STEREO IMPACT Measurements and CISM...

Luhmann1

STEREO IMPACT / CISM MODELS: Tools for LWS LWS Workshop, Boulder23-26 March, 2004

STEREO IMPACT Measurements and CISM Heliospheric Models: Tools for LWS Science & Applications

J.G. Luhmann, D.W. Curtis, R.P. Lin, D. Larson, P. Schroeder (SSL, UC Berkeley)A. Cummings, R.A. Mewaldt, E.C. Stone (Caltech)T. von Rosenvinge, M.H. Acuna (GSFC)R. Mueller-Mellin, H. Kunow (U. of Kiel)G.M. Mason (U. of Maryland)M. Wiedenbeck (JPL)A. Sauvaud, C. Aoustin (CESR/CNRS)A. Korth (MPAe)T. Sanderson (ESTEC)C.T. Russell (UCLA)P. Riley and J.A. Linker (SAIC) D. Odstrcil and V.J. Pizzo (CIRES and NOAA-SEC)W. Abbett and Y. Li (UCB)C.N. Arge (AFRL)

http://www.bu.edu/cism/index.html

Luhmann2


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

STE-U

SEPSEPT-E

SEP LET,HET, SIT

MAG, STE-D

SWEA

• 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 Boom– SEP Central– Instrument Data Processing Unit

(IDPU)

Luhmann3


IMPACT Team Member Institutions and Primary Roles

Luhmann4


STEREO Mission Objectives that IMPACT & CISM Models Address

• Understand the causes and mechanisms of CME initiation

• Characterize the propagation of CMEs through the heliosphere

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

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

Luhmann5


Overall IMPACT Investigation Rationale I.

Luhmann6


Overall IMPACT Investigation Rationale II.

•FOV coverage: •~4π solar wind and heat flux electron coverage to meet solar wind electron and magnetic topology objectives

•Parker Spiral orientations of suprathermal and energetic particle FOVs on both spacecraft- both toward and away from Sun to detect counterstreamingor backstreaming from ICME shock source

•North-South (out of ecliptic) energetic particle measurements to detect SEPsin highly inclined magnetic field situations during ICMEs and periods of isotropic distributions

•Energy Coverage to accomplish solar wind, magnetic topology, and SEP distribution function and source identification objectives

•Ion Composition to accomplish SEP source objectives

•Clean magnetic measurements to organize and interpret particle observations and deduce solar wind and ICME magnetic topology

Luhmann7


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)

Luhmann8


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

Luhmann9


IMPACT Directional Coverage

Parker Spiral

Earth

Leading spacecraft

Mercator projection of 4 π angular coverage sphere. Sun in center. Contours show statistics of interplanetary field direction. Dark lines show IMPACT particle instrument fields of view.

Luhmann10


SEP Ions Spectral Coverage

Luhmann11


SEP Ions Composition Coverage

SEPTSEPT

Luhmann12


IMPACT uses multipoint measurement to locate ICME and/or flare acceleration site(s) of SEP

Luhmann13


Acceleration Sites can be Inferred from SEP Timing

Luhmann14


Locating Acceleration Sites and Inferring Magnetic Topology Using IMPACT Electrons

(see next page)

WIND SWEA, STE and SEPT-type electron measurements

Electron velocity dispersion gives field line length, topology

Radio burst gives electron injection times

SWEA-type electrons indicate ICME field lines solar connectivityField line length in ICME model vs. inferred length

Luhmann15


Image of Possible Flare Source of Electrons (from Yohkoh SXT) in the previous figure

(figures from Davin Larson, UCB)

Flare near connected field lines

spacecraft trajectory

Suprathermal electrons

Counter streaming heat flux electrons

Luhmann16


Magnetic Topology Measurements Using Magnetic Fields

(flux rope fits by Tamitha Mulligan,UCLA, from the paper by Yan Li et al., JGR 2001)

Spacecraft sampling

“Fly Through” Model ICME Flux Rope (or other models) to reproduce Vector Field observations.

Luhmann17


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

Luhmann18


A Major Challenge will be to Integrate Multipoint Measurements of ICMEs and SEPs with the Images

Example from Helios 1/2 data for Carrington Rotation 1663 (left), Spacecraft locations (bottom), and SECCHI image placeholder from SOHO (S. Yashiro CDAW website images)

Special browsers need to be designed.

Luhmann19


…will also require models

Luhmann20


InnerMagnetosphere

The CISM Coupled Modeling Scheme offers one approach.

Solar CoronaSAIC

Solar WindENLIL Ionosphere

T*GCM

Active Regions

SEP

Ring Current

Radiation Belts

Geocorona and Exosphere

Plasmasphere

MI Coupling

MagnetosphereLFM

Solar CISM

Luhmann21


Find out about Solar/Heliospheric CISM athttp://sprg.ssl.berkeley.edu/cism

Luhmann22


CISM Coupled Coronal and Solar Wind Computational Grids merge coronal and heliospheric domains

Figure courtesy of Dusan Odstrcil, CIRES

Photospheric boundary conditions

MAS Coronal Model Grid ENLIL Solar Wind Model Grid

Luhmann23


Simulated Eruption and Evolution of Active Regions

Left: simulated flux rope emerges into the photosphere. Field lines are overplotted on the gray scale active region “magnetograms” indicating field strength and polarity.

Right: constructed global magnetic field maps using a dipole background and the radial component of the emerging flux rope simulation.

Images courtesy of Bill Abbett and Yan Li, UCB

Luhmann24


Coronal Adjustments to Active Regions Can Be Studied

Simulated coronal images using the plasma density of the MHD model to calculate polarization brightness (pB). The streamer belt on the right is distorted and separates into two streamers. The transient behavior is under investigation.

Snapshot of Global MHD Model field lines with the active region located at the right limb. As the active region emerges, the field lines and streamer belt are distorted.Images courtesy of Jon Linker and Zoran Mikic, SAIC

Luhmann25


Ambient Solar Wind Source Models and Data Comparisons Can Be Made

Top figure shows open field footpoints color coded with solar wind velocity.

Bottom figure shows interplanetary field polarity.

At right stream structure projected on ecliptic plane and in meridional cut (top). Comparisons with in situ observations (bottom).

Images courtesy of Nick Arge, AFRL and Dusan Odstrcil, CIRES

Luhmann26


Modeling of CMEs will physically connect IMPACT in situ observations to SECCHI images

(Shown: SAIC CME model, CISM merged CME/Solar Wind model)

Simulated time series in situ

Simulated coronal eruption (CME)

Simulated corona-graph image (right)

Inter-planetary transport (ICME)

Images courtesy of Jon Linker, SAIC, and Dusan Odstrcil, CIRES

Luhmann27


Ambient Solar Wind

Detail of an ad-hoc simulated CME in the model solar wind

ICME Shock and Sheath

ICME Flux Rope Field Lines

Image courtesy of Dusan Odstrcil, CIRES

Luhmann28


Shock Front Surface

Conditions for Energetic Particles Transport are derived from the model

Magnetic Field Lines

theta = 90 deg

theta = 60 deg

theta = 70 deg

theta = 80 deg

Magnetic field lines, as observed at given locations can be:(a) part of the magnetic flux rope;(b) connected to the solar surface; or(c) disconnected from the solar surface.

Luhmann29


Simulated In Situ Data can be generated at any 1AU location

Plasma Density

Plasma Temperature

Velocity X Component

Velocity Y Component

Velocity Z Component

Total B Field

B Field X Component

B Field Y Component

B Field Z Component Image courtesy of Dusan Odstrcil, CIRES

Luhmann30


Multiperspective and Multi-Point Models hold the potential for STEREO event simulations from Sun to 1AU

White light images of a simulated modeled CME event from 3 perspectives. In-situ data corresponding to the viewer location are readily obtainable.Image courtesy of Dusan Odstrcil, CIRES

STEREO IMPACT Measurements and CISM...

Documents

Transcript of STEREO IMPACT Measurements and CISM...