CISM Advisory Council Meeting 4 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling

CISM Advisory Council Meeting 4 March 2003

Janet Luhmann

and the Solar CISM Modeling Team

Solar and Interplanetary Modeling


InnerMagnetosphere

Coupled Modeling Scheme

Solar Corona SAIC

Solar Wind ENLIL Ionosphere

T*GCM

Active Regions

SEP

Ring Current

Radiation Belts

Geocorona and Exosphere

Plasmasphere

MI Coupling

MagnetosphereLFM

Solar CISM


Solar CISM Participants


Solar CISM Organizational Activities Since STC Selection

Participated in BU Kickoff Meeting (Sept. ‘02) Met with collaborators at ‘02 SPD and SHINE Meetings Posted SolarCISM website (http://sprg.ssl.berkeley.edu/cism) Collaborated on CISM-related SF Exploratorium EPO proposal to NASA IDEAS

Program Held first annual SSL SolarCISM meeting in Dec. ‘02 (26 participants from 14

institutions) Advertised two UCB CISM positions (NRL liaison and UCB Senior Fellow for

SEP), also filled HAO liaison position Interacted with KT group on CISM Empirical Model contribution for corona/solar

wind (Arge) Identified potential Access Grid rooms at UCB, SAIC, Stanford now working with

BU to purchase and install equipment Participated in bimonthly executive telecons Multi-institution working subgroups met at HAO/U of Colo., UCB, and SAIC


Solar CISM WebsiteNow Available

http://sprg.ssl.berkeley.edu/cism


SAIC and CIRES/NOAA SEC Coronal and Heliospheric Modeling For

CISM: Pre-STC and 1st Year CISM Results

Performed propagation of 2D CME in the

coupled model, studied results.

Performed large-angle 3D CME in the coupled

model.

Performed 3D simulation of emerging Active

Region.

Developing new MPI version of the coronal code

which is currently in testing.

Introduced rotation into the 2D CME

calculation: spiral magnetic field modifies

shock characteristics.

Investigated in situ properties of simulated

CMEs.


Coronal/Heliospheric Modeling For CISM (Continued)

Developing new MPI version of the coronal

code which is currently in testing.

Introduced rotation into the 2D CME

calculation: spiral magnetic field modifies

shock characteristics.

Investigated in situ properties of simulated

CMEs.

Studied the extension of the Wang-Sheeley

approach using the NOAA/SEC heliospheric

MHD model.

Investigated STEREO views of a simulated

CME.

Publications:

1) Odstrcil et al., J. Geophys. Res. 107, 10.1029/2002JA009334, 2002

2) Riley et al., Astrophys. J. 578, 972, 2002

3) Linker et al., Phys. Plasmas, to appear, 2003


Current SAIC + U. Colorado CISM EffortTwo dimensional flux rope eruption simulation

undergoing improvements (e.g. in coronal/solar wind model coupling and spatial resolution)


Expanding Magnetic Flux Rope -Initial 3D Version Developed

Model Interface

Compressed Plasma

Shock

Magnetic LegEjected Plasma


Evidence of Post-Eruption Reconnection Jet- samples of visualizations and diagnostics


Conditions for Energetic Particles

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.

Shock Front Surface Magnetic Field Lines

theta = 90 deg

theta = 60 deg

theta = 70 deg

theta = 80 deg


Multi-Perspective Imaging- sample of application to heliospheric imaging

observations from SMEI and STEREO


UCB + SAICEmerging active region magnetic fields effects on

the coronal field configuration

Steps to provide constructed magnetic field maps to SAIC to be the boundary condition for their MHD models:

1. Perform a local ANMHD simulation of an emerging fluxrope.

2. Use the radial component of the fluxrope as it emerges up into the photosphere to be the active region field.

3. Make a global background field, i.e., a dipole field.

4. Insert the series of simulated active region field into the background field.

5. SAIC uses the series of synthetic synoptic maps as boundary condition and starts with a potential field to perform their global MHD model to generate coronal field lines, coronal hole areas and coronal streamer belt images.


