HR: 0800h
AN: SM11A-1171    [Abstracts]
TI: Formation of Plasmoids and Magnetic Flux Ropes during Southward IMF
AU: * Karimabadi, H
EM: homa@ece.ucsd.edu
AF: UCSD, 950 Gilman Drive, Dept. of ECE, MC 0407, La Jolla, ca 92093-0407 United States
AU: Omidi, N
EM: omidi@adelphia.net
AF: UCSD, 950 Gilman Drive, Dept. of ECE, MC 0407, La Jolla, ca 92093-0407 United States
AU: Vu, H X
EM: hxv@101freeway.com
AF: UCSD, 950 Gilman Drive, Dept. of ECE, MC 0407, La Jolla, ca 92093-0407 United States
AB: We have shown previously that 2D global hybrid (electron fluid, kinetic ions) simulations capture correctly the physics of the many of the important boundaries in the Earth's magnetosphere. Given that 2D simulations are much less CPU intensive than 3D, we have used them more extensively to study kinetic structure of magnetospheres. Here we report on the results of simulations during southward IMF and the structure of plasmoids and flux ropes formed at the magnetopause. These structures undergo large changes as they are convected away from their point of origin. This can include coalescence of multiple magnetic islands, changes in the core field and other internal structures. There are two effects that can lead to differences in regards to dynamics of reconnection in 2D versus 3D global simulations: (1) In 2D, only plasmoids can form whereas in 3D it becomes possible to form magnetic flux ropes with varying pitch angle. (2) In 3D the plasma flow around the obstacle is more complex whereas in 2D it is confined to one plane. The consequences and relative importance of these two effects will be illustrated.
DE: 7835 Magnetic reconnection
DE: 7843 Numerical simulation studies
DE: 2700 MAGNETOSPHERIC PHYSICS
DE: 2724 Magnetopause, cusp, and boundary layers
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting