.Lindsay Status: needs improvements Code: phase shifts D.Braun C.Lindsay Status: needs improvements (showglass corrections) Code: sensitivity kernels A. Birch Status: in development Code: holographic inversions A.Birch Status: in development Code: Far-side imaging P.Scherrer C.Lindsay D.Braun Status: needs improvements Acoustic Holography

  14. Vector Magnetic Field Maps Code: Stokes I,V, Lev0.5 V & LOS field J. Schou S. Tomzcyk Status: in development Code: Stokes I,Q,U,V J. Schou S. Tomzcyk Status: in development Filtergrams 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 Magnetograms Inversion algorithm Coronal magnetic Field Extrapolations Tracked Tiles Coronal and Solar wind models Magnetic Fields

  15. Filtergrams Stokes I,V Line-of-sight Magnetograms Line-of-Sight Magnetic Field Maps Synoptic Magnetic Field Maps Magnetic Footpoint Velocity Maps Code: LOS magnetograms J. Schou S. Tomzcyk R. Ulrich (cross calib) Status: in development Code: LOS magnetic maps (project?) T. Hoeksema R. Bogart Status: in development Code: Synoptic Magnetic Field Maps T. Hoeksema X. Zhao R. Ulrich Status: in development Code: Velocity Maps of Magnetic Footpoints Y. Liu G. Fisher Status: in development Line-of Sight Magnetic Field

  16. Vector Magnetic Field Maps Filtergrams Stokes I,Q,U,V Full-disk 10-min Averaged maps Vector Magnetograms Fast algorithm Coronal magnetic Field Extrapolations Vector Magnetograms Inversion algorithm Tracked Tiles Coronal and Solar wind models Code: fastrack R. Bogart Status: needs modifications for fields Code: Vector Field Fast and Inversion Algorithms J. Schou S. Tomzcyk Status: in development Code: Vector Field Maps T. Hoeksema Y.Liu Status: in development Code: Coronal Field Extrapolations & Ambiguity issue T.Hoeksema Y.Liu, X.Zhao C. Schrijver P.Goode T.Metcalf K.D.Leka Status: in development Code: Coronal Magnetic Field Topological Properties J.Linker V. Titov Status: needs implementation Code: Solar Wind Models X.Zhao K.Hayshi J.Linker P.Goode V.Yurchishin Status: in development Vector Magnetic Field Need $$

  17. Brightness Images Filtergrams Tracked full-disk 1-hour averaged Continuum maps Continuum Brightness Brightness Synoptic Maps Solar limb parameters Solar limb parameters per image for Lev0.5 Brightness feature maps Code: Continuum Maps Schou Status: in development Code: Solar Limb Parameters, Lev0.5 used to make other Lev1 products, Lev2 for science goals R. Bush J. Kuhn Status: in development Code: Brightness Feature Maps (European contribution) Status: in development Code: Averaged Continuum Maps Bush Status: in development Code: Brightness Synoptic Maps Scherrer Status: in development Intensity

  18. 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) • Resolution: 0.06 deg/pixel • Track AR with NOAA probability of X-class flare > 30% ? (need selection criteria) • Need corresponding high-cadence vector magnetograms • Deep-focus flow maps • Keep as research topic, include in pipeline when ready. Additional funding/FTE required.

  19. 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 (Junwei’s IDL widgets) – should be able to import intermediate data from pipeline processing (e.g. travel times for experimental inversions)

  20. Summary • HMI will provide key data to study the Sun’s 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-I’s teams (in particular, for helioseismic imaging of the deep interior/tachocline, and coronal/heliospheric magnetic field analysis and models).

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