Current UCB + SAIC CISM EffortInitiation of Coronal Eruptions

UCB simulation of emergence of an active region from below the photosphere into the corona –provides sample boundary conditions for the SAIC corona model.


Current UCB + SAIC Effort(continued)

a) Transverse magnetic field vectors b) Transverse velocity vectors and radial magnetic field contours

The simulated emerging active region model coupling tells us how to better use observations to drive the coronal model.


Left: ANMHD flux rope as it emerges up to the photosphere. Field lines are overplotted on the gray scale active region images.

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


SAIC’s global MHD model results using the constructed maps as the inner boundary condition. The evolving photospheric field maps are here shown in a blue-white-red color scheme. The green lines are initially closed field lines, and black lines are initially open.

SAIC’s global MHD model results. The green lines are initially closed field lines, and black lines are initially open. The dark gray areas are coronal holes.


A different perspective of the global MHD field lines with the active region located at the right side. As the active region emerges, the field lines and streamer belt are distorted.

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.


HAO + U of Colorado + NOAA/SEC + UCB + Lockheed CISM Effort

HAO

Synoptic map project (de Toma, Arge, Gibson, & Mayer) Global coronal magnetic field-solar wind relationships (Gibson & Arge)

NOAA/SEC

Wang-Sheeley-Arge (WSA) empirical coronal/solar wind model (Arge, Pizzo, & Mayer) WSA coronal and Odstrcil MHD solar wind model coupling (Odstrcil, Arge, & Pizzo)

CU/LASP

Incorporation of the WSA model into the CISM Sun-to-Earth Empirical

Model (CSEM) (Baker, Weigel, Arge, & Mayer)

UC Berkeley

Solar event studies (Luhmann, Arge, & Li)

Lockheed

Incorporation of Schrijver-Derosa photospheric field evolution model into WSA. (Arge, Schrijver, & DeRosa)


HAO + U of Colorado + Stanford Synoptic Map Projects

At HAO: Routine construction of solar/coronal synoptic maps

He 10830 Å H (HAO) White light Photospheric field (NOAA/SEC)

IDL software package will be made available to solar community.


HAO + U of Colorado + Stanford Synoptic Map Projects

Event-specific modified maps

Magnetic field from WSO Magnetic field from MDI mag

Intensity from MDI

EIT 171Å EIT 254Å

EIT 195Å EIT 304Å

At Stanford:


Near Solar Maximum

2.5 R

21.5 R

Schatten Current Sheet Model (SCS): 2.5 – 21.5 R

Coupled Model: PFSS+SCS

L1

U of Colorado + NOAA/SEC Empirical Wang-Sheeley-Arge Model provided to CISM KT group

Near Solar Minimum

1D Modified Kinematic Solar Wind ModelPotential

Field Source Surface Model (PFSS): 1.0 – 2.5 R


Level 1 Data Flow Diagram for WSA IDL Fortran PERL

Hourly Ace DATA

Assemble latest WSO Daily

Updated Synoptic Map

2 3Convert LOS

Photospheric B Field to Radial, Interpolate

Grid, & Subtract Monopole

5Potential Field Source

Surface Model withField Line Tracing

4

Generate Date File

Predict Solar WindSpeed and IMF Polarity at 1 AU

6

7 Plot Photospheric Field,Derived Coronal Holes,Source Surface Field,

Solar Wind Speed

Latest Synoptic Map

Date, Time, File name of Synoptic Maps

Interpolated Map

Date File for Last Three Rotations

Solar Wind Speed andIMF Polarity Predictions for Last Three Rotations

Photospheric FieldDerived Coronal HolesSource Surface FieldField Expansion Factor

Output from PreviousPFSS Model Runs(Last 3 Rotations)

Plot Solar WindSpeed and IMF Polarity

Predictions Against Real-Time ACE

Observations

9

Magnetograms

Retrieve Latest WSO

Magnetograms

1

8Retrieve Last 24 Hours of ACE

Velocity & IMF Observations


U of Colorado + NOAA/SECWSA Coronal - Odstrcil MHD Solar Wind Model Coupling

PFSS model now generalized to work for different grid resolutions.

A new & improved photospheric field remapping routine written.

Work on improving the interface between the models.

Working to inter-calibrate models better.


Calibration Study – Near Solar Minimum( CR 1954 )

0.1 AU 1 AU

Low inclination of the streamer belt causes difficulties

in timing of fast streams


Calibration Study – Near Solar Maximum( CR 1954 )

0.1 AU 1 AU

•Source-Surface models are applicable at solar maximum• Amplitudes need to be balanced


Selected CISM Solar Event: May 12, 1997 CME

Photospheric field from SOHO MDI

SOHO EIT EUV observations

SOHO LASCO C2 and C3 observations


Selected CISM Solar Event: May 12, 1997 CME (continued) This flare was probably caused by magnetic cancellation The filament disappeared during the flare but did not appear to erupt

SOHO MDI MagnetogramsHiraiso/CRL H_alpha


Selected CISM Solar Event: May 12, 1997 CME (continued)

WIND and SAMPEX observations


UCB + SAIC + Stanford Driving MHD codes with

sequences of magnetograms Physically consistent evolution at bottom plane

in a simulation: Terms on LHS describe evolution driven by

horizontal motion; RHS describes evolution due to flux emergence or submergence

This requires knowledge of vector components of B and v.

How do we determine v self-consistently from a sequence of vector magnetograms (which give only B)?

Price for ignoring the problem: Incorrect coronal magnetic topology

)()(

Bv zzt

vBBz


UCB + SAIC + Stanford Driving MHD codes with

sequences of magnetogramsVector magnetic field data show no obvious change before and after the flare.


UCB + SAIC + Stanford (continued)Exploring methods for finding the

velocity boundary conditions:

Stokes Profiles could be used to get vz

Local Correlation Tracking (LCT) can find a velocity field v (But is it correct?)

Vertical component of induction equation provides a constraint equation on v from a sequence of vector magnetograms (but solution is under-constrained)

Kusano et al. used combination of LCT and vertical induction equation to solve for vz

Longcope has developed a solution by adding an additional constraint: minimize the horizonal kinetic energy. Method appears to work in some cases, but not yet thoroughly tested.

AR 8038 May 12, 1997


UCB + SAIC + Stanford (continued)Stanford force-free models may help set up the

initial conditions for MHD simulations

Potential field modelsNon-linear force-free

models

Active region field lines

Synoptic display of global field lines 1.0-1.4 Rs


UCB + SAIC + Stanford (continued)Non-linear force-free fields contain free energy to be released in the eruptive events, while the potential field doesn’t. Extrapolation of the force-free field incorporates all three components of the magnetic field, and therefore reflects a more realistic structure of the corona.

Description of non-linear force-free field modeling approach

The technique used is the Boundary Element Method (BEM) developed by Yan, et al. ( Yan & Sakurai, 2000);

The technique needs the three components of the magnetic field at the surface as inputs;

To prepare the vector magnetograms for boundary conditions:

compute potential field from the synoptic maps of magnetic field;

obtain the three components of the potential field on the surface;

replace the vector field data where observation of vector magnetic field are unavailable.


U of Colorado and UCBSolar Event: May 12, 1997 Solar Wind and Stream Context

Derived Coronal Holes and Photospheric Field Polarity

Solar Wind Speed at Source Surface (2.5Rs)Solar Wind Speed Predictions & Observations

PredictionsObservations

IMF Polarity Predictions & Observations

Stream source region

Stream source region

May 12th CME

(suggests solar wind stream following the ICME comes from the southern hemisphere)


Solar CISM Modeling Near-Term Issues and Challenges

Improve ambient solar wind MHD simulation to give realistic speeds and stream structure

Collect needed resources for model coupling and driving (e.g. potential or force-free field models and/or synoptic maps as initial states + boundary conditions, vector magnetograms)

Develop solar energetic particle (SEP) modeling capability

Establish NRL connection

Standardize simulation and other data formats and visualization tools

Track progress (e.g. against implementation plan, metrics)

Documents

CISM Advisory Council Meeting 4 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling