HR: 14:30h
AN: SP43C-04    [Abstracts]
TI: Resistive MHD Modeling of CME Acceleration and Impulsive Magnetic Reconnection
AU: Ren, Y
EM: yren@pppl.gov
AF: Princeton University, PPPL, Princeton, NJ 08543 United States
AU: * Cheng, C Z
EM: fcheng@pppl.gov
AF: Princeton University, PPPL, Princeton, NJ 08543 United States
AU: Choe, G S
EM: gchoe@pppl.gov
AF: Princeton University, PPPL, Princeton, NJ 08543 United States
AU: Qiu, J
EM: qiuj@bbso.njit.edu
AF: BBSO, NJIT, Big Bear City, CA United States
AB: CME (or Flux rope) acceleration and impulsive magnetic reconnection are modeled by resistive MHD simulations with anomalous resistivity. We discuss the role of nonuniform anomalous resistivity on the time scale of flux rope acceleration and reconnection rate. Our simulation results show that the reconnection electric field reaches a peak value of O(1 keV) for X-class flares during the GOES X-ray flare rise phase, which is consistent with estimates obtained from several observations of two ribbon expansion in flare-CME events. Our simulations provide quantitative agreement with observations of CME acceleration during the flare rise phase and predict an enhanced magnetic reconnection rate during this period. We will discuss the physical scenario of how the phenomenological anomalous resistivity can be created in collisionless turbulent plasmas in the current sheet, how the current sheet can be significantly wider than the ion skin depth, and how particles are accelerated in the globally evolving EM fields with turbulence in the current sheet.
DE: 7513 Coronal mass ejections
DE: 7519 Flares
DE: 7524 Magnetic fields
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly