HR: 1340h
AN: SH53B-0306    [Abstracts]
TI: Numerical MHD Simulation of Key Parameters for CME Initiation
AU: * Wu, S
EM: wus@cspar.uah.edu
AF: Center for Space Plasma & Aeronomic Research, The University of Alabama in Huntsville, Technology Hall, Room S101, Huntsville, AL 35899 United States
AU: * Wu, S
EM: wus@cspar.uah.edu
AF: Department of Mechanical & Aerospace Engineering, The University of Alabama in Huntsville, Huntsville, AL 35899 United States
AU: Wang, A
EM: wanga@cspar.uah.edu
AF: Center for Space Plasma & Aeronomic Research, The University of Alabama in Huntsville, Technology Hall, Room S101, Huntsville, AL 35899 United States
AU: Falconer, D A
EM: David.A.Falconer@msfc.nasa.gov
AF: Department of Physics, The University of Alabama in Huntsville, Huntsville, AL 35899 United States
AU: Falconer, D A
EM: David.A.Falconer@msfc.nasa.gov
AF: SD 50, NASA/Marshall Space Flight Center, NSSTC, 301 Sparkman Drive, Huntsville, AL 35899 United States
AU: Fry, C D
EM: fryc@cspar.uah.edu
AF: Center for Space Plasma & Aeronomic Research, The University of Alabama in Huntsville, Technology Hall, Room S101, Huntsville, AL 35899 United States
AU: Fry, C D
EM: fryc@cspar.uah.edu
AF: Exploration Physics International, Space Weather & Planetary Science, 6275 University Drive, Suite 37-105, Huntsville, AL 35806-1776 United States
AB: Recently, Falconer et al. (2002) have developed a set of physical parameters to correlate the coronal mass ejection productivity of solar active regions with measures of their non-potentiality from vector magnetograms. In this presentation, we will use a newly developed three-dimensional, time-dependent, magnetic field transport model with magnetohydrodynamic (MHD) effects, which is named the Photospheric Surface Dynamo (PSD) model. This model is based on MHD theory with additional physics of the photosphere including differential rotation and meridional flow. Thus, the inertial centrifugal force and the coriolis force which are usually not taken into account in the MHD equations are included. In addition, the effect of diffusion due to random motion of the granules or super-granules and cyclonic turbulence are also included. This model is used to simulate those CME production parameters: (i) the magnetic flux content ($\Phi)$ of the active region, (ii) the length of strong-shear, strong-field main neutral line ($L_{ss}$), (iii) the net electric current ($I_n$) and (iv) a flux-normalized measure of the field twist ($\alpha = \mu I_n / \Phi$), suggested by Falconer et al. (2002). An example is given by using SOHO/MDI magnetic field measurements of AR8100, recorded from October 31, - November 3, 1997. These simulated parameters show good agreement with the observations.
DE: 7513 Coronal mass ejections
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting