LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager Philip Scherrer...

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LWS Science Team Meeting, 23 Mar 2004, Boulder 1 Helioseismic and Magnetic Imager http://hmi.stanford.edu Philip Scherrer [email protected] LWS-SDO Workshop 23-26 March 2004

Transcript of LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager Philip Scherrer...

Page 1: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 2: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 3: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 4: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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.

Page 5: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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.

Page 6: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 7: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 8: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 9: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 10: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 11: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 12: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 13: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 14: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 15: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 16: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 17: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

LWS Science Team Meeting, 23 Mar 2004, Boulder 17

HMI S/C Accommodations

HOP

HEB

X

Y

Z

Page 18: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 19: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 20: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 21: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 22: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 23: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 24: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 25: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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

Page 26: LWS Science Team Meeting, 23 Mar 2004, Boulder1 Helioseismic and Magnetic Imager  Philip Scherrer pscherrer@solar.stanford.edu LWS-SDO.

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