Presentation is loading. Please wait.

Presentation is loading. Please wait.

Tucson MURI SEP Workshop 17-18 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling.

Published by Modified over 9 years ago

Similar presentations

Presentation on theme: "Tucson MURI SEP Workshop 17-18 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling."— Presentation transcript:

1 Tucson MURI SEP Workshop 17-18 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling

2 Tucson MURI SEP Workshop 17-18 March 2003 Inner Magnetosphere 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 Magnetosphere LFM Solar CISM

3 Tucson MURI SEP Workshop 17-18 March 2003 Solar CISM Participants

4 Tucson MURI SEP Workshop 17-18 March 2003 Solar CISM Website Now Available  http://sprg.ssl.berkeley.edu/cism

5 Tucson MURI SEP Workshop 17-18 March 2003 Current SAIC + U. Colorado CISM Effort Two dimensional flux rope eruption simulation undergoing improvements (e.g. in coronal/solar wind model coupling and spatial resolution)

6 Tucson MURI SEP Workshop 17-18 March 2003 Expanding Magnetic Flux Rope - Initial 3D Version Developed Model Interface Compressed Plasma Shock Magnetic Leg Ejected Plasma

7 Tucson MURI SEP Workshop 17-18 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

8 Tucson MURI SEP Workshop 17-18 March 2003 Current UCB + SAIC CISM Effort Initiation 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.

9 Tucson MURI SEP Workshop 17-18 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.

10 Tucson MURI SEP Workshop 17-18 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.

11 Tucson MURI SEP Workshop 17-18 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.

12 Tucson MURI SEP Workshop 17-18 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 Model Potential Field Source Surface Model (PFSS): 1.0 – 2.5 R 

13 Tucson MURI SEP Workshop 17-18 March 2003 U of Colorado + NOAA/SEC WSA 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.

14 Tucson MURI SEP Workshop 17-18 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

15 Tucson MURI SEP Workshop 17-18 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

16 Tucson MURI SEP Workshop 17-18 March 2003 Selected CISM Solar Event: May 12, 1997 CME (continued) WIND and SAMPEX observations

17 Tucson MURI SEP Workshop 17-18 March 2003 U of Colorado and UCB Solar 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 Predictions Observations IMF Polarity Predictions & Observations Stream source region May 12 th CME (suggests solar wind stream following the ICME comes from the southern hemisphere)

18 Tucson MURI SEP Workshop 17-18 March 2003 CISM Near Term Plans Relating to SEP Modeling  In process of hiring a new UCB Senior Fellow to work with Ilan Roth and Dusan Odstrcil  Learn to work with MHD model results as background  Gather data for May 12 th 1997 case study

Download ppt "Tucson MURI SEP Workshop 17-18 March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling."

Similar presentations

Heliospheric Computations Dusan Odstrcil University of Colorado/CIRES and NOAA/Space Environment Center Solar MURI Team Meeting, Berkeley CA, December.

Heliospheric Computations Dusan Odstrcil University of Colorado/CIRES and NOAA/Space Environment Center Solar MURI Team Meeting, Berkeley CA, December.
ESS 7 Lecture 14 October 31, 2008 Magnetic Storms

ESS 7 Lecture 14 October 31, 2008 Magnetic Storms
Using Potential Field Models to Learn About CME Coronal Context and Consequences J.G. Luhmann and Yan Li (Space Sciences Lab, UCB) C.N. Arge (CIRES, U.

Using Potential Field Models to Learn About CME Coronal Context and Consequences J.G. Luhmann and Yan Li (Space Sciences Lab, UCB) C.N. Arge (CIRES, U.
“Insights” on Coronal Hole Magnetic Fields From a High-Order PFSS Model D.J. Bercik and J.G. Luhmann Space Sciences Lab, UC Berkeley 1 FEW 2011, Aug 24.

“Insights” on Coronal Hole Magnetic Fields From a High-Order PFSS Model D.J. Bercik and J.G. Luhmann Space Sciences Lab, UC Berkeley 1 FEW 2011, Aug 24.
Heliospheric MHD Models (for the LWS Community) LWS Workshop, Boulder, CO, March 23-26, 2004 Dusan Odstrcil 1,2 and Vic Pizzo 2 1 University of Colorado/CIRES,

Heliospheric MHD Models (for the LWS Community) LWS Workshop, Boulder, CO, March 23-26, 2004 Dusan Odstrcil 1,2 and Vic Pizzo 2 1 University of Colorado/CIRES,
Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3, 2004 Dusan Odstrcil University of Colorado/CIRES &

Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3, 2004 Dusan Odstrcil University of Colorado/CIRES &
A General Cone Model Approach to Heliospheric CMEs and SEP Modeling Magnetogram-based quiet corona and solar wind model The SEPs are modeled as a passive.

A General Cone Model Approach to Heliospheric CMEs and SEP Modeling Magnetogram-based quiet corona and solar wind model The SEPs are modeled as a passive.
1 SDO/HMI Products From Vector Magnetograms Yang Liu – Stanford University

1 SDO/HMI Products From Vector Magnetograms Yang Liu – Stanford University
Synoptic maps and applications Yan Li Space Sciences Laboratory University of California, Berkeley, CA HMI team meeting, Jan 27, 2005, Stanford.

Synoptic maps and applications Yan Li Space Sciences Laboratory University of California, Berkeley, CA HMI team meeting, Jan 27, 2005, Stanford.
Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.
Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.
Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.

Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.
1 WSA Model and Forecasts Nick Arge Space Vehicles Directorate Air Force Research Laboratory.

1 WSA Model and Forecasts Nick Arge Space Vehicles Directorate Air Force Research Laboratory.
C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.

C. May 12, 1997 Interplanetary Event. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC.
CISM solar wind metrics M.J. Owens and the CISM Validation and Metrics Team Boston University, Boston MA Abstract. The Center for Space-Weather Modeling.

CISM solar wind metrics M.J. Owens and the CISM Validation and Metrics Team Boston University, Boston MA Abstract. The Center for Space-Weather Modeling.
The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.

The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.
Expanded Observatory support (redundancy, verification) CME (Empirical) propagation (Cone Model) (ICME strength and arrival time) Electrodynamics model.

Expanded Observatory support (redundancy, verification) CME (Empirical) propagation (Cone Model) (ICME strength and arrival time) Electrodynamics model.
When will disruptive CMEs impact Earth? Coronagraph observations alone aren’t enough to make the forecast for the most geoeffective halo CMEs. In 2002,

When will disruptive CMEs impact Earth? Coronagraph observations alone aren’t enough to make the forecast for the most geoeffective halo CMEs. In 2002,
February 26, 2007 KIPAC Workshop on Magnetism Modeling/Inferring Coronal And Heliospheric Field From Photospheric Magnetic Field Yang Liu – Stanford University.

February 26, 2007 KIPAC Workshop on Magnetism Modeling/Inferring Coronal And Heliospheric Field From Photospheric Magnetic Field Yang Liu – Stanford University.
Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results S. A. Ledvina 1, D. Odstrcil 2 and J. G. Luhmann 1 1.Space Sciences.

Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results S. A. Ledvina 1, D. Odstrcil 2 and J. G. Luhmann 1 1.Space Sciences.

Similar presentations

Ads by Google