HMI Science Analysis. Primary Goal: Origins of Solar Variability The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study

HMI Science Analysis

Primary Goal: Origins 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 HMI science problems

• Dynamo and activity cycle

• Emergence and evolution of AR

• Energetics and triggering of flares

and CMEs

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 Major Science ObjectivesSolar Dynamo

Global Circulation

Irradiance Sources

Far-side Imaging

Solar Subsurface Weather

Coronal Magnetic Field

Magnetic Connectivity

Sunspot Dynamics

Magnetic Stresses

Interior Structure

NOAA 9393

Far-side

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

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

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 …)

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


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





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

Egression andIngression maps

Time-distanceCross-covariance

function

Ring diagrams


Wave travel times

Local wave frequency shifts


Deep-focus v and cs

maps (0-200Mm)


maps (0-30Mm)


maps (0-30Mm)


Maps (0-30Mm)


HeliographicDoppler velocity

maps

SphericalHarmonic




Global helioseismology

Code: projectJ. Schou

Status: ready to port

Code: qdotprodJ.Schou


Code: peak baggingJ.Schou


Code: sound-speed inversionsA.Kosovichev


Code: rotation inversionJ.SchouR. Howe


DopplerVelocity

Filtergrams

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

Doppler velocitymaps

SphericalHarmonic




DopplerVelocity

Tracked TilesOf DopplergramsFiltergrams

Ring diagramsLocal wave

frequency shifts


maps (0-30Mm)


Maps (0-30Mm)

Ring Diagrams

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


Additional funding: 0.5 FTE

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


Additional funding:0.75 FTE

Total Needed : 2 FTE

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)

Time-Distance Helioseismology

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



Total Need: 1.5 FTE

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

Status: needs substantial development

Additional funding: 1FTE

DopplerVelocity


Filtergrams Egression andIngression maps




maps (0-30Mm)

Acoustic Holography

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 (shower glass corrections)

Code: sensitivity kernelsA. Birch


Code:holographic inversionsA.Birch


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


Inversions

Magnetic FieldsStokes

I,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 FieldStokes

I,VFiltergrams

Line-of-sightMagnetograms Line-of-Sight

Magnetic Field Maps

SynopticMagnetic Field Maps

Magnetic Footpoint Velocity Maps

Code: LOS magnetogramsJ. SchouS. Tomzcyk


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


Code: Synoptic Magnetic Field Maps T. HoeksemaX. ZhaoE. Benevolenskaya


Code: Velocity Maps of Magnetic FootpointsY. LiuG. Fisher


Additional funding: TBD

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 T.HoeksemaY.Liu, X.ZhaoC. SchrijverP.Goode K.D.Leka


Additional funding: 2 FTE

Code: Coronal Magnetic Field Topological PropertiesJ.LinkerV. Titov

Status: needs implementation

Code: Solar Wind ModelsX.ZhaoK.HayshiJ.LinkerP.GoodeV.Yurchishin


0.5 FTE

Total Need: 2.5 FTE

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

Tracked full-disk1-hour averagedContinuum maps

Code: Brightness Synoptic MapsScherrer


Solar limb parameters

Brightness featuremaps

Coronal andSolar wind Properties

Surface Plasma Flows

HMI Science Analysis Plan – Magnetic Topics

9-3A Magnetic Shear

1-1A Tachocline

3-1B Differential Rotation

2-1C Meridional Circulation

4-1D Near-Surface Shear Layer

6-2B Active Regions

7-2C Sunspots

12-3D Magnetic Carpet+Heating

10-3B Flare/CME Mag. Config

11-3C Flux Emergence

13-4A Coronal Energetics AIA]1

14-4B Large-scale B, Ph+Cor

15-4C Solar Wind + Evol, Struct

16-5A Far-side Activity Evolution

17-5B Predicting A-R Emergence

18-5C IMF Bs Events

Filtergrams


Vector Magnetograms


Coronal Magnetic FieldExtrapolations (non MHD)


Magnetic Data Products

MagneticObservables

HMI Data

5-2A Activity Complexes, Cycle

8-2D Irradiance Variations

19 Topology Structure over AR

THoeksema

YLiu

Benevolenskaya, Bai

Hoeksema

Bai

Bush

JBeck, YLiu,

XPZhao, KHayashi

YLiu, Schrijver

Kosovichev

Kosovichev

Kosovichev

Beck

LM,Hayashi

YLiu

Hayashi, LM

YLiu LM

Schrijver, YLiu

XPZhao

Bai

Scherrer

Hayashi

Hayashi

??

THoeksema, JSchou, HAO

YLiu, JSchou,*HAO

ContinuumBrightness

RBush, JSchou 20 B-Polar, Large/Small Int Benevolenskaya

Incomplete Magnetic Topic Group Affiliations (Please Sign Up!!)Tachocline - AKosovichev

Meridional Circulation - AKosovichev

Differential Rotation - AKosovichev

Near-surface Shear Layer - JBeck

Activity Complexes – Benevolenskaya, Bai, Hoeksema, Hayashi, Hurlburt, Gaizauskus, JHarvey

Active Regions – THoeksema, EBenevolenskaya, TBai, KHayashi, NHurlburt

Sunspots – TBai, THoeksema, EBenevolenskaya, NHurlburt

Irradiance Variations – RBush, TBerger, PBoerner

Magnetic Shear – YLiu, JBeck, KHayashi, AKosovichev, VYurchyshyn

Flare/CME Magnetic Config – Hayashi, LM, YLiu, XPZhao, Bai, Kosovichev, UC-B, HWang

Flux Emergence – YLiu, JBeck, Benevolenskaya, Hayashi, LM, BLites, Leka, HWang

Mag. Carpet & Heating [AIA#1] – KHayashi, KSchrijver, JBeck, EBenevolenskaya

Coronal Energetics [AIA] – KSchrijver, YLiu, Benevolenskaya, XPZhao, Hayashi, Leka, MCheung, UC-B, HWang

Large-scale B – Ph. + Cor. - KHayashi, THoeksema, EBenevolenskaya, XPZhao

Solar Wind – Evol+Struct. - Hayashi, Hoeksema, XPZhao, MWSO, CISM, Fuselier, Mikic

Far-side Activity – PScherrer, CLindsey, DBraun, SAIC

Predicting AR Emergence - TBai

IMF Bs Events – XPZhao, YLiu, KHayashi, VYurchyshyn, Hu, SFuselier, ZMikic

Magnetic Topology – YLiu, MSU-DLongcope, Barnes, SAIC-Titov

Polar & Multi-scale Field – EBenevolenskaya, THoeksema

Summary

Needs

Helioseismology

Global helioseismology

Ring Diagrams 2.0 FTE

Time-Distance Helioseismology 1.5 FTE

Magnetic Fields

Vector Magnetic Field 2.5 FTE

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).

Documents

HMI Science Analysis. Primary Goal: Origins of Solar Variability The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study