Page 1LWS Teams Day JSOC Overview HMI Data Products: Plan and Status.

LWS Teams Day JSOC Overview

HMI Data Products:Plan and Status


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.


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)


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


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


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


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


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





Deep-focus v and cs

maps (0-200Mm)


maps (0-30Mm)

Carrington synoptic v and cs maps (0-30Mm)

Full-disk velocity, sound speed, Maps (0-30Mm)

Internal sound speed

Internal rotation


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


JSOC - HMI Pipeline

HMI Data Analysis Pipeline

DopplerVelocity


maps


StokesI,V

Filtergrams

ContinuumBrightness




StokesI,Q,U,V


Tracked Tiles






function

Ring diagrams


Wave travel times


SphericalHarmonic

Time seriesTo l=1000


Brightness Images





Deep-focus v and cs

maps (0-200Mm)


maps (0-30Mm)


maps (0-30Mm)


Maps (0-30Mm)




HMI DataData ProductProcessing

Level-0

Level-1


Helioseismology

Code: Doppler velocity, Lev1J.SchouS.Tomczyk

Status: needs improvements

Code: artificial dataN. MansourA. WrayR. Stein

Status: in development

DopplerVelocity


Filtergrams



function

Ring diagrams


Wave travel times



Deep-focus v and cs

maps (0-200Mm)


maps (0-30Mm)


maps (0-30Mm)


Maps (0-30Mm)



maps

SphericalHarmonic





Global helioseismology

Code: projectJ. Schou

Status: ready to port

Code: qdotprodJ.Schou


Code: med-l peak baggingJ.SchouHigh-l ridge fitting,E. Rhodes


Code: sound-speed inversionsA.Kosovichev


Code: rotation inversionJ.SchouR. Howe


DopplerVelocity

Filtergrams

Internal rotation Ω(r,Θ)(0<r<R)Heliographic

Doppler velocitymaps

SphericalHarmonic





Ring Diagrams

DopplerVelocity

Tracked TilesOf DopplergramsFiltergrams

Ring diagramsLocal wave

frequency shifts


maps (0-30Mm)


Maps (0-30Mm)

Code: fastrackR.Bogart,J.Toomre D. HaberB. Hindman


Code: power spectrumR.Bogart


Code: sensitivity kernelsA.Birch


Code: inversionsJ.Toomre, D.Haber, B.Hindman


Code: ring fittingS.Basu, F.Hill, J.Toomre,D.Haber,B.Hindman


Need $$ Need $$


Time-Distance Helioseismology

DopplerVelocity


Filtergrams Time-distanceCross-covariance

functionWave travel times

Deep-focus v and cs

maps (0-200Mm)


maps (0-30Mm)


maps (0-30Mm)


Maps (0-30Mm)

Code: fastrackR.Bogart,T.DuvallJ.Zhao

Status: needs improvements (remapping issues)

Code: cross-covarianceT.DuvallJ.Zhao


Code: travel time fittingT.DuvallJ.ZhaoS.Couvidat


Code: sensitivity kernelsA.KosovichevJ.ZhaoA.Birch


Code: inversionsA.KosovichevJ.Zhao, A.BirchS.CouvidatJ.ToomreB.Hindman


Code: deep-focus mapsT.DuvallA.KosovichevJ.Zhao

Status: needs substantial development


Acoustic Holography

DopplerVelocity


Filtergrams Egression andIngression maps




maps (0-30Mm)

Code: fastrackR.BogartD.BraunC.Lindsay

Status: needs improvements (field-effect corrections)

Code: egression-ingressionD.BraunC.Lindsay


Code: phase shiftsD.Braun C.Lindsay

Status: needs improvements (showglass corrections)

Code: sensitivity kernelsA. Birch


Code:holographic inversionsA.Birch


Code: Far-side imagingP.ScherrerC.LindsayD.Braun


Inversions


Magnetic Fields

StokesI,VFiltergrams

StokesI,Q,U,V


Tracked Tiles








Code: Stokes I,V,Lev0.5 V & LOS fieldJ. SchouS. Tomzcyk


Code: Stokes I,Q,U,VJ. SchouS. Tomzcyk



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)


Code: LOS magnetic maps (project?)T. HoeksemaR. Bogart


Code: Synoptic Magnetic Field Maps T. HoeksemaX. ZhaoR. Ulrich


Code: Velocity Maps of Magnetic FootpointsY. LiuG. Fisher



Vector Magnetic Field

Filtergrams StokesI,Q,U,V


Tracked Tiles




Code: fastrackR. Bogart

Status: needs modifications for fields

Code: Vector Field Fast and Inversion AlgorithmsJ. SchouS. Tomzcyk


Code: Vector Field MapsT. HoeksemaY.Liu


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




Need $$


Intensity

Filtergrams ContinuumBrightness

Brightness Images

Code: Continuum MapsSchou


Code: Solar Limb Parameters, Lev0.5 used to make other Lev1 products, Lev2 for science goals

R. BushJ. Kuhn


Code: Brightness Feature Maps(European contribution)


Code: Averaged Continuum MapsBush


Solar limb parametersper image for Lev0.5

Brightness Synoptic Maps


Code: Brightness Synoptic MapsScherrer





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.


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)


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).

Page 1LWS Teams Day JSOC Overview HMI Data Products: Plan and Status.

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