Page 1HMI Team Meeting – January 26-27, 2005 HMI Investigation Overview Philip Scherrer...

HMI Team Meeting – January 26-27, 2005

HMI Investigation Overview

Philip Scherrer

[email protected]

650-723-1504


SDO - Solar Dynamics Observatory

HOP

HEB

SDO will carry:

•AIA - The Atmospheric Imaging ArrayLockheed Martin Solar and Astrophysics Lab

•EUV – EUV Variability ExperimentUniversity of Colorado

•HMI – Helioseismic and Magnetic ImagerStanford University with LMSAL

SDO will be in an inclined geosynchronous orbit with data collected at White Sands NM and operations managed at GSFC.


Goals for January 2005 Team Meeting

We are now just after the HMI Critical Design Review.

The flight instrument is being built and will be ready for optical testing this summer.

It will be delivered to NASA for integration onto SDO in November of next year.

Proposal was about three years ago and launch about three years away.

The data processing center design is near completion.

We are near the point where we will need to begin the process of incorporating analysis software.

The primary goals for this meeting are to:

• Update the specifications for standard data products

• Confirm Co-I plans for analysis software development

• Encourage coordination in development of science analysis techniques

• Update the Science Team on the project status

• Clarify priorities for early science goals


HMI Institutional Roles

HMI Instrument

HMI & AIA JSOC

SDO Science

LWS Science

E/POStanford

LMSAL

The HMI Science Team includes 30 Co-Investigators and many Associate Investigators at 21 institutions in the US and abroad

HMI Science Team


HMI Science Investigator 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


HMI Science Investigator Team - 2

HMI 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


SDO/HMI – Stanford Personnel

Phil ScherrerHMI Principal Investigator

Jesper SchouHMI Instrument Scientist

Rock BushHMI-Stanford Prg. Mgr.

Romeo DurscherAdmin

Sasha KosovichevHMI Science Lead

Phil Scherrer/20**Acting JSOC Data Lead

Alan TitleAIA Principal Investigator

Larry SpringerHMI-AIA Prg. Mgr.

Jerry DrakeInst. Software Lead

LM

SA

L

Barbara FischerHMI Deputy Prg.Mgr.

Jim LemenJSOC Ops Lead

Yang LiuMagnetic Field Science

Margie StehleAdmin Support

Carl CimiluccaJSOC System Engineer

Keh-Cheng ChuJSOC Hardware

TBDSystem Support

Jim AloiseJSOC Software

Jeneen SommersDatabase & GUI

Hao ThaiData Operations

Rasmus LarsenProcessing & Analysis

Sebastien CouvidatSci Prog Support

Rick BogartData Export

Karen TianVSO Access

TBDSci Programmer


HMI Schedule


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.

HMI makes measurements of the motion of the solar photosphere to study solar oscillations in order to determine the interior sources and mechanisms of solar variability

It also makes measurements of the photospheric magnetic field in order to study how the physical processes inside the Sun are related to surface magnetic field and to enable estimates of the low and far coronal magnetic field for studies of variability in the extended solar atmosphere.

Investigation Overview


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 requires a science team with experience in multiple disciplines.

HMI Science Objectives – Top Level


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

HMI Team Meeting – January 26-27, 2005 Version 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


HMI-AIA Joint Science Operations Center

• HMI and AIA SOCs have been merged to form a JSOC

• Components of the JSOC will be at both Stanford and Lockheed-Martin Solar and Astrophysics Lab (LMSAL)

– JSOC-Ops for both HMI and AIA at LMSAL

– Data capture, pipeline processing, online archive, tape archive, export functions at Stanford.

– HMI Higher level processing at Stanford

– AIA Higher level processing at LMSAL

– High-speed network connection between the two sites

• The JSOC will be discussed in more detail as part of both the SDO CDR and the SDO ground system CDR next year


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-AIA JSOC Pipeline Processing System

DataExport& WebService

Stanford

LMSAL

High-LevelData Import

AIA AnalysisSystem

Local Archive

QuicklookViewing

housekeeping GSFCWhite Sands

World


Schematic Diagram of HMI

Telescope with

polarization

analysis

Tunable narrow

band filter

Camera

system

SDOMOC

DDSComputers

Electronics to make it

work

Science Investigation

Science Team, NASA, Taxpayers


6169 6172 6175 6178

Measure Here

HMI consists of a telescope, tunable filter, camera, and necessary electronics.

HMI repeatedly images the Sun in six polarizations at five wavelengths across a spectral line.

The position of the line tells us the velocity while the shape changes of the line in different polarizations tell us the magnetic field direction and strength in the part of the Sun’s surface seen by each pixel.

Long gap-free sequences of velocity images are needed to enable the techniques of helioseismology.

HMI – How It Works


The green and red curves are Left and Right circular polarized components and allow measurement of the line-of-sight projection of the field.

Analysis of both polarizations is required to infer the Doppler velocity and line-of-sight magnetic flux.

For vector magnetic fields two directions of linear polarization are added to infer the field direction.

One HMI camera is used for velocity and LOS field, the other for vector fields.

Magnetic Field Sample Profile

HMI measures magnetic fields by sampling the Zeeman split line in multiple polarizations.

The figure shows the five sample positions for a sunspot umbral field (about 3000G) with a 1000 m/s offset.


Basic Requirements Sources

• SDO Level 1 Requirements

• SDO Mission Requirements Document (MRD)

– Summary of spacecraft and instrument driving requirements

• HMI Instrument Functional Specification

– Top level instrument requirements – part of the HMI contract statement of work

• HMI Instrument Performance Document (IPD)

– Detailed HMI science drivers and flowdown to subsystem requirements

• HMI Performance Assurance and Implementation Plan (PAIP)

– HMI implementation of the SDO Mission Assurance Requirements

• HMI to Spacecraft Interface Control Documents (HMI-S/C ICD)

• Ground System Interface Control Documents


HMI “Level 1” Requirements

To enable accomplishment of the science objectives of the investigation, the HMI instrument will produce measurements in the form of filtergrams in a set of polarizations and spectral line positions at a regular cadence for the duration of the mission that meet these basic requirements:

• Full-disk Doppler velocity and line-of-sight magnetic flux images with 1 arc-sec resolution at least every 50 seconds.

• Full-disk vector magnetic images of the solar magnetic field with 1 arc-sec resolution at least every 10 minutes.

The HMI data completeness and continuity requirement is to capture 99% of the HMI science observables 95% of the time.


Source of HMI Requirements

• HMI Science Objectives– Duration of mission

– Completeness of coverage

– HMI Science Data Products

– Roll accuracy

– Time accuracy (months)

• HMI Observation Sequences – Duration of sequence

– Cadence

– Completeness data sequence

– Noise

– Resolution

– Time accuracy (days)

• HMI Observables– Sensitivity

– Linearity

– Acceptable measurement noise

– Image stability

– Time rate (minutes)

– Orbit knowledge

• HMI Instrument Data– Accuracy

– Noise levels

– Completeness of filtergrams

– Tuning & shutter repeatability

– Wavelength knowledge

– Image registration

– Image orientation jitter

• HMI Instrument– Mass

– Power

– Telemetry

– Envelope

• Subsystem requirements– CCD: Thermal environment

– ISS: pointing drift rate, jitter

– Legs: pointing drift range


HMI Performance Requirements Summary

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

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