HR: 14:00h
AN: SP43C-02 [Abstracts]
TI: 3D Numerical Simulations of the Breakout Model
AU: * Lynch, B J
EM: lynchb@engin.umich.edu
AF: AOSS Department,
University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109 United States
AU: * Lynch, B J
EM: lynchb@engin.umich.edu
AF: E. O. Hulburt Center for Space Research, Naval Research Lab, 4555 Overlook Ave. SW, Washington, DC
20375 United States
AU: Antiochos, S K
EM: antiochos@nrl.navy.mil
AF: AOSS Department,
University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109 United States
AU: Antiochos, S K
EM: antiochos@nrl.navy.mil
AF: E. O. Hulburt Center for Space Research, Naval Research Lab, 4555 Overlook Ave. SW, Washington, DC
20375 United States
AU: DeVore, C R
EM: devore@lcp.nrl.navy.mil
AF: Laboratory for Computational Physics & Fluid Dynamics, Naval Research Lab, 4555 Overlook Ave. SW,
Washintgon, DC 20375 United States
AU: Zurbuchen, T H
EM: thomasz@umich.edu
AF: AOSS Department,
University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109 United States
AB:
We present the continuing progress of the numerical simulations of the breakout model for coronal mass ejection initiation.
To validate the 3D spherical ARMS code we have run the 2.5D breakout problem and compare the eruption to the published 2D
results. The ARMS 2.5D CME also forms a large magnetic island ahead of the erupting plasmoid due to the code's excellent
maintenance of equatorial symmetry.
Progress on the fully 3D breakout problem is also discussed. To build up enough magnetic free energy for an eruption the
active region field must be strong with a steep gradient near the polarity inversion line and the shear must be highly
concentrated there. This requires adaptive griding techniques. In the current simulation, the active region to background
field ratio is 20-to-1 and the neutral line is long compared to the active region width. We present the evolution of this
topology under Br-conserving shearing flow and discuss implications for a 3D eruption.
This work is supported by NASA and ONR. BJL is supported by NASA GSRP grant NGT5-50453.
DE: 7509 Corona
DE: 7513 Coronal mass ejections
DE: 7524 Magnetic fields
DE: 7835 Magnetic reconnection
DE: 7843 Numerical simulation studies
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly