HMI Science Analysis Plan Magnetic ShearTachocline Differential Rotation Meridional Circulation...

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 Helioseismolog

y 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

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 Magnetograms

Fast 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




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)


HMI DataData ProductProcessing

Level-0

Level-1

Magnetic FieldsStokes

I,VFiltergrams

StokesI,Q,U,V


Tracked Tiles


Vector MagnetogramsFast algorithm

Vector Magnetograms

Inversion algorithm





Code: Stokes I,V,Lev0.5 V & LOS field

J. SchouS. Tomzcyk

Status: in development

Code: Stokes I,Q,U,V

J. SchouS. Tomzcyk


HMI Vector Field Pipeline & Products

Calibration and Correction of Filtergrams

Magnetic ObservablesHMI Data

Increase s/n:Standard HMI resolutionRebinned data (retains temporal resolution)

Averaged data (retains spatial resolution)


180 Degree Ambiguity SolverFast (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

HMI Vector Field Pipeline & Products

Calibration and Correction of Filtergrams

Magnetic ObservablesHMI Data

Increase s/n:Standard HMI resolutionRebinned data (retains temporal resolution)

Averaged data (retains spatial resolution)


180 Degree Ambiguity SolverFast (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

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

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

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-request)(in a cadence of 2-minute)

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































SYNOPTIC PRODUCTS









SYNOPTIC PRODUCTS









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 magnetograms

J. SchouS. TomzcykR. Ulrich (cross calibration)


Code: LOS magnetic maps

T. HoeksemaR. Bogart


Code: Synoptic Magnetic Field Maps

T. HoeksemaE. Benevolenskaya X. ZhaoR. Ulrich


See Detail

Code: Velocity Maps of Magnetic Footpoints

Y. LiuG. Fisher

Status: Almost Ready to port

See Detail

Vector Magnetic FieldFiltergrams

StokesI,Q,U,V


Tracked Tiles

Vector MagnetogramsFast algorithm

Vector Magnetograms

Inversion algorithm




Code: fastrackR. Bogart

Status: needs modifications for fields

Code: Vector Field Fast and Inversion Algorithms

J. SchouS. Tomzcyk


Code: Vector Field Maps & Ambiguity Resolution

T. HoeksemaY.LiuKD Leka,CORA


See Details

Code: Coronal Field Extrapolations

T.HoeksemaY.Liu, X.ZhaoC. SchrijverS.T. Wu


Additional 2 FTE ?

See Details

Code: Coronal Magnetic Field Topological Properties

J.LinkerV. Titov

Status: needs implementation

Code: Solar Wind Models

X.ZhaoK.HayashiJ.LinkerS.T. Wu


0.5 FTE?

See Details

Needs additional FTEs

Coronal andSolar wind Properties

Surface Plasma Flows

HMI Science Analysis Plan – Magnetic Topics

Filtergrams


Vector Magnetograms


Coronal Magnetic FieldExtrapolations (non MHD)


Magnetic Data Products

MagneticObservables

HMI Data

THoeksema

YLiu

JBeck, YLiu,

XPZhao, KHayashi

YLiu, Schrijver

THoeksema, JSchou, HAO

YLiu, JSchou,*HAO

ContinuumBrightness

RBush, JSchou

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

5-2A Activity Complexes, Cycle

8-2D Irradiance Variations

19 Topology Structure over AR

Benevolenskaya, Bai

Hoeksema

Bai

Bush

Kosovichev

Kosovichev

Kosovichev

Beck

LM,Hayashi

YLiu

Hayashi, LM

YLiu LM

Schrijver, YLiu

XPZhao

Bai

Scherrer

Hayashi

Hayashi

??

20 B-Polar, Large/Small Int Benevolenskaya

Incomplete Magnetic Topic Group Affiliations (September, 2007)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

AIA Level-2

Backup Charts

Synoptic magnetic field maps

• Pipeline: synoptic magnetic field maps.

• Lead by: Todd & Xuepu.

• Task:

• Summary: based on line-of-sight magnetograms to generate synoptic maps of magnetic field.

• Input: remapped line-of-sight magnetograms.

• Output: Carrington synoptic charts (routine), synoptic frames with a cadence of as high as 1 minute (on-demand), evolved synoptic maps with a cadence of 16 minutes (routine).

• Code: at Stanford.

• Processors

• Status: almost ready to port. Already apply to MDI mags for Carrington rotation charts.

• Issues: some minor issues for synoptic frame and evolved maps.

Velocity maps of magnetic footpoints

• Pipeline: Velocity maps of magnetic footpoints.

• Lead by: UC Berkeley (Fisher & Brian) and Yang

• Task:

• Summary: based on the Local Correlation Tracking (LCT) technique, using time-series line-of-sight magnetograms to derive motion of magnetic footpoints.

• Input: time-series line-of-sight magnetograms.

• Output: velocity map with a cadence of 10 minutes. Generate on-demand and temporarily (?) stored.

• Code: LCT code developed by Fisher & Brian.

• Processors

• Status: almost ready to port. Already apply to MDI mags.

• Issues: some minor issues.

Vector magnetic field maps• Pipeline: vector magnetic field maps.

• Lead by: Todd & Yang & K.D. Leka.

• Task:

• Summary: based on algorithms (fast and slow) to solve 180-degree ambiguity, and to map the vector magnetic field on solar surface (spherical coordinates).

• Input: field strength, inclination, azimuth, and filling factor.

• Output: Br, B_theta, B_phi at a 5-minute cadence with fast algorithm (routine), 6-hour (?) cadence with slow algorithm, and 30-minute cadence with slow algorithm for active regions.

• Code: developed at Boulder.

• Processors

• Status: Codes for fast and slow algorithms are available.

• Issues: The code of slow algorithm is too slow, and loss of its author will lead an improvement very difficult. The code of fast algorithm works for Cartesian coordinate only. Need to extend to a spherical coordinate.

Coronal field extrapolation• Pipeline: coronal field extrapolation.• Lead by: Schrijver & Keiji & Yang• Task: • Summary: based on potential field and force free field models to compute

coronal field from vector magnetograms. Also seek possible MHD solutions.• Input: vector magnetograms for local regions and vector field synoptic maps.• Output: one global NLFFF solution (3D vector field) per day, one global MHD

solution (3D vector field) per day, one PFSS & HCCSSS solutions (3D vector field) per day. Global solutions and solutions(3D vector field) for local region with a cadence as high as the data temporary resolution (on-request).

• Code: Potential field codes at Stanford, NLFFF provided by Thomas Wiegelmann at Germany (in C, on a 4 processor machine, for 320x320x256, 4GB memory, 1 hour CPU time), global MHD solution at SAIC, local MHD code provided by Wu at Alabama (in Fortran, one processor, 15 CPU hours for 99x99x99; not allow parallel computation) (and Abbete at Berkeley ?)

• Processors: • Status: all codes are ready to port except MHD code for global solution with

vector field data as input.• Issues: global MHD simulation with vector field data as input needs to be

tested. better visualization tool is required.

Coronal & solar wind models• Pipeline: coronal & solar wind models.

• Lead by: Linker & Zhao & Hayashi

• Task:

• Summary: MHD simulation to model coronal structure (steady state) with vector field data as an input. Also seek dynamic solutions driven by time-series data. Empirical solar wind models from PFSS-like result computed from magnetic field synoptic maps (i.e. WSA model); MHD solar wind model from synoptic maps.

• Input: vector magnetograms for local regions and vector field synoptic maps.

• Output: 3D plasma data.

• Code: Potential field codes at Stanford, global MHD solution at SAIC, local MHD code provided by Wu at Alabama (in Fortran, one processor, 15 CPU hours for 99x99x99; not allow parallel computation) (and Abbete at Berkeley ?)

• Processors:

• Status:

• Issues:

Magnetic-Fields Pipeline

Status 11/5/2007

Vector Magnetic Field

• Lead – Todd Hoeksema, Yang Liu• Tasks

– Field inversion– Azimuth disambiguation– Vector magnetogram generation– Coordinate transformation and remapping– Calibration– Synoptic chart/ Synoptic frame generation– Potential field processing– MHD processing– NLFFF processing– Solar wind model processing

Vector Magnetic Field (cont’d.)

• Input– Lev 0 data from both vector and LOS cameras, rebinned

and averaged spatially/temporally – Dataseries names ???

• Level 1 Output– I, Q, U, V – data possibly saved in series, size is 16 MPx

ea. image– |B|, inclination, azimuth, filling factor – data saved in

series ???, size is 16 MB ea.– Cadence for all is ~ 3 min.– Coordinate-transformer module is a deliverable


• Level 2 Output– Synoptic charts – data saved in series ???, cadence ???,

size ???– Frames – data saved in series ???, cadence ???, size ???– Global potential field – data saved in series ???, cadence is

1 hr., size is small– Local potential field – data saved ???, cadence is on-

demand, size is ???– Low res global MHD – saved for short duration in series ???,

cadence is 1 day, size is ~ 1MB– Hi res global MHD – data saved ???, cadence is ???, size

is ???– Hi res local MHD – data saved ???, cadence is on-demand,

size is ???– MHD temporary/intermediate files – data saved for 2

weeks in series ???, size is 100 MB– Local NLFFF – data saved ???, cadence is on-demand, size

is ???– Solar wind models – data saved ???, cadence is ???, size

is ???


• Code– Rebin/avg module (Rick???)– inversion code from HAO (S. Tomczyk, but we create

module)– “fast” azimuth-disambiguation module (???)– “slow” azimuth-disambiguation module (Yang)– coordinate-transformation/remapping (Yang)– global potential field (Yang)– local potential field (Yang)– MHD (Keiji + SAIC)– NLFFF (Yang + Keiji)– Solar wind models (???)


• Processors– 32 (field inversion)– 8 (low-res global MHD)– 8 (hi-res local MHD), – ??? (slow disambiguation)– 2 (fast disambiguation)– 1 (rebinning/averaging), – ??? (coordinate transformation/remapping), – 1 (calibration), – 0 (hi-res global MHD – runs at CCMC), – ??? (NLFFF – 40 CPU hours)– ??? (Solar wind models)


• Status – ??? (how much is done), NLFFF algorithm selected (IDL and C implementation exist)

• Plan/Issues– Are we saving I, Q, U, V products? – Slow azimuth disambiguation algorithm TBD. – Coordinate-transformation/remapping algorithm TBD. – Calibration TBD. – Synoptic charts/frames TBD. – Global potential field processors and output data size

unknown. – Hi-res local MHD is TBD. – Is time-evolved data used for NLFFF?

LOS Magnetic Field

• Lead – Todd• Task – Generation of LOS magnetograms from lev 0 LOS

data, generation of calibrated, radial LOS magnetic field maps from LOS magnetograms, generation of synoptic charts and frames

• Input – Lev 0 data from LOS camera (dataseries ???)• Level 1 Output

– Calibrated magnetic field map – data saved in series ???, cadence is 48 seconds, size is 2 MB

• Level 2 Output– ~ 450 Radial images – data not saved, cadence is 1 day, size is

4 MB ea.– 9 Charts + 18 diagnostic images (incl. off center) – data saved

in series ???, cadence is 1 day, 7 MB ea.– Frames – data saved ???, cadence is on-demand, size is ???

LOS Magnetic Field (Cont’d)

• Code– Conversion to radial (Art) – MDI implementation exists– Remapping (Rick/Art) – MDI implementation exists– Chart creation (Keh-Cheng/Art) – MDI implementation

exists– Time-evolved chart creation (???)

• Processors – 1 (radialize), 1 (remapping), 1 (chart creation)

• Status – MDI implementation exists for all code, except time-evolved chart creation, needs porting to JSOC (remapping mostly ported, needs testing)

• Plan/Issues – MDI port complete in a couple of months; who is doing, time-evolved chart code, and by when?

HMI Science Analysis Plan Magnetic ShearTachocline Differential Rotation Meridional Circulation...

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