Transcript iv.   Magnetic Fields

HMI Magnetic Data
Summary
• Determining vector magnetic field is biggest
single computing challenge
– Problem is bounded
• Different anaylsis model than Doppler Data
– Not all data are analyzed to same degree
• Level 2 products are open ended
– Resolution, cadence, quality, algorithms
– Some in research state
HMI Data
HMI Science Analysis Plan
Processing
Data Product
Science Objective
Tachocline
Global
Helioseismology
Processing
Internal rotation Ω(r,Θ)
(0<r<R)
Internal sound speed,
cs(r,Θ) (0<r<R)
Differential Rotation
Local
Helioseismology
Processing
Full-disk velocity, v(r,Θ,Φ),
And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Activity Complexes
Filtergrams
Carrington synoptic v and cs
maps (0-30Mm)
Observables
Doppler
Velocity
High-resolution v and cs
maps (0-30Mm)
Deep-focus v and cs
maps (0-200Mm)
Far-side activity index
Line-of-sight
Magnetograms
Vector
Magnetograms
Continuum
Brightness
Line-of-Sight
Magnetic Field Maps
Meridional Circulation
Near-Surface Shear Layer
Active Regions
Sunspots
Irradiance Variations
Magnetic Shear
Flare Magnetic Configuration
Flux Emergence
Magnetic Carpet
Coronal energetics
Vector Magnetic
Field Maps
Large-scale Coronal Fields
Coronal magnetic
Field Extrapolations
Far-side Activity Evolution
Coronal and
Solar wind models
Brightness Images
Solar Wind
Predicting A-R Emergence
IMF Bs Events
JSOC - HMI Pipeline
Processing
HMI Data
Heliographic
Doppler velocity
maps
Filtergrams
Level-0
Doppler
Velocity
Spherical
Harmonic
Time series
To l=1000
Mode frequencies
And splitting
Ring diagrams
Local wave
frequency shifts
Time-distance
Tracked Tiles
Cross-covariance
Of Dopplergrams
function
Egression and
Ingression maps
Level-1
Data Product
Wave travel times
Wave phase
shift maps
Internal rotation Ω(r,Θ)
(0<r<R)
Internal sound speed,
cs(r,Θ) (0<r<R)
Full-disk velocity, v(r,Θ,Φ),
And sound speed, cs(r,Θ,Φ),
Maps (0-30Mm)
Carrington synoptic v and cs
maps (0-30Mm)
High-resolution v and cs
maps (0-30Mm)
Deep-focus v and cs
maps (0-200Mm)
Far-side activity index
Stokes
I,V
Line-of-sight
Magnetograms
Stokes
I,Q,U,V
Full-disk 10-min
Averaged maps
Vector Magnetograms
Fast algorithm
Tracked Tiles
Vector Magnetograms
Inversion algorithm
Coronal magnetic
Field Extrapolations
Tracked full-disk
1-hour averaged
Continuum maps
Solar limb parameters
Coronal and
Solar wind models
Brightness feature
maps
Brightness Images
Continuum
Brightness
HMI Data Analysis Pipeline
Line-of-Sight
Magnetic Field Maps
Vector Magnetic
Field Maps
Magnetic Fields
Filtergrams
Stokes
I,V
Line-of-sight
Magnetograms
Stokes
I,Q,U,V
Full-disk 10-min
Averaged maps
Vector Magnetograms
Fast algorithm
Tracked Tiles
Vector Magnetograms
Inversion algorithm
Line-of-Sight
Magnetic Field Maps
Vector Magnetic
Field Maps
Coronal magnetic
Field Extrapolations
Coronal and
Solar wind models
Code: Stokes I,V,
Lev0.5 V & LOS
field
J. Schou
S. Tomzcyk
Status: in
development
Code: Stokes
I,Q,U,V
J. Schou
S. Tomzcyk
Status: in
development
HMI Vector Field Pipeline & Products
Increase s/n:
 Standard HMI resolution
 Rebinned data
(retains temporal resolution)
 Averaged data
(retains spatial resolution)
Magnetic Observables
HMI Data
Filtergrams
Stokes I, Q, U, and V;
Vector Magnetograms
(|B|, inclination,
azimuth, …)
Vector Magnetic
Field Maps
Field Inversion
Calibration and
Correction of
Filtergrams
180 Degree Ambiguity Solver


Fast (potential or lfff);
Slower but better.
Vector magnetic field in active regions:
In heliographic coordinates
In image coordinates
Full disk vector magnetic field:
In image coordinates
In spherical coordinates
Synoptic maps of vector field
(B_r, B_theta, B_phi):
Standard synoptic charts;
Synoptic frames;
Daily update synoptic maps.
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
“Ambiguous” Observables
Magnetograms (standard)
(full disk, full resolution,
10-minute cadence?)
Magnetograms (standard)
(full disk, full resolution,
1-hour average)
VECTOR MAGNETIC MAPS
Full disk vector field maps (standard)
(full resolution, 10-minute cadence)
Full disk vector field maps (standard)
(full resolution, 6-hour cadence)
Magnetograms (on-request)
(full disk, full resolution,
2-minute cadence)
Synoptic frame (standard)
(in a cadence of 1-day)
Daily update Synoptic map (standard)
(in a cadence of 1-day)
Vector magnetic field maps in AR patches (standard)
(in heliographic coord., full res., 6-hour cadence)
Synoptic map (standard)
1-hour average vector magnetic field maps (standard)
(full disk, full resolution, 6-hour cadence)
Magnetograms (on-request)
(AR patches, full resolution,
2-minute cadence)
SYNOPTIC PRODUCTS
Vector magnetic field maps (on-demand)
(full disk, full resolution, 30-minute cadence)
Synoptic frame (on-demand)
(in a cadence of 30-minute)
Synoptic frame (on-demand)
(in a cadence of 30-minute)
Vector magnetic field maps (on-demand)
(AR patches, full resolution, 30-minute cadence)
Daily update Synoptic map (on-demand)
(in a cadence of 30-minute)
Vector magnetic field maps (on-request)
(full disk, full resolution, 2-minute cadence)
Synoptic frame (on-request)
(in a cadence of 2-minute)
Stokes I, Q, U and V (on-request).
Vector magnetic field maps (on-request)
(AR patches, full resolution, 2-minute cadence)
Daily update Synoptic map (on-request)
(in a cadence of 2-minute)
Magnetic Processing Scheduling
Three kinds of processing scheduling
• Standard
– Routinely completed for all data on regular
cadence (e.g. Vector B)
• On Demand
– Completed 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 Request
– Completed when system resources allow
Line-of Sight Magnetic Field
Filtergrams
Stokes
I,V
Line-of-sight
Magnetograms
Line-of-Sight
Magnetic Field Maps
Synoptic
Magnetic Field Maps
Magnetic Footpoint
Velocity Maps
Code: LOS
magnetograms
Code: LOS
magnetic maps
J. Schou
S. Tomzcyk
R. Ulrich (cross
calibration)
T. Hoeksema
R. Bogart
Status: in
development
Status: in
development
Code: Synoptic
Magnetic Field
Maps
Code: Velocity
Maps of Magnetic
Footpoints
T. Hoeksema
E. Benevolenskaya
X. Zhao
R. Ulrich
Y. Liu
G. Fisher
Status: in
development
See Detail
Status: Almost
Ready to port
See Detail
Vector Magnetic Field
Filtergrams
Stokes
I,Q,U,V
Full-disk 10-min
Averaged maps
Tracked Tiles
Vector Magnetic
Field Maps
Vector Magnetograms
Fast algorithm
Vector Magnetograms
Inversion algorithm
Coronal magnetic
Field Extrapolations
Coronal and
Solar wind models
Code: fastrack
R. Bogart
Status: needs
modifications
for fields
Code: Vector
Field Fast and
Inversion
Algorithms
J. Schou
S. Tomzcyk
Status: in
development
Code: Vector
Field Maps &
Ambiguity
Resolution
T. Hoeksema
Y.Liu
KD Leka,CORA
Status: in
development
Code: Coronal
Field
Extrapolations
T.Hoeksema
Y.Liu, X.Zhao
C. Schrijver
S.T. Wu
Status: in
development
Code: Solar
Wind Models
X.Zhao
K.Hayashi
J.Linker
S.T. Wu
Status: in
development
Code: Coronal
Magnetic Field
Topological
Properties
J.Linker
V. Titov
Status: needs
implementation
0.5 FTE?
See Details
Additional 2 FTE ?
See Details
See Details
Needs additional FTEs
Vector Magnetic Field
Processor Summary
• Processors
–
–
–
–
–
–
–
–
–
–
–
32 (field inversion)
8 (low-res global MHD)
8 (hi-res local MHD),
<10 (slow disambiguation)
~2 (fast disambiguation)
<1 (rebinning/averaging),
??? (coordinate transformation/remapping),
<1 (calibration),
0 (hi-res global MHD – runs at CCMC),
??? (NLFFF) – on demand/request - 40 CPU hours per run
<1 (Solar wind models)
HMI Science Analysis Plan – Magnetic Topics
HMI Data
Filtergrams
Magnetic
Observables
Magnetic Data
Products
Line-of-Sight
Magnetic Field Maps
THoeksema
Line-of-sight
Magnetograms
Vector Magnetic
Field Maps
YLiu
THoeksema,
JSchou, HAO
Vector
Magnetograms
YLiu, JSchou,
*HAO
1-1A Tachocline
Kosovichev
2-1C Meridional Circulation
Kosovichev
3-1B Differential Rotation
Kosovichev
4-1D Near-Surface Shear Layer
Beck
5-2A Activity Complexes, Cycle
Benevolenskaya, Bai
6-2B Active Regions
Hoeksema
7-2C Sunspots
Bai
8-2D Irradiance Variations
Bush
9-3A Magnetic Shear
YLiu
10-3B Flare/CME Mag. Config
LM,Hayashi
Coronal Magnetic Field
Extrapolations (non MHD)
11-3C Flux Emergence
YLiu LM
YLiu, Schrijver
12-3D Magnetic Carpet+Heating
Hayashi, LM
13-4A Coronal Energetics AIA]1
Schrijver, YLiu
14-4B Large-scale B, Ph+Cor
Hayashi
15-4C Solar Wind + Evol, Struct
Hayashi
16-5A Far-side Activity Evolution
Scherrer
Surface Plasma Flows
JBeck, YLiu,
17-5B Predicting A-R Emergence Bai
Continuum
Brightness
RBush, JSchou
Coronal and
Solar wind Properties
XPZhao, KHayashi
18-5C IMF Bs Events
XPZhao
19 Topology Structure over AR
??
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
Details Charts
Velocity maps of magnetic
footpoints
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•
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
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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), 6hour (?) 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.
Synoptic magnetic field maps
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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.
Coronal & solar wind models
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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 timeseries 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:
Coronal field extrapolation
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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.
Magnetic-Fields Pipeline
Status 11/5/2007
Vector Magnetic Field
• Lead – Todd Hoeksema, Yang Liu
• Task
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Field inversion
Azimuth disambiguation
Vector magnetogram generation
Coordinate transformation and remapping
Calibration
Synoptic chart/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, aligned, rebinned and
averaged spatially/temporally
– Dataseries names TBD
• Level 1 Output
– I, Q, U, V – data possibly saved in series \ size is 16 MPixels ea.
– |B|, inclination, azimuth, filling factor – data saved in series TBD, size
is 16 MPx ea.
– Cadence for all is ~ 3 min.
– Coordinate-transformer module is a deliverable
Vector Magnetic Field (cont’d.)
• Level 2 Output
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Synoptic charts – data saved in series, cadence few per day, size 50 MPx
Frames – data saved in series, cadence hourly/varies, size 16Mpx
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 small
Low res global MHD – saved for short durations in series, cadence is 1
day, size is ~ 1MB
Hi res global MHD – data saved, cadence is few per month, size is small
Hi res local MHD – data saved, cadence is on-demand, size is moderate
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 moderate
Solar wind models – data saved, cadence is few per day, size is small
Vector Magnetic Field (cont’d.)
• Code
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Rebin/avg module (Rick?)
inversion code from HAO (S. Tomczyk, but we create module)
“fast” azimuth-disambiguation module (Yang, Leka/CORA)
“slow” azimuth-disambiguation module (Yang, Leka/CORA)
coordinate-transformation/remapping (Yang)
global potential field (Yang)
local potential field (Yang)
MHD (Keiji + SAIC)
NLFFF (Yang + Keiji)
Solar wind models (Todd + Yang)
Vector Magnetic Field (cont’d.)
• Processors
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32 (field inversion)
8 (low-res global MHD)
8 (hi-res local MHD),
<10 (slow disambiguation)
~2 (fast disambiguation)
<1 (rebinning/averaging),
??? (coordinate transformation/remapping),
<1 (calibration),
0 (hi-res global MHD – runs at CCMC),
??? (NLFFF) – on demand/request - 40 CPU hours per run
<1 (Solar wind models)
Vector Magnetic Field (cont’d.)
• Status – (how much is done), a NLFFF algorithm selected (IDL
and C implementations exist)
• Plan/Issues
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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
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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 16 MPx
•
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 hourly/on-demand, size is ???
LOS Magnetic Field (Cont’d)
• Code
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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 timeevolved 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 schedule TBD?