Science Objectives, Observables, and Magnetic Data Product Teams

Preliminary Magnetic Topic Group AffiliationsPlease Participate!

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, A. Pevtsov•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] – 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

The Helioseismic & Magnetic Imager – Magnetic Field Data Products

The Helioseismic and Magnetic Imager (HMI) instrument on the Solar Dynamic Observatory (SDO) spacecreaft will begin observing the solar photospheric magnetic field continuously after launch and commissioning in early 2009. This paper describes the HMI magnetic processing pipeline and the expected data products that will be available. The full-disk line-of-sight magnetic field will be available every 45 seconds with 1” resolution. Comparable vector measurements collected over a three-minute time interval will ordinarily be averaged for at least 10 minutes before inversion.

Useful Quick-Look products intended only for forecasting and planning purposes will be available a few minutes after observation.

Standard final science data products will be computed within 36 hours and made available through the SDO Joint Science Operations Center (JSOC). Three kinds of magnetic science data products have been defined – standard, on-demand, and on-request.

Standard products, such as frequently updated synoptic charts, are made all the time on a fixed cadence.

On-demand products, such as high-cadence full-disk disambiguated vector magnetograms, will be generated whenever a user asks for them.

On-request products, such as high-resolution time serieos of MDH model solutions, will be generated as resources allow. This paper describes the observations, magnetograms, synoptic, and synchronic products, and field model calculations that will produced by the HMI magnetic pipeline.

The Helioseismic & Magnetic Imager – Magnetic Field Data ProductsJ. Todd Hoeksema for the HMI Magnetic Team

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

Lundstedt

THoeksema, JSchou, HAO

YLiu, JSchou,*HAO, CORA

ContinuumBrightness

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

HMI Vector Field Pipeline & Products

Calibration and Correction of Filtergrams

Magnetic Observables

HMI 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 (10m)

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

(|B|, inclination, azimuth, …)

Filtergrams

SYNOPTIC PRODUCTSSYNCHRONIC PRODUCTS

Synoptic & Synchronic maps (CR, standard)

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

Daily update Synoptic & Synchronic maps (standard cadence of 1-day)

Synoptic frame (on-demand)Synchronic frame (on-demand)

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

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

Synoptic or Synchronic 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

Quick Look Observables – HMI Magnetic Field Images

One Minute (Doppler cadence, ~45 seconds)•1-minute line-of-sight velocity•1-minute line-of-sight magnetic field (or Br or signed total l-o-s mean field)•1-minute continuum intensity•1-minute indices, movies computed from the above

10-Minute (fastest vector field cadence averaged over 6 cycles, 90s*6)

•10-minute global quick-look inversions•inversion method may depend on flux/noise•map of inversion method provided•selected rectangular patches will be disambiguated

•indices for patches computed from 10-minute field values

1-hour•Synoptic maps of B_r at lower resolution (1-degree, tbd)•Vector field updated only in patches

6-hour•Quick-look full-disk disambiguated vector field

Science Data Products – HMI Magnetic Field Images

PipelineOne-minute

signed |Br| on full diskmagnetic line-of-sight velocity on full diskcontinuum intensity on full disk

10-minuteinverted B on full diskdisambiguated B on selected patches

3-hourdisambiguated vector field on full disk, use QL results as appropriate

On Demand• 3-second level 1.5 filtergrams (limited number)• 3-minute (180-second) spatially binned disambiguated vector field in patches• 6-minute (360-second) disambiguated patches• 10-minute full disk disambiguated vector field

On Request• 100-second disambiguated patches• 100-second IQUV• Anything else

Dataflow (GB/day)

Joint Ops

ScienceArchive440TB/yr(Offiste)

Data Capture

2 processors each

1230

1610

HMI &AIA Science

Hk

0.04

30d cache40TB each

Quick Look

LMSAL secure host

Level 0(HMI & AIA)

2 processors

75

Level 1(HMI)

16 processors

Online Data

325TB+50TB/yr

HMI High LevelProcessingc. 200 processors

HMI Science Analysis Archive 650TB/yr

Redundant data capture system

1210

1210

Data Exports

1200

LMSAL Link(AIA Level 0, HMI Magnetograms)

240

1610

1820

1230

rarelyneeded

1230

2 processorsSDO Scientist &User Interface

Dataflow (GB/day)

Joint Ops

ScienceArchive440TB/yr(Offiste)

Data Capture

2 processors each

1230

1610

HMI &AIA Science

Hk

0.04

30d cache40TB each

Quick Look

LMSAL secure host

Level 0(HMI & AIA)

2 processors

75

Level 1(HMI)

16 processors

Online Data

325TB+50TB/yr

HMI High LevelProcessingc. 200 processors

HMI Science Analysis Archive 650TB/yr

Redundant data capture system

1210

1210

Data Exports

1200

LMSAL Link(AIA Level 0, HMI Magnetograms)

240

1610

1820

1230

rarelyneeded

1230

2 processorsSDO Scientist &User Interface

Magnetic Processing Scheduling

There are four schedules for Magnetic Field data processing

Quick LookRoutine processing on data available within minutes of observation

StandardRoutinely completed for all data on regular

cadence (e.g. Vector B)

On DemandCompleted for small fraction of data when

interesting things happen or whenever requested by a qualified user (HiRes MHD time series for a big flare & CME campaign

On RequestCompleted when system resources allow

SP51B-13

Magnetic Field Model ProductsProduced as Standard, On-demand, andOn-request products

Automated Identification of AR PatchesPFSS Model – various resolutionsNLFFF Model – AR patches only, dailyMHD Models – daily low-resolution

– Monthly major events in hi-resOpen Field Foot Point MapsSurface Flow Maps – ILCT, DAVE

HMI after delivery to GSFC

HMI Complete and Awaiting Integration onto SDO

Vector magnetic quantities: |B|, filling factor, inclination to l-o-s, azimuth, magnetic velocity, & uncertainties.