Science Objectives, Observables, and Magnetic Data Product TeamsPreliminary Magnetic Topic Group Affiliations

(Please Sign Up!!)Observables

•Line-of-sight magnetograms – THoeksema, JSchou, HAO, KD Leka•Vector magnetograms – YLiu, JSchou, HAO, SCouvidat, KD Leka•Continuum Brightness – RBush?, JSchou, NHurlburt, TBerger, PBoerner, JKuhn

Magnetic Data Products•Line of sight magnetic maps – THoeksema, EBenevolenskaya, TBai•Vector field maps – YLiu, THoeksema, EBenevolenskaya, ANorton, KD Leka, Blites, BBSO-JJing, VYurchyshyn•Coronal field extrapolations [AIA] – YLiu, KSchrijver, XPZhao, KHayashi, LM-MCheung•Coronal & Solar Wind – XPZhao, KHayashi, THoeksema, SAIC-Linker•Surface Plasma Flows – JBeck, YLiu, KHayashi, EBenevolenskaya, TBai, BWelsh, STWu, RShine, BDePontieu, TBerger, SAIC-Linker

Science Objectives•1-1A – Tachocline - AKosovichev•2-1C – Meridional Circulation - AKosovichev•3-1B – Differential Rotation - AKosovichev•4-1D – Near-surface Shear Layer - JBeck•5-2A – Activity Complexes – EBenevolenskaya, TBai, THoeksema, KHayashi, NHurlburt, VGaizauskus, JHarvey•6-2B – Active Regions – THoeksema, EBenevolenskaya, TBai, KHayashi, NHurlburt•7-2C – Sunspots – TBai, THoeksema, EBenevolenskaya, NHurlburt •8-2D – Irradiance Variations – RBush, TBerger, PBoerner•9-3A – Magnetic Shear – YLiu, JBeck, KHayashi, AKosovichev, BBSO-VYurchyshyn•10-3B – Flare/CME Magnetic Config – KHayashi, LM?, YLiu, XPZhao, TBai, AKosovichev, UC-B,BBSO-HWang•11-3C – Flux Emergence – YLiu, JBeck, EBenevolenskaya, LHayashi, LM, BLites, KD Leka, BBSO-HWang•12-3D – Mag. Carpet & Heating [AIA#1] – KHayashi, KSchrijver, JBeck, EBenevolenskaya•13-4A – Coronal Energetics [AIA] – KSchrijver, YLiu, EBenevolenskaya, XPZhao, KHayashi, KD Leka, MCheung, UC-B,BBSO HWang•14-4B – Large-scale B – Ph. + Cor. - KHayashi, THoeksema, EBenevolenskaya, XPZhao•15-4C – Solar Wind – Evol. + Struct. - KHayashi, THoeksema, XPZhao, MWSO, CISM, LM-SFuselier, SAIC-ZMikic•16-5A – Far-side Activity – PScherrer, CLindsey, DBraun, SAIC•17-5B – Predicting AR Emergence - TBai•18-5C – IMF Bs Events – XPZhao, YLiu, KHayashi, BBSO-VYurchyshyn, Hu, HINODE, LM-SFuselier, SAIC-ZMikic•19 – Magnetic Topology – YLiu, MSU-DLongcope, Barnes, SAIC-Titov•20 – Polar & Multi-scale Field – EBenevolenskaya, THoeksema

ABSTRACT

The HMI investigation will study the origin of solar variability and will characterize and understand the Sun’s interior and the various components of magnetic activity.

Teams are forming to address the principle scientific goals of the mission. These topics, outlined in the HMI Science Plan (http://hmi.stanford.edu/doc/Science_Plan/HMI_Science_Plan.pdf) encompass a broad range of science that will be enabled by

HMI magnetic field observations. The Co-I team desperately needs your participation to take full advantage of the opportunities provided.

Polarized filtergrams around the Fe I spectral line at 617.3 nm made with the HMI tunable narrow band filter enable determination of all three components of the vector photospheric magnetic field in half arc second pixels with a cadence of five minutes at all times.

Development of pipeline processing modules to produce the full menu of data products is currently underway. The final data products are presently being defined. Some STANDARD products will be computed at all times, others will be produced On DEMAND or during times of special interest. Some data products requiring intensive processing will only be produced On REQUEST when resources allow.

The Helioseismic & Magnetic Imager – Magnetic InvestigationsJ.Todd Hoeksema for the HMI Magnetic Team

HMI Sun Testing- Early Images

First Dopplergram First Magnetogram

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 ProductHMI Data Processing

Level-1

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

Line-of-sightMagnetograms

Vector Magnetograms

Line-of-SightMagnetic Field Maps

Coronal Magnetic FieldExtrapolations (non MHD)

Vector MagneticField Maps

Magnetic Data Products

MagneticObservables

HMI Data

5-2A Activity Complexes, Cycle

8-2D Irradiance Variations

19 Topology Structure over AR

THoeksema

YLiu

EBenevolenskaya, TBai

THoeksema

TBai

RBush

JBeck, YLiu,

XPZhao, KHayashi

YLiu, Schrijver

AKosovichev

AKosovichev

AKosovichev

JBeck

LM, KHayashi

YLiu

KHayashi, LM

YLiu, LM

Schrijver, YLiu

XPZhao

TBai

PScherrer

KHayashi

KHayashi

??

THoeksema, JSchou, HAO

YLiu, JSchou,*HAO

ContinuumBrightness

RBush, JSchou20 B-Polar, Large/Small Int EBenevolenskay

HMI Vector Field Pipeline & Products

Calibration and Correction of Filtergrams

Magnetic ObservablesHMI Data

Increase s/n: Standard HMI resolution Rebinned data (retains temporal resolution) Averaged data (retains spatial resolution)

Vector MagneticField Maps

180 Degree Ambiguity Solver Fast (potential or lfff); Slower but better.

Full disk vector magnetic field:In image coordinatesIn spherical coordinates

Vector magnetic field in active regions:In heliographic coordinatesIn image coordinates

Synoptic maps of vector field(B_r, B_theta, B_phi):

Standard synoptic charts;Synoptic frames;Daily update synoptic maps.

Field Inversion

Stokes I, Q, U, and V;Vector Magnetograms

(|B|, inclination, azimuth, …)

Filtergrams

VECTOR MAGNETIC MAPS

Full disk vector field maps (standard)(full resolution, 10-minute cadence)

Vector magnetic field maps (on-request)(full disk, full resolution, 2-minute cadence)

Vector magnetic field maps (on-request)(AR patches, full resolution, 2-minute cadence)

Full disk vector field maps (standard)(full resolution, 6-hour cadence)

1-hour average vector magnetic field maps (standard)(full disk, full resolution, 6-hour cadence)

Vector magnetic field maps in AR patches (standard)(in heliographic coord., full res., 6-hour cadence)

Vector magnetic field maps (on-demand)(full disk, full resolution, 30-minute cadence)

Vector magnetic field maps (on-demand)(AR patches, full resolution, 30-minute cadence)

“Ambiguous” Observables

Magnetograms (standard)(full disk, full resolution,10-minute cadence?)

Magnetograms (on-request)(full disk, full resolution, 2-minute cadence)

Stokes I, Q, U and V (on-request).

Magnetograms (on-request)(AR patches, full resolution,2-minute cadence)

Magnetograms (standard)(full disk, full resolution,1-hour average)

SYNOPTIC PRODUCTS

Synoptic map (standard)

Synoptic frame (standard)(in a cadence of 1-day)

Daily update Synoptic map (standard)(in a cadence of 1-day)

Synoptic frame (on-demand)(in a cadence of 30-minute)

Daily update Synoptic map (on-demand)(in a cadence of 30-minute)

Synoptic frame (on-demand)(in a cadence of 30-minute)

Synoptic frame (on-request)(in a cadence of 2-minute)

Daily update Synoptic map (on-request)(in a cadence of 2-minute)

HINODE Spectropolarimetric Magnetic Field Inverted with HMI-like Algorithm by S. Tomczyk & J. Borrero (HAO)The three panels show Inclination, Azimuth & Magnetic Field Strength as observed May 7, 2007

0 180 -180 180 0 3097