HMI Magnetic Data Summary

1
HMI Magnetic DataSummary

• 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

2
HMI Science Analysis Plan
Data Product
Processing
HMI Data
Science Objective
Tachocline
Global Helioseismology Processing
Internal rotation O(r,T) (0ltrltR)
Meridional Circulation
Filtergrams
Internal sound speed, cs(r,T) (0ltrltR)
Differential Rotation
Near-Surface Shear Layer
Full-disk velocity, v(r,T,F), And sound speed,
cs(r,T,F), Maps (0-30Mm)
Local Helioseismology Processing
Activity Complexes
Active Regions
Carrington synoptic v and cs maps (0-30Mm)
Sunspots
Irradiance Variations
High-resolution v and cs maps (0-30Mm)
Observables
Magnetic Shear
Deep-focus v and cs maps (0-200Mm)
Flare Magnetic Configuration
Flux Emergence
Far-side activity index
Magnetic Carpet
Line-of-Sight Magnetic Field Maps
Coronal energetics
Large-scale Coronal Fields
Vector Magnetic Field Maps
Solar Wind
Coronal magnetic Field Extrapolations
Far-side Activity Evolution
Predicting A-R Emergence
Coronal and Solar wind models
IMF Bs Events
Brightness Images
3
JSOC - HMI Pipeline
Data Product
Processing
HMI Data
Internal rotation O(r,T) (0ltrltR)
Spherical Harmonic Time series To l1000
Heliographic Doppler velocity maps
Filtergrams
Mode frequencies And splitting
Internal sound speed, cs(r,T) (0ltrltR)
Full-disk velocity, v(r,T,F), And sound speed,
cs(r,T,F), Maps (0-30Mm)
Local wave frequency shifts
Ring diagrams
Doppler Velocity
Level-0
Carrington synoptic v and cs maps (0-30Mm)
Time-distance Cross-covariance function
Tracked Tiles Of Dopplergrams
Wave travel times
High-resolution v and cs maps (0-30Mm)
Egression and Ingression maps
Wave phase shift maps
Deep-focus v and cs maps (0-200Mm)
Far-side activity index
Stokes I,V
Line-of-sight Magnetograms
Level-1
Line-of-Sight Magnetic Field Maps
Stokes I,Q,U,V
Full-disk 10-min Averaged maps
Vector Magnetograms Fast algorithm
Vector Magnetic Field Maps
Vector Magnetograms Inversion algorithm
Coronal magnetic Field Extrapolations
Tracked Tiles
Tracked full-disk 1-hour averaged Continuum maps
Coronal and Solar wind models
Continuum Brightness
Solar limb parameters
Brightness Images
Brightness feature maps
HMI Data Analysis Pipeline
4
Magnetic Fields
Vector Magnetic Field Maps
5
(No Transcript)
6
(No Transcript)
7
(No Transcript)
8
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

9
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
10
Vector Magnetic Field
Vector Magnetic Field Maps
Filtergrams
Stokes I,Q,U,V
Full-disk 10-min Averaged maps
Vector Magnetograms Fast algorithm
Coronal magnetic Field Extrapolations
Vector Magnetograms Inversion algorithm
Tracked Tiles
Coronal and Solar wind models
Needs additional FTEs
11
Vector Magnetic Field Processor Summary

• Processors
• 32 (field inversion)
• 8 (low-res global MHD)
• 8 (hi-res local MHD),
• lt10 (slow disambiguation)
• 2 (fast disambiguation)
• lt1 (rebinning/averaging),
• ??? (coordinate transformation/remapping),
• lt1 (calibration),
• 0 (hi-res global MHD runs at CCMC),
• ??? (NLFFF) on demand/request - 40 CPU hours
  per run
• lt1 (Solar wind models)

12
HMI Science Analysis Plan Magnetic Topics
HMI Data
Filtergrams
Magnetic Data Products
Line-of-Sight Magnetic Field Maps
Magnetic Observables
THoeksema
Line-of-sight Magnetograms
Vector Magnetic Field Maps
YLiu
THoeksema, JSchou, HAO
Coronal Magnetic Field Extrapolations (non MHD)
YLiu, Schrijver
Vector Magnetograms
YLiu, JSchou, HAO
Surface Plasma Flows
JBeck, YLiu,
Continuum Brightness
Coronal and Solar wind Properties
RBush, JSchou
XPZhao, KHayashi
13

• 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 AIA1 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 EvolStruct. - 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

14
AIA Level-2
15
Details Charts
16
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.

17
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.

18
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.

19
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

20
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.

21
Magnetic-Fields Pipeline

• Status 11/5/2007

22
Vector Magnetic Field

• Lead Todd Hoeksema, Yang Liu
• Task
• 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

23
Vector Magnetic Field (contd.)

• Input
• Lev 0 data from both vector and LOS cameras,
  aligned, rebinned and averaged spatially/temporall
  y
• 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

24
Vector Magnetic Field (contd.)

• Level 2 Output
• 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

25
Vector Magnetic Field (contd.)

• Code
• 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)

26
Vector Magnetic Field (contd.)

• Processors
• 32 (field inversion)
• 8 (low-res global MHD)
• 8 (hi-res local MHD),
• lt10 (slow disambiguation)
• 2 (fast disambiguation)
• lt1 (rebinning/averaging),
• ??? (coordinate transformation/remapping),
• lt1 (calibration),
• 0 (hi-res global MHD runs at CCMC),
• ??? (NLFFF) on demand/request - 40 CPU hours
  per run
• lt1 (Solar wind models)

27
Vector Magnetic Field (contd.)

• Status (how much is done), a NLFFF algorithm
  selected (IDL and C implementations 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?

28
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 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 ???

29
LOS Magnetic Field (Contd)

• 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 schedule TBD?