CISM Advisory Council Meeting 4 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling.
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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
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
CISM Advisory Council Meeting 4 March 2003
Solar CISM Participants
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
Solar CISM WebsiteNow Available
http://sprg.ssl.berkeley.edu/cism
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 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)
CISM Advisory Council Meeting 4 March 2003
Expanding Magnetic Flux Rope -Initial 3D Version Developed
Model Interface
Compressed Plasma
Shock
Magnetic LegEjected Plasma
CISM Advisory Council Meeting 4 March 2003
Evidence of Post-Eruption Reconnection Jet- samples of visualizations and diagnostics
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
Multi-Perspective Imaging- sample of application to heliospheric imaging
observations from SMEI and STEREO
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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)
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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:
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
Selected CISM Solar Event: May 12, 1997 CME
Photospheric field from SOHO MDI
SOHO EIT EUV observations
SOHO LASCO C2 and C3 observations
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
Selected CISM Solar Event: May 12, 1997 CME (continued)
WIND and SAMPEX observations
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
UCB + SAIC + Stanford Driving MHD codes with
sequences of magnetogramsVector magnetic field data show no obvious change before and after the flare.
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
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
CISM Advisory Council Meeting 4 March 2003
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.
CISM Advisory Council Meeting 4 March 2003
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)
CISM Advisory Council Meeting 4 March 2003
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)
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