Solar Terrestrial Relations Observatory (STEREO) Science Plans

Janet Luhmann forSTEREO Instrument and Science teamsPresentation to LWS Workshop, Boulder

March, 2004

Science Objectives1. Understand the causes and

mechanisms of CME initiation 2. Characterize the propagation of

CMEs through the heliosphere3. Discover the mechanisms and

sites of energetic particle acceleration in the low corona and the interplanetary medium

4. Develop a 3D time-dependent model of the magnetic topology, temperature, density, and velocity structure of the ambient solar wind

Science Approach: Two sun-viewing spacecraft moving away from Earth Ahead and Behind

Sun SunEarth

Ahead @ +22/year

Behind @ -22/year

1 yr.

2 yr.

3 yr.4 yr.

1yr.

2yr.3 yr.4 yr.

Ahead

BehindEarth

Heliocentric Inertial Coordinates(Ecliptic Plane Projection)

Geocentric Solar Ecliptic CoordinatesFixed Earth-Sun Line

(Ecliptic Plane Projection)

STEREO INSTRUMENTSSECCHI- Remote Sensing Package that will track Coronal Mass Ejections (CMEs) from the Sun to the Earth.

Two White Light Coronagraphs (COR1,COR2)- COR1 explores 1.4 4 Rsun. COR2 explores 2 15 Rsun Extreme Ultra Violet Imager (EUVI)- Observes chromosphere and inner corona Heliospheric Imager (HI1, HI2)- Observes Coronal Mass Ejections from the Sun to the Earth (12 300 Rsun)

IMPACT- will sample the 3-D distribution of solar wind plasma electrons, the characteristics of the energetic particle ions and electrons, and the local magnetic field.

Solar Wind Experiment (SWEA)-Measures ~0-3 keV electrons with wide angle coverageSuprathermal Electron Telescope (STE)-Measures electrons from 2-100 keV with wide angle coverageMagnetometer Experiment (MAG)-Measures the vector magnetic field at 65,536 nT and 500 nT rangesSolar Energetic Particle Experiment (SEP) Suite

Measures electrons from 0.02-6 MeV Measures protons from 0.02 100 MeV Measures helium ions from 0.03 100 MeV/nucleon Measures heavier ions form 0.03 40 MeV/nucleon

PLASTIC- will provide the plasma characteristics of protons, alpha particles, and heavy ion. Provide composition measurements of heavy ions and characterizes the CME plasma

SWAVES- in-situ as well as remote sensing instrument. Tracks CME Driven Shocks from the Corona to the Earth.

STEREO-B (BEHIND) OBSERVATORY

Deployed SWAVES Electric Field Antenna

(3 places)

DeployedIMPACT Boom

IMPACTSolar Wind Electron Analyzer (SWEA)

IMPACTSuprathermal Electron Detector

(STE)

IMPACTMagnetometer

(MAG)

DeployedHigh Gain RF

Antenna(HGA)

SECCHI Heliospheric Imager

(HI)

SECCHISun-Centered ImagingPackage (SCIP) Assy

(COR-1, COR-2, EUVI, GT)

Low Gain RFAntenna (2)

(LGA)

Sun Sensor (5)

Adapter Ring

Bi-fold Solar Panel Inertial Measurement Unit (IMU)

PLASTIC Instrument

- X

- Y

+ Y

+ X+ Z

- Z

IMPACT SEP

STEREO Organization (science elements)Project Manager

Nick ChrissotimosDeputy Project Manager

Jim AdamsDeputy Project Manager/Instruments

Mike DelmontDeputy Project Manager/Resources

Pietro Campanella

Project ManagerNick Chrissotimos

Deputy Project ManagerJim Adams

Deputy Project Manager/InstrumentsMike Delmont

Deputy Project Manager/ResourcesPietro Campanella

Project ScientistMichael Kaiser

Project ScientistMichael Kaiser

Deputy Proj. ScientistTerry Kucera

STEREO Science CenterBill Thompson-EITI

Instrument ManagementInstrument Management

IMPACT/ UCBInstrument Mgr. / Lil Reichenthal,

Renan Borelli

SWAVES/ UMNInstrument Mgr. / Paul Buchanan

SECCHI/ NRLInstrument Mgr. / Bernie Klein

PLASTIC/ UNHInstrument Mgr. / Art Jacques-OSC

Mission Systems EngineeringSystems Engineer / Shane Hynes Swales

Instrument Systems Engineer / Lisa Bartusek, Steve Wasserzug-SwalesSystems Engineering / Joe Cerullo-ASRC

S/W Systems Engineering / Jerry Hengemihle-MTEL

Mission Systems EngineeringSystems Engineer / Shane Hynes Swales

Instrument Systems Engineer / Lisa Bartusek, Steve Wasserzug-SwalesSystems Engineering / Joe Cerullo-ASRC

S/W Systems Engineering / Jerry Hengemihle-MTEL

AETD Engineering Support

STP Program Support OfficeConfiguration Management / D. Dusterwald-CSC, L. Hepler-CSC

Planning / T. Parr-CSC, K. Milligan-CSC, D. Wicks-CSC, J. Rogers-CSCBusiness Support / Mandy Tatum-SERV, Bobbie Power-SGT

STP Program Support OfficeConfiguration Management / D. Dusterwald-CSC, L. Hepler-CSC

Planning / T. Parr-CSC, K. Milligan-CSC, D. Wicks-CSC, J. Rogers-CSCBusiness Support / Mandy Tatum-SERV, Bobbie Power-SGT

System AssuranceSystems Assurance Mgr. / Michael Haynes

Quality Engineer / Pam Hopkins-HTSI, Larry Gibb-SRSTE

System AssuranceSystems Assurance Mgr. / Michael Haynes

Quality Engineer / Pam Hopkins-HTSI, Larry Gibb-SRSTE

Parts AssuranceAntonio Reyes-OSC

SafetyRichard Bolt

ReliabilityMatt Samuel-MUNIZ

Observatory ManagementObservatory Manager / Larry Christensen

Mark Jarosz

Observatory ManagementObservatory Manager / Larry Christensen

Mark Jarosz

JHU/APLTed Mueller, Project Mgr.

GSFC Procurement OfficeRex Elliot

Contracting Officer / Julie Janus

GSFC Procurement OfficeRex Elliot

Contracting Officer / Julie Janus

Financial ManagerElaine Blazosky

Resource AnalystTracy Felton, Linnette Morales,

Beverly Thomas

General Business SupportJack Arrison-OSC

Business SupportBusiness Support

25 November 03

Project Support ManagerLeslie Cusick-SGT

Software Quality AssuranceMike Garner-HTSI

Unique Science Opportunities

Stereo viewing by remote sensing suite to obtain 3D images of CME and coronal features

Multipoint remote/in-situ observations of a single event In-situ observations to determine ICME structure Imaging and in-situ data from a single event to

sharpen predictive capability Imaging Earth directed events

Sun Earth Connection Coronal and Heliospheric Investigation (PI: Russ Howard, PM: Daniel Moses)

SECCHI Instrumentation

SECCHI Science Overview

010926-27SECCHI_PDR_02_Overview.10

SECCHI Instrument Measurements

010926-27SECCHI_PDR_03_Science.11

EUVI COR1 COR2 HI-1 HI-2Instrument Type Narrow-Band

Ritchet-CrtienTelescope

Internally-Occulted

Coronagraph

Externally-Occulted

Coronagraph

Externally-Occulted

Coronagraph

Externally-Occulted

CoronagraphImage Products He II, Fe IX,

Fe XII, Fe XV Images

Multi-Viewpoints

B ImagepB Image

Polarization Angle Map

Multi-viewpoints

B ImagepB Image

Polarization Angle Map

Multi-viewpoints

B Image

Multi-viewpoints

B Image

Multi-viewpoints

Bandpass (nm) He II 30.4Fe IX 17.1Fe XII 19.5Fe XV 28.4

650-660 650-750 650-750 400-1000

Telescope Orientation Sun-Centered Sun-Centered Sun-Centered

Side-lookingalong Sun-Earth Line

=13.65 deg

Side-lookingalong Sun-Earth Line

=53.35 degCoronal Coverage (Rsun) Disk to 1.7 1.3 to 4.0 2 to 15 12 to 84 66 to 318

Telescope Field of View (deg) 0.90 2.13 8.53 20.0 69.2Image Array 2048x2048 1024x1024 2048x2048 1024x1024 1024x1024

Spatial Scale (arcsec/pixel) 1.6 7.5 15 70 240Exposure Time Range (sec) [0.1, 30] [0.1, 1.0] [0.1, 5] [10, 30] [60, 90]

Nominal Images per Sequence 2 image 3 images 3 images 70 images 50 imagesRequired Cadence (min per sequence) 1 1 5 60 120

Brightness Sensitivity (log10 B/B0) N/A -9.5 -12 -14.5 -15.5

Straylight Rejection (log10 B/B0) N/A -6.0 -10.5 -12.5 -14Brightness Accuracy (%) 10 10 10 10 10

Polarized Brightness Accuracy (%) N/A 10 10 N/A N/A

SECCHI Instrument Performance Specification

Why Multiple Coronagraphs?

010926-27SECCHI_PDR_02_Overview.12

Each coronagraph is designed to operate in a small height regime.

This makes the problem of observing the corona over many orders of magnitude tractable.

Shown are the 1 sigma CME detection threshold compared to the coronal brightness.

Coronagraph ImagingView from Earth

Solar disk is 106 times brighter than the corona

The central part of the field is blocked to eliminate the bright disk

The surrounding coronal structure is brightest when within +/- 30 degrees of the plane of the sky as seen from the spacecraft

A

EARTH

B

EARTH

Polar Views

Stereo Imaging with COR1 or COR2

No overlap in line of sight (LOS) at intermediate separation angles

Overlapping LOS exists at small angles, and large separation angles

AB

EARTH

Corona seen by coronagraph B

Corona seen by coronagraph A

Polar View

Overlap of Views from HI1 and CORs

(SWAVES) PI: J-L Bougeret, US Deputy: M Kaiser, PM: K Goetz

SWAVES Instrumentation

3 km wavelength !

SWAVES Science Overview

Track and probe CME-driven shocks from the corona to 1 AU - model free

Map in-situ structure of CME-driven shocks and flare electron beams

Probe density and IMF structure of the heliosphere before and after CMEs

Understand the radio emission process and beam pattern of radio bursts

Measure electron density and temperature of filament material in clouds

Receivers in frequency domain and time domain

SWAVES is two instruments in one - remote sensing and in-situ

The SWAVES Instrument Radio Remote Sensing (LESIA- Obs. Paris) : heritage

High Frequency Receiver 125 kHz - 16 MHz Cassini Low Frequency Receiver 2.5 kHz - 160 kHz and Wind Fixed Frequency Receiver 32 or 34 MHz Stro-1,-5

In situ measurements (Minnesota) wave form receiver (250,000 samples/s) Wind

(3 components E)

SWAVES Data Products(available on Web immediately)

Dual daily dynamic spectra Catalog of type II/IV bursts Selected source locations versus time In situ electron density, when possible

Must have density model to get distance

What can we learn from radio stereoscopy?

type III bursts (energetic electrons) (SWAVES /SECCHI) Radiation mechanism, association with electron events structure and topology of large scale magnetic fields (mapping) understanding propagation phenomena (weak/strong scattering)

type II bursts (shock waves) (SWAVES /SECCHI) association with Coronal Mass Ejections (3-D localization of the source) formation and evolution of the shock (study of multiple sources) acceleration of energetic particles from the shock and interacting shocks

(cannibalism)

radio radiation mechanisms (SWAVES /IMPACT) radiation modes (fundamental and/or harmonic) Wave-particle correlations (micro-physics)

contraints on theories local structure and topology of the source

In-situ Measurements of Particles and CME Transients Investigation (PI: Janet Luhmann, PM: Dave Curtis)

IMPACT (In-situ Measurements of Particles and CME Transients) Instrument Overview

Boom Suite: Solar Wind Electron Analyzer (SWEA) Suprathermal Electron Telescope (STE) Magnetometer (MAG)

Solar Energetic Particles Package (SEP):

Suprathermal Ion Telescope (SIT) Solar Electron and Proton Telescope (SEPT) Low Energy Telescope (LET) High Energy Telescope (HET)

Support:IMPACT BoomSEP CentralInstrument Data Processing Unit (IDPU)

STE-U

SEPSEPT-E

SEP LET,HET, SIT

MAG, STE-D

SWEA

Overall IMPACT Investigation Rationale

Basic IMPACT Measurements

Experiment Instrument Measurement Energy or Mag. field range

Time Res. Beacon Time Res. (*)

Instrument provider

STE Electron flux and anistropy

2-100 keV 16 s 2D x 3E, 60s UCB (Lin) SW

SWEA 3D electron distrib., core & halo density, temp. & anisotropy

~0-3 keV 3D=1 min 2D=8s

Mom.=2s

Moments, 60s

CESR (Sauvaud) + UCB (Lin)

MAG MAG Vector field 500nT, 65536 nT

1/4 s 60s GSFC (Acuna)

He to Fe ions 0.03-2 MeV/nuc 1 min 3S x 2E, 60s SIT 3He 0.15-0.25

MeV/nuc 1 min ----

U. of Md. (Mason) + MPAE (Korth) + GSFC (von Rosenvinge)

Diff. electron flux 20-400 keV 1 min 3E, 60s Diff. proton flux 60-7000 keV 1 min 3E, 60s

SEPT

Anistropies of e,p As above 15 min ----

U. of Kiel (Mueller-Mellin) + ESTEC (Sanderson)

Ion mass numbers 2-28 & anisotropy

3-30 MeV/nuc 1-15 min. 2S x 2E, 60s

3He ions flux & anistropy

2-15 MeV/nuc 15 min. 1E, 60s

LET

H ions flux & anistropy

1.5-6 MeV 1-15 min. 1E, 60s

Caltech (Mewaldt) + GSFC (von Rosenvinge) + JPL (Wiedenbeck)

Electrons flux 1-6 MeV 1-15 min. 1E, 60s H 13-100 MeV 1-15 min. 1E, 60s He 13-100 MeV 1-15 min. 1E, 60s

HET

3He 15-60 MeV/nuc 15 min ----

GSFC (von Rosenvinge) + Caltech (Mewaldt) + JPL (Wiedenbeck)

SEP

SEP Common

---- ---- ---- ---- Caltech (Mewaldt) + GSFC (von Rosenvinge)

IMPACT Common

IDPU (+Mag

Analog)

---- ---- ---- ---- UCB (Curtis)

IMPACT Particles Domain: Solar Wind, Suprathermal and SEP electrons, SEP ions

SEP Ions Composition Coverage

SEPTSEPT

IMPACT Investigation Approaches:

Multipoint interplanetary characterization of the imaged CMEs and their associated solar energetic particles (SEP) at increasing separations

Quadrature measurements with imagers on STEREO and at Earth

Space Weather detection, modeling and prediction

Doing STEREO Science with IMPACT

Plasma and SupraThermal Ion Composition Investigation (PI: Toni Galvin, PM: Steve Turco)

PLASTIC Instrumentation on the STEREO Spacecraft

PLASTIC SCIENCE GOALS

Coronal elemental abundances show fractionation affects from the photospheric values, indicative of the extraction process.

Coronal charge states are a function of the coronal temperature and distribution functions (and perhaps other processes).

Solar wind flow types (fast, slow, ICME) show distinguishing abundances and charge states reflective of their coronal origins and acceleration processes.

The Plasma and SupraThermalIon Composition (PLASTIC) Investigation provides solar wind ion and suprathermal (0.3 to 80 keV/e) positive ion measurements for the Solar Terrestrial Relations Observatory (STEREO).

PLASTIC incorporates three science sensor functions into one package:

The PLASTIC PLASTIC Solar Wind SectorSolar Wind Sector (SWS) Proton (SWS) Proton ChannelChannel measures the distribution functions of solar wind protons (H+) and alphas (He+2), providing proton density (n ), velocity (Vsw), kinetic temperature (Tk) and its anisotropy (T || , T), and alpha to proton (He+2 / H+) ratios with a time resolution up to about one minute (60 seconds).

The PLASTIC PLASTIC Solar Wind SectorSolar Wind Sector (SWS) Main (SWS) Main (Composition) Channel(Composition) Channel measures the elemental composition, charge state distribution, kinetic temperature, and speed of themore abundant solar wind heavy ions (e.g., C, O, Mg, Si, and Fe) by using Electrostatic Analyzer (E/Q), Time-of-Flight (TOF), and Energy (E) measurement to determine Mass and M/Q. Typical time resolution for selected ions will be ~ 5 x 60 = 300seconds.

The PLASTIC PLASTIC WideWide--Angle PartitionAngle Partition (WAP)(WAP) measures distribution functions of suprathermal ions, including interplanetary shock-accelerated (IPS) particles associated with CME-related SEP events, recurrent particle events associated with Co-rotating Interaction Regions (CIRs), and heliosphericpickup ions. Typical time resolution for selected ions will be several minutes to hours.

Solar WindSector

Wide Angle Partition For Suprathermals

STEREO Ions Spectral Coverage PLASTIC and IMPACT

PLASTIC

IMPACT

PLASTIC Science Goal: Solar Wind Ion Abundances

Composition of Solar Wind Particles key to coronal sources and conditions

Different coronal structures emit solar wind with different speeds and different composition

Solar wind charge state composition is an indication of the coronal temperatures and conditions where the solar wind

originated, including the initiation of CMEs.

Solar wind in Interplanetary CMEs often exhibit higher ionization states than other solar wind flows

0

50

100

150

200

250

300

0 200 400 600 800 1000

Time After Launch (days)

Cum

ulat

ive

Tota

l of

Ste

reo

CM

Es

Earth Directed

Stereo Imaged

Multipoint In-Situ

Mission Phases

Mission Observational Capabilities

Mission Phase Remote Sensing In-Situ

Prime Stereo Science

Stereo view of plane of sky CMEs and their propagation

Multipoint observation of Earth directed CMEsMultipoint observation of Earth directed CMEsSTEREO-A at quadrature with STEREO-B

Multipoint Science

Halo and limb CMEs and their propagation

LWS Precursor Science

Earth directed CMEsSTEREO-A at quadrature with STEREO-B

Ground Segment Elements

Deep Space Mission System (DSMS) Mission Operations Center (MOC)

Flight operations team located at APL Payload Operations Centers (POCs)

Instrument teams at home institutions (nominal) Instrument teams co-located at MOC during

commissioning and contingency operations STEREO Science Center (SSC)

What is the SSC? The SSC performs the following functions

1. Collects telemetry and processed data, archives it, and serves it on the web.

2. Receives beacon data from the DSN and NOAA antenna partners, processes it, and makes space weather products available in near real-time.

3. Focal point for science coordination4. Focal point for education and public outreach.

In addition, through interaction with the SOLAR Software Library, the SSC can act as a focal point for software coordination.

Personnel Chief Observer - Bill Thompson SDAC/VSO liaison Joe Gurman Web Master Emilie Drobnes

System/Network Administrators Amy Skowronek, Marc Despres, Alex Young

Data Flow/SSC Block DiagramPublic Internet Access

Interfaces & Data Volume

Data Type Transfer Method Volume(per day, 2 s/c)

All level-0 Off-line from MOC (ftp)

1.25 GB

Mission Support Off-line from MOC (ftp)

0.01 GB

Space Weather Packets

Near-real-time from MOC (socket)

0.002 GB

Space Weather transfer frames

Near-real-time from antenna partners

0.02 GB

Higher level data Off-line from PI teams (ftp)

25 GB

Software tools Off-line from PI teams (ftp)

0.005 GB

STEREO Space Weather Prediction

STEREO modeling will physically connect in situ observations to images

(shown: SAIC CME model, Linker/ Odstrcil merged CME/Solar Wind model)

Simulated time series

STEREO Status

1. STEREO re-plan officially approved by Headquarters Feb 11-24, 2006 launch (mostly due to thruster valve problem) Increased price cap (about 10-11% including launch slip) all contained within STP probe

line item (includes missing SSC space weather funding) No descopes Instrument delivery target dates have been adjusted based on Feb 2006 launch date.

Additional time may be granted on case-by-case basis Launch vehicle prep time now acceptable (27 months)

2. Terry Kucera (DPS) heading up EPO effort First EPO telecon March 17: nominally monthly STEREO now top priority with Goddard Visualization group

3. CCMC may provide STEREO modeling support4. Post-launch organization/operations now being actively pursued

Mission Director to be named (for post launch) Mission Operation Manager (MOM) to organize pre-launch

Solar Terrestrial Relations Observatory (STEREO) Science PlansScience ObjectivesScience Approach: Two sun-viewing spacecraft moving away from Earth Ahead and BehindSTEREO Organization (science elements)Unique Science OpportunitiesCoronagraph ImagingStereo Imaging with COR1 or COR2The SWAVES InstrumentWhat can we learn from radio stereoscopy?Overall IMPACT Investigation RationaleBasic IMPACT MeasurementsIMPACT Particles Domain: Solar Wind, Suprathermal and SEP electrons, SEP ionsSEP Ions Composition CoverageIMPACT Investigation Approaches:PLASTIC Instrumentation on the STEREO SpacecraftSTEREO Ions Spectral Coverage PLASTIC and IMPACTComposition of Solar Wind Particles key to coronal sources and conditionsSolar wind charge state composition is an indication of the coronal temperatures and conditions where the solar wind originateMission PhasesMission Observational CapabilitiesGround Segment ElementsData Flow/SSC Block DiagramInterfaces & Data VolumeSTEREO modeling will physically connect in situ observations to imagesSTEREO Status

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