HR: 0800h
AN: SH11A-0246    [Abstracts]
TI: MHD Simulation of the Global Solar Corona Using the Synoptic Frame of the Photospheric Magnetic Field
AU: * Hayashi, K
EM: keiji@quake.stanford.edu
AF: W.W.Hansen Experimental Physics Lab., Stanford University, 445 Via Palou, Stanford, CA 94305 United States
AU: Zhao, X
EM: zhao@quake.stanford.edu
AF: W.W.Hansen Experimental Physics Lab., Stanