HR: 0800h
AN: SH21B-0400 [Abstracts]
TI: 3D Breakout: Preliminary Results
AU: * Lynch, B J
EM: lynchb@engin.umich.edu
AF: Atmospheric, Oceanic, and Space Sciences Dept., 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 Laboratory, 4555 Overlook Ave. SW, Washington,
DC 20375
United States
AU: Antiochos, S K
EM: antiochos@nrl.navy.mil
AF: Atmospheric, Oceanic, and Space Sciences Dept., 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 Laboratory, 4555 Overlook Ave. SW, Washington,
DC 20375
United States
AU: DeVore, C R
EM: devore@lcp.nrl.navy.mil
AF: Laboratory for Computational Physics and Fluid Dynamics, Naval Research Laboratory, 4555 Overlook Ave.
SW, Washington, DC 20375
United States
AU: Zurbuchen, T H
EM: thomasz@umich.edu
AF: Atmospheric, Oceanic, and Space Sciences Dept., University of Michigan, 2455 Hayward St., Ann Arbor, MI
48109
United States
AB:
We present preliminary results of the breakout model for solar coronal mass ejections in a global-scale 3D topology. Starting
with a background dipole field, we use a series of point dipole sources create a latitudinally extended ($\sim 100^o$)
delta-spot active region configuration with a null point high in the corona. This is the natural 3D extension of our very
successful 2.5D case. Magnetic free energy is added to the initial field configuration via two compressible vortex flows that
preserve $B_r$ at the surface and concentrate the shear near the central neutral line of the AR flux system. Reconnection at
the null point removes the restraining overlying flux allowing rapid, unstable expansion of the innermost sheared field. We
examine the evolution of the system and discuss its implications for a fully 3D breakout eruption. We also discuss
observational tests of the breakout model that can be performed with the unique viewing capabilities of STEREO.
This work is supported in part by NASA and ONR.
DE: 7509 Corona
DE: 7513 Coronal mass ejections
DE: 7524 Magnetic fields
DE: 7835 Magnetic reconnection
DE: 7843 Numerical simulation studies
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting