LWS Science Team Meeting, 23 Mar 2004, Boulder 1
Helioseismic and Magnetic Imager
http://hmi.stanford.edu
Philip [email protected]
LWS-SDO Workshop23-26 March 2004
LWS Science Team Meeting, 23 Mar 2004, Boulder 2
HMI Investigation Overview
Investigation Overview
Science Objectives
Data Products and Objectives
Data Product Examples
Science Team and Institutional Roles
HMI Instrument
HMI-AIA Joint SOC
HMI EPO
LWS Science Team Meeting, 23 Mar 2004, Boulder 3
The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to study the origin of solar variability and to characterize and understand the Sun’s interior and the various components of magnetic activity.
The HMI investigation is based on measurements obtained with the HMI instrument as part of the Solar Dynamics Observatory (SDO) mission.
HMI makes measurements of the motion of the solar photosphere to study solar oscillations and measurements of the polarization in a spectral line to study all three components of the photospheric magnetic field.
Investigation Overview - 1
LWS Science Team Meeting, 23 Mar 2004, Boulder 4
Investigation Overview - 2
The basic HMI measurements must be processed into higher level data products before analysis can proceed
HMI produces data products suitable to determine the interior sources and mechanisms of solar variability and how the physical processes inside the Sun are related to surface magnetic field and activity.
It also produces data products to enable model estimates of the low and far coronal magnetic field for studies of variability in the extended solar atmosphere.
LWS Science Team Meeting, 23 Mar 2004, Boulder 5
Investigation Overview - 3
The production of HMI high level data products and analysis of HMI data requires the participation of the HMI Team with active collaboration with other SDO instrument teams and the LWS community.
HMI observations will enable establishing the relationships between the internal dynamics and magnetic activity in order to understand solar variability and its effects. This is a prerequisite to understanding possible solar activity predictability.
HMI data and results will be made available to the scientific community and the public at large through data export, publications, and an Education and Public Outreach program.
LWS Science Team Meeting, 23 Mar 2004, Boulder 6
HMI science objectives are grouped into five broad categories:
Convection-zone dynamics and the solar dynamo;How does the solar cycle work?
Origin and evolution of sunspots, active regions and complexes of activity;What drives the evolution of spots and active regions?
Sources and drivers of solar activity and disturbances;How and why is magnetic complexity expressed as activity?
Links between the internal processes and dynamics of the corona and heliosphere;
What are the large scale links between the important domains?
Precursors of solar disturbances for space-weather forecasts.What are the prospects for predictions?
These objectives are divided into 18 sub-objectives each of which needs data from multiple HMI data products.
Progress will require a science team with experience in multiple disciplines.
HMI Science Objectives – Top Level
LWS Science Team Meeting, 23 Mar 2004, Boulder 7
HMI Science Objectives
Convection-zone dynamics and the solar dynamo Structure and dynamics of the tachocline Variations in differential rotation Evolution of meridional circulation Dynamics in the near surface shear layer
Origin and evolution of sunspots, active regions and complexes of activity Formation and deep structure of magnetic complexes of activity Active region source and evolution Magnetic flux concentration in sunspots Sources and mechanisms of solar irradiance variations
Sources and drivers of solar activity and disturbances Origin and dynamics of magnetic sheared structures and d-type sunspots Magnetic configuration and mechanisms of solar flares Emergence of magnetic flux and solar transient events Evolution of small-scale structures and magnetic carpet
Links between the internal processes and dynamics of the corona and heliosphere Complexity and energetics of the solar corona Large-scale coronal field estimates Coronal magnetic structure and solar wind
Precursors of solar disturbances for space-weather forecasts Far-side imaging and activity index Predicting emergence of active regions by helioseismic imaging Determination of magnetic cloud Bs events
LWS Science Team Meeting, 23 Mar 2004, Boulder 8Version 1.0
Global Helioseismology
Processing
Local Helioseismology
Processing
Filtergrams
Line-of-sightMagnetograms
Vector Magnetograms
DopplerVelocity
ContinuumBrightness
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
Tachocline
Differential Rotation
Meridional Circulation
Near-Surface Shear Layer
Activity Complexes
Active Regions
Sunspots
Irradiance Variations
Magnetic Shear
Flare Magnetic Config.
Flux Emergence
Magnetic Carpet
Coronal energetics
Large-scale Coronal Fields
Solar Wind
Far-side Activity Evolution
Predicting A-R Emergence
IMF Bs Events
Science ObjectiveData ProductProcessing
Observables
HMI Data
HMI Data Products and Objectives
LWS Science Team Meeting, 23 Mar 2004, Boulder 9
A. Sound speed variations relative to a standard solar model.
B. Solar cycle variations in the sub-photospheric rotation rate.
C. Solar meridional circulation and differential rotation.
D. Sunspots and plage contribute to solar irradiance variation.
E. MHD model of the magnetic structure of the corona.
F. Synoptic map of the subsurface flows at a depth of 7 Mm.
G. EIT image and magnetic field lines computed from the photospheric field.
H. Active regions on the far side of the sun detected with helioseismology.
I. Vector field image showing the magnetic connectivity in sunspots.
J. Sound speed variations and flows in an emerging active region.
B – Rotation VariationsC – Global Circulation
D – Irradiance Sources
H – Far-side Imaging
F – Solar Subsurface Weather
E – Coronal Magnetic Field
I – Magnetic Connectivity
J – Subsurface flows
G – Magnetic Fields
A – Interior Structure
HMI Data Product Examples
LWS Science Team Meeting, 23 Mar 2004, Boulder 10
Solar Domain of HMI Helioseismology
rota
tion
2
3
4
5
6
7
Sun
Log
Siz
e (k
m)
Zonal flow
AR
spot
SG
dynamoP
-mod
es
Tim
e-D
ista
nce
Rin
gs
Glo
bal H
S1 2 3 4 5 6 7 8 9
min
5min
hour
day
year
cycl
e
Log Time (s)
10
polar field
Earth
HMI resolution
granule
LWS Science Team Meeting, 23 Mar 2004, Boulder 11
Solar Domain of HMI Magnetic Field
2
3
4
5
6
7
Sun
Log
Siz
e (k
m)
Large-Scale
AR
spot
SG
dynamoP
-mod
es
1 2 3 4 5 6 7 8 9
min
5min
hour
day
rota
tion
year
cycl
e
Log Time (s)
10
polar field
Earth
HMI resolution
granule
Coronal field estimates
Vector
Line-of-sight
LWS Science Team Meeting, 23 Mar 2004, Boulder 12
HMI Co-Investigator Science Team-1
HMI Science Team
Name Role Institution Phase B,C,D Phase-E
HMI Lead Institutions
Philip H. Scherrer PI Stanford University HMI Investigation Solar Science
John G. Beck A-I Stanford University E/PO Science Liaison Surface Flows
Richard S. Bogart Co-I Stanford University Data Pipeline and Access Near Surface Flows
Rock I. Bush Co-I Stanford University Program Manager Irradiance and Shape
Thomas L. Duvall, Jr. Co-I NASA Goddard Space Flight Center Time-Distance Code Helioseismology
Alexander G. Kosovichev Co-I Stanford University Inversion Code Helioseismology
Yang Liu A-I Stanford University Vector Field Observable Code Active Region Fields
Jesper Schou Co-I Stanford University Instrument Scientist Helioseismology
Xue Pu Zhao Co-I Stanford University Coronal Code Coronal Field Models
Alan M. Title Co-I LMSAL HMI Instrument Solar Science
Thomas Berger A-I LMSAL * Vector Field Calibration Active Region Science
Thomas R. Metcalf Co-I LMSAL * Vector Field Calibration Active Region Science
Carolus J. Schrijver Co-I LMSAL * Magnetic Field Assimilation Models Active Region Science
Theodore D. Tarbell Co-I LMSAL HMI Calibration Active Region Science
Bruce W. Lites A-I High Altitude Observatory Vector Field Inversions Active Region Science
Steven Tomczyk Co-I High Altitude Observatory Vector Field Inversions Active Region Science
* Phase D only
LWS Science Team Meeting, 23 Mar 2004, Boulder 13
HMI Co-Investigator Science Team-2HMI Science Team – US and International Co-Is
Name Role Institution Phase B,C,D Phase-E
HMI US Co-Investigator Institutions
Sarbani Basu Co-I Yale University * Ring Analysis Code Helioseismology
Douglas C. Braun Co I Colorado Research Associates * Farside Imaging Code Helioseismology
Philip R. Goode Co-I NJIT, Big Bear Solar Observatory * Magnetic and Helioseismic Code Fields and Helioseismology
Frank Hill Co-I National Solar Observatory * Ring Analysis Code Helioseismology
Rachel Howe Co-I National Solar Observatory * Internal Rotation Inversion Code Helioseismology
Sylvain Korzennik A-I Smithsonian Astrophysical Observatory Helioseismology
Jeffrey R. Kuhn Co-I University of Hawaii * Limb and Irradiance Code Irradiance and Shape
Charles A. Lindsey Co-I Colorado Research Associates * Farside Imaging Code Helioseismology
Jon A. Linker Co-I Science Applications Intnl. Corp. * Coronal MHD Model Code Coronal Physics
N. Nicolas Mansour Co-I NASA Ames Research Center * Convection Zone MHD Model Code Convection Physics
Edward J. Rhodes, Jr. Co-I University of Southern California * Helioseismic Analysis Code Helioseismology
Juri Toomre Co-I JILA, Univ. of Colorado * Sub-Surface-Weather Code Helioseismology
Roger K. Ulrich Co-I University of California, Los Angeles * Magnetic Field Calibration Code Solar Cycle
Alan Wray Co-I NASA Ames Research Center * Convection Zone MHD Model Code Convection Physics
HMI International Co-Investigators
J. Christensen-Dalsgaard Co-I TAC, Aarhus University, DK * Solar Model Code Helioseismology
J. Leonard Culhane Co-I MSSL, University College London, UK Active Region Science
Bernhard Fleck Co-I European Space Agency ILWS Coordination Atmospheric Dynamics
Douglas O. Gough Co-I IoA, Cambridge University, UK * Local HS Inversion Code Helioseismology
Richard A. Harrison Co-I Rutherford Appleton Laboratories, UK Active Region Science
Takashi Sekii Co-I National Astron. Obs. of Japan, JP Helioseismology
Hiromoto Shibahashi Co-I University of Tokyo, JP Helioseismology
Sami K. Solanki Co-I Max-Planck-Institut für Aeronomie, DE AR Science
Michael J. Thompson Co-I Imperial College, UK Helioseismology
* Phase D only
LWS Science Team Meeting, 23 Mar 2004, Boulder 14
HMI Institutional Roles
HMI Instrument
HMI-AIA JSOC
HMI Science Team
SDO Science
LWS Science
HMIE/PO
Stanford
LMSAL
LWS Science Team Meeting, 23 Mar 2004, Boulder 15
HMI Team Organization
Alan TitleHMI-LMSAL Lead
Rock BushHMI-Stanford Prg. Mgr.
Larry SpringerLMSAL SDO Prg. Mgr.
Jim AloiseGround System
Rasmus LarsenProcessing & Analysis
Deborah ScherrerEduc. & Public Outreach
Rick BogartData Export
Barbara FischerHMI Deputy Prg. Mgr.
Philip ScherrerHMI Principal Investigator
Edgar ThomasCamera Electronics
Dexter DuncanCCDs
John MilesSystem Engineering
Rose NavarroThermal
Russ LindgrenElectrical Lead
Glenn GradwohlMechanical Lead
Dave AkinMechanism Lead
Rick RairdenOptical Elements
Jerry DrakeInst. Software Lead
Mike LevayIntegration & Test
Jesper SchouInstrument Scientist
Local Helioseismology - Alexander KosovichevGlobal Helioseismology - Jesper SchouMagnetic Fields - Yang LiuHAO Vector Fields teamCo-I Science Team
Science Team
Romeo DurscherHMI Admin
Keh-Cheng ChuGround Sys Hardware
LWS Science Team Meeting, 23 Mar 2004, Boulder 16
Science Team Coordination
• Team meetings: May 2003, Mag splinter Oct 2003
• Next HMI (+AIA?) September 2004
• Leads for Planning• Local Helioseismology Sasha Kosovichev
• Global Helioseismology Jesper Schou
• Modeling & Inversions Sasha Kosovichev
• Mag Field large & small Yang Liu
• Vector Field Inversions Steve Tomczyk
• Continuum studies Rock Bush
• Space Weather Coord. Yang Liu
LWS Science Team Meeting, 23 Mar 2004, Boulder 17
HMI S/C Accommodations
HOP
HEB
X
Y
Z
LWS Science Team Meeting, 23 Mar 2004, Boulder 18
Instrument Overview – Optical Path
Optical Characteristics:Focal Length: 495 cmFocal Ration: f/35.2Final Image Scale: 24m/arc-secRe-imaging Lens Magnification: 2Focus Adjustment Range: 16 steps of 0.4 mm
Filter Characteristics:Central Wave Length: 613.7 nmReject 99% Solar Heat LoadBandwidth: 0.0076 nmTunable Range: 0.05 nmFree Spectral Range: 0.0688 nm
LWS Science Team Meeting, 23 Mar 2004, Boulder 19
HMI Optics Package (HOP)
OP Structure
Telescope
Front Window
Front Door
Vents
Support Legs (6)
Polarization Selector
Focus/Calibration Wheels
Active Mirror
Limb B/S
Alignment Mech
Oven Structure
Michelson Interf.
Lyot Filter
Shutters
Connector Panel
CEBs
Detector(Vector)
Fold MirrorFocal Plane B/S
Mechanical Characteristics:Box: 0.84 x 0.55 x 0.16 mOver All: 1.19 x 0.83 x 0.29 mMass: 39.25 kgFirst Mode: 63 Hz
YX
Detector(Doppler)
Limb Sensor
Z
LWS Science Team Meeting, 23 Mar 2004, Boulder 20
HMI Requirements - Driving
Parameter Requirement
Central wavelength 6173.3 Å ± 0.1 Å (Fe I line)
Filter bandwidth 76 mÅ ± 10 mÅ fwhm
Filter tuning range 680 mÅ ± 68 mÅ
Central wavelength drift < 10 mÅ during any 1 hour period
Field of view > 2000 arc-seconds
Angular resolution better than 1.5 arc-seconds
Focus adjustment range ± 4 depths of focus
Pointing jitter reduction factor > 40db with servo bandwidth > 30 Hz
Image stabilization offset range > ± 14 arc-seconds in pitch and yaw
Pointing adjustment range > ± 200 arc-seconds in pitch and yaw
Pointing adjustment step size < 2 arc-seconds in pitch and yaw
Dopplergram cadence < 50 seconds
Image cadence for each camera < 4 seconds
Full image readout rate < 3.2 seconds
Exposure knowledge < 5 microseconds
Timing accuracy < 0.1 seconds of ground reference time
Detector format > 4000 x 4000 pixels
Detector resolution 0.50 ± 0.01 arc-second / pixel
Science telemetry compression To fit without loss in allocated telemetry
Eclipse recovery < 60 minutes after eclipse end
Instrument design lifetime 5 years at geosynchronous orbit
LWS Science Team Meeting, 23 Mar 2004, Boulder 21
Data Section
HMI Overview – HEB Key Features
Power all HMI sub-systemsProcessing for decoding and execution of commands and acquiring and formatting of housekeeping telemetryContains: Processor Board (2) PCI to Local Bus Bridge and 1553 Interface board (2) Mechanism and Heater Controller Board (4) Housekeeping Data Acquisition Board (2?) CCD Camera Interface Board (2) Data Compressor/High Rate Interface Board (2) ISS Limb Tracker Board ISS PZT Driver Board Power Converter Subsystem with redundant power
convertersHEB dimensions: 254 X 424 X 320 mm, Mass 19.3 kgOven Controller and Limb Sensor Pre-Amp are in HOP
X Y
Z
Power Section
LWS Science Team Meeting, 23 Mar 2004, Boulder 22
HMI & AIA JSOC Architecture
Science TeamForecast Centers
EPOPublic
Catalog
Primary Archive
HMI & AIAOperations
House-keeping
Database
MOCDDS
Redundant Data
Capture System
30-DayArchive
OffsiteArchiv
e
OfflineArchiv
e
HMI JSOC Pipeline Processing System
DataExport& WebService
Stanford
LMSAL
High-LevelData Import
AIA AnalysisSystem
LM-Local Archive
QuicklookViewing
housekeeping GSFCWhite Sands
World
LWS Science Team Meeting, 23 Mar 2004, Boulder 23
HMI - SOC 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
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 ProductProcessing
Level-0
Level-1
LWS Science Team Meeting, 23 Mar 2004, Boulder 24
HMI - SOC Processing and Data Flow
Dataflow (GB/day)
Joint Ops
ScienceArchive440TB/yr(Offsite)
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
LWS Science Team Meeting, 23 Mar 2004, Boulder 25
JSOC Development Strategy
SOC Ops system developed at LMSAL as evolution of MDI, TRACE, SXI, etc. programs.
During instrument build, used with EGSE for I&T
During operations hour/day for health check and day/week for command loads
SOC Data system developed at Stanford as evolution of existing MDI data system.
2004 - 2005: First 2 Years Procure development system with most likely components (e.g. tape type, cluster
vs SMP, SAN vs NAS, etc) Modify pipeline and catalog infrastructure and implement on prototype system. Modify analysis module API for greater simplicity and compliance with pipeline. Develop calibration software modules.
2006 - 2007: Two years prior to launch Complete Level-1 analysis development, verify with HMI test data. Populate prototype system with MDI data to verify performance. Procure, install, verify computer hardware. Implement higher-level pipeline processing modules with Co-I support
During Phase-E Add media and disk farm capacity in staged plan, half-year or yearly increments First two years of mission continue Co-I pipeline testing support
LWS Science Team Meeting, 23 Mar 2004, Boulder 26
HMI E/PO Education / Public Outreach
HMI E/PO Plans:
Development of a model Science Fellow Program: a science-outreach, community service student training program implemented and tested in a collection of underserved environments
Solar Planetarium Program for small, interactive planetaria (joint with LWS, Lawrence Hall of Science, & AIA)
Solar Sudden Ionospheric Disturbance Monitor (Solar SID) Program developed and established in high schools throughout the nation (collaborative effort with NSF CISM)
Information Resources – Posters, Web, Press, etc.
Partnerships with AIA instrument team, other NASA entities, science museums and planetaria