HR: 1340h
AN: SH13A-0276    [Abstracts]
TI: A Simple Dynamical Model for Filament Formation in the Solar Corona
AU: * Litvinenko, Y
EM: yuri.litvinenko@unh.edu
AF: UNH Space Science Center, 39 College Rd, Durham, NH 03824 United States
AB: Filament formation in the solar corona is considered in the case of a slowly evolving force-free magnetic field. The strong-field approximation is used, which takes into account the magnetohydrodynamic equations of motion, induction, and compressibility. Methods for solving the relevant equations are presented and applied to filament modeling. A three-dimensional calculation is presented, which uses linear force-free magnetic fields. The boundary conditions are chosen to resemble the qualitative linkage model for the formation of filaments, suggested by Martens and Zwaan (2001). Consistent with this model, dense formations, reminiscent of filament pillars, are shown to appear in the corona above the region of converging and canceling magnetic bipoles. The results demonstrate the principal role of magnetic field in the dynamical processes of dense plasma accumulation and support in filaments. The model can be useful for clarifying the role of flux emergence in coronal mass ejection initiation.
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7531 Prominence eruptions
DE: 7833 Mathematical and numerical techniques (0500, 3200)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005