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HMI Data Products: Plan and Status. Primary goal: origin of solar variability. - PowerPoint PPT Presentation
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Page 1 LWS Teams Day JSOC Overview
HMI Data Products:Plan and Status
Page 2 LWS Teams Day JSOC Overview
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.
Page 3 LWS Teams Day JSOC Overview
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)
Page 4 LWS Teams Day JSOC Overview
HMI Major Science Objectives1.B – Solar Dynamo
1.C – Global Circulation
1.D – Irradiance Sources
1.H – Far-side Imaging
1.F – Solar Subsurface Weather
1.E – Coronal Magnetic Field
1.I – Magnetic Connectivity
1.J – Sunspot Dynamics
1.G – Magnetic Stresses
1.A – Interior Structure
NOAA 9393
Far-side
Page 5 LWS Teams Day JSOC Overview
1. 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.
2. 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.
3. 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.
4. 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
5. 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.
Primary Science Objectives
Page 6 LWS Teams Day JSOC Overview
HMI Science Analysis Plan
Magnetic Shear
Tachocline
Differential Rotation
Meridional Circulation
Near-Surface Shear Layer
Activity Complexes
Active Regions
Sunspots
Irradiance Variations
Flare Magnetic Configuration
Flux Emergence
Magnetic Carpet
Coronal energetics
Large-scale Coronal Fields
Solar Wind
Far-side Activity Evolution
Predicting A-R Emergence
IMF Bs Events
Brightness Images
Global Helioseismology
Processing
Local Helioseismology
Processing
Version 1.0w
Filtergrams
Line-of-sightMagnetograms
Vector Magnetograms
DopplerVelocity
ContinuumBrightness
Line-of-SightMagnetic Field Maps
Coronal magneticField Extrapolations
Coronal andSolar wind models
Far-side activity index
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Internal sound speed,cs(r,Θ) (0<r<R)
Internal rotation Ω(r,Θ)(0<r<R)
Vector MagneticField Maps
Science ObjectiveData ProductProcessing
Observables
HMI Data
Page 7 LWS Teams Day JSOC Overview
HMI module status and MDI heritage
DopplerVelocity
HeliographicDoppler velocity
maps
Tracked TilesOf Dopplergrams
StokesI,V
ContinuumBrightness
Tracked full-disk1-hour averagedContinuum maps
Brightness featuremaps
Solar limb parameters
StokesI,Q,U,V
Full-disk 10-minAveraged maps
Tracked Tiles
Line-of-sightMagnetograms
Vector MagnetogramsFast algorithm
Vector MagnetogramsInversion algorithm
Egression andIngression maps
Time-distanceCross-covariance
function
Ring diagrams
Wave phase shift maps
Wave travel times
Local wave frequency shifts
SphericalHarmonic
Time series
Mode frequenciesAnd splitting
Brightness Images
Line-of-SightMagnetic Field Maps
Coronal magneticField Extrapolations
Coronal andSolar wind models
Far-side activity index
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs maps (0-30Mm)
Full-disk velocity, sound speed, Maps (0-30Mm)
Internal sound speed
Internal rotation
Vector MagneticField Maps
MDI pipeline modules exist
Standalone production codes in use at Stanford
Research codes in use by team
Codes to be developed at HAO
Codes being developed in the community
Codes to be developed at Stanford
Primary observables
Intermediate and high level data products
Page 8 LWS Teams Day JSOC Overview
JSOC - HMI Pipeline
HMI Data Analysis Pipeline
DopplerVelocity
HeliographicDoppler velocity
maps
Tracked TilesOf Dopplergrams
StokesI,V
Filtergrams
ContinuumBrightness
Tracked full-disk1-hour averagedContinuum maps
Brightness featuremaps
Solar limb parameters
StokesI,Q,U,V
Full-disk 10-minAveraged maps
Tracked Tiles
Line-of-sightMagnetograms
Vector MagnetogramsFast algorithm
Vector MagnetogramsInversion algorithm
Egression andIngression maps
Time-distanceCross-covariance
function
Ring diagrams
Wave phase shift maps
Wave travel times
Local wave frequency shifts
SphericalHarmonic
Time seriesTo l=1000
Mode frequenciesAnd splitting
Brightness Images
Line-of-SightMagnetic Field Maps
Coronal magneticField Extrapolations
Coronal andSolar wind models
Far-side activity index
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Internal sound speed,cs(r,Θ) (0<r<R)
Internal rotation Ω(r,Θ)(0<r<R)
Vector MagneticField Maps
HMI DataData ProductProcessing
Level-0
Level-1
Page 9 LWS Teams Day JSOC Overview
Helioseismology
Code: Doppler velocity, Lev1J.SchouS.Tomczyk
Status: needs improvements
Code: artificial dataN. MansourA. WrayR. Stein
Status: in development
DopplerVelocity
Tracked TilesOf Dopplergrams
Filtergrams
Egression andIngression maps
Time-distanceCross-covariance
function
Ring diagrams
Wave phase shift maps
Wave travel times
Local wave frequency shifts
Far-side activity index
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Internal rotation Ω(r,Θ)(0<r<R)
HeliographicDoppler velocity
maps
SphericalHarmonic
Time seriesTo l=1000
Mode frequenciesAnd splitting
Internal sound speed,cs(r,Θ) (0<r<R)
Page 10 LWS Teams Day JSOC Overview
Global helioseismology
Code: projectJ. Schou
Status: ready to port
Code: qdotprodJ.Schou
Status: ready to port
Code: med-l peak baggingJ.SchouHigh-l ridge fitting,E. Rhodes
Status: needs improvements
Code: sound-speed inversionsA.Kosovichev
Status: ready to port
Code: rotation inversionJ.SchouR. Howe
Status: ready to port
DopplerVelocity
Filtergrams
Internal rotation Ω(r,Θ)(0<r<R)Heliographic
Doppler velocitymaps
SphericalHarmonic
Time seriesTo l=1000
Mode frequenciesAnd splitting
Internal sound speed,cs(r,Θ) (0<r<R)
Page 11 LWS Teams Day JSOC Overview
Ring Diagrams
DopplerVelocity
Tracked TilesOf DopplergramsFiltergrams
Ring diagramsLocal wave
frequency shifts
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Code: fastrackR.Bogart,J.Toomre D. HaberB. Hindman
Status: needs improvements
Code: power spectrumR.Bogart
Status: ready to port
Code: sensitivity kernelsA.Birch
Status: in development
Code: inversionsJ.Toomre, D.Haber, B.Hindman
Status: needs improvements
Code: ring fittingS.Basu, F.Hill, J.Toomre,D.Haber,B.Hindman
Status: needs improvements
Need $$ Need $$
Page 12 LWS Teams Day JSOC Overview
Time-Distance Helioseismology
DopplerVelocity
Tracked TilesOf Dopplergrams
Filtergrams Time-distanceCross-covariance
functionWave travel times
Deep-focus v and cs
maps (0-200Mm)
High-resolution v and cs
maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
Full-disk velocity, v(r,Θ,Φ),And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Code: fastrackR.Bogart,T.DuvallJ.Zhao
Status: needs improvements (remapping issues)
Code: cross-covarianceT.DuvallJ.Zhao
Status: needs improvements
Code: travel time fittingT.DuvallJ.ZhaoS.Couvidat
Status: needs improvements
Code: sensitivity kernelsA.KosovichevJ.ZhaoA.Birch
Status: needs improvements
Code: inversionsA.KosovichevJ.Zhao, A.BirchS.CouvidatJ.ToomreB.Hindman
Status: needs improvements
Code: deep-focus mapsT.DuvallA.KosovichevJ.Zhao
Status: needs substantial development
Page 13 LWS Teams Day JSOC Overview
Acoustic Holography
DopplerVelocity
Tracked TilesOf Dopplergrams
Filtergrams Egression andIngression maps
Wave phase shift maps
Far-side activity index
High-resolution v and cs
maps (0-30Mm)
Code: fastrackR.BogartD.BraunC.Lindsay
Status: needs improvements (field-effect corrections)
Code: egression-ingressionD.BraunC.Lindsay
Status: needs improvements
Code: phase shiftsD.Braun C.Lindsay
Status: needs improvements (showglass corrections)
Code: sensitivity kernelsA. Birch
Status: in development
Code:holographic inversionsA.Birch
Status: in development
Code: Far-side imagingP.ScherrerC.LindsayD.Braun
Status: needs improvements
Inversions
Page 14 LWS Teams Day JSOC Overview
Magnetic Fields
StokesI,VFiltergrams
StokesI,Q,U,V
Full-disk 10-minAveraged maps
Tracked Tiles
Line-of-sightMagnetograms
Vector MagnetogramsFast algorithm
Vector MagnetogramsInversion algorithm
Line-of-SightMagnetic Field Maps
Coronal magneticField Extrapolations
Coronal andSolar wind models
Vector MagneticField Maps
Code: Stokes I,V,Lev0.5 V & LOS fieldJ. SchouS. Tomzcyk
Status: in development
Code: Stokes I,Q,U,VJ. SchouS. Tomzcyk
Status: in development
Page 15 LWS Teams Day JSOC Overview
Line-of Sight Magnetic Field
StokesI,VFiltergrams
Line-of-sightMagnetograms Line-of-Sight
Magnetic Field Maps
SynopticMagnetic Field Maps
Magnetic Footpoint Velocity Maps
Code: LOS magnetogramsJ. SchouS. TomzcykR. Ulrich (cross calib)
Status: in development
Code: LOS magnetic maps (project?)T. HoeksemaR. Bogart
Status: in development
Code: Synoptic Magnetic Field Maps T. HoeksemaX. ZhaoR. Ulrich
Status: in development
Code: Velocity Maps of Magnetic FootpointsY. LiuG. Fisher
Status: in development
Page 16 LWS Teams Day JSOC Overview
Vector Magnetic Field
Filtergrams StokesI,Q,U,V
Full-disk 10-minAveraged maps
Tracked Tiles
Vector MagnetogramsFast algorithm
Coronal magneticField Extrapolations
Vector MagneticField Maps
Code: fastrackR. Bogart
Status: needs modifications for fields
Code: Vector Field Fast and Inversion AlgorithmsJ. SchouS. Tomzcyk
Status: in development
Code: Vector Field MapsT. HoeksemaY.Liu
Status: in development
Code: Coronal Field Extrapolations &Ambiguity issue T.HoeksemaY.Liu, X.ZhaoC. SchrijverP.Goode T.MetcalfK.D.LekaStatus: in development
Code: Coronal Magnetic Field Topological PropertiesJ.LinkerV. Titov
Status: needs implementation
Code: Solar Wind ModelsX.ZhaoK.HayshiJ.LinkerP.GoodeV.Yurchishin
Status: in development
Coronal andSolar wind models
Vector MagnetogramsInversion algorithm
Need $$
Page 17 LWS Teams Day JSOC Overview
Intensity
Filtergrams ContinuumBrightness
Brightness Images
Code: Continuum MapsSchou
Status: in development
Code: Solar Limb Parameters, Lev0.5 used to make other Lev1 products, Lev2 for science goals
R. BushJ. Kuhn
Status: in development
Code: Brightness Feature Maps(European contribution)
Status: in development
Code: Averaged Continuum MapsBush
Status: in development
Solar limb parametersper image for Lev0.5
Brightness Synoptic Maps
Tracked full-disk1-hour averagedContinuum maps
Code: Brightness Synoptic MapsScherrer
Status: in development
Solar limb parameters
Brightness featuremaps
Page 18 LWS Teams Day JSOC Overview
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.
Page 19 LWS Teams Day JSOC Overview
Organization of TD data analysis
• Two parallel techniques:
1. Gabor wavelet fitting for phase and group travel times + ray-path inversions
2. Cross-correlation measurement of reference travel times + Born inversions
– Two data analysis options:
1. Standard pipeline processing with standard fitting and inversion parameters
2. Interactive processing (Junwei’s IDL widgets) – should be able to import intermediate data from pipeline processing (e.g. travel times for experimental inversions)
Page 20 LWS Teams Day JSOC Overview
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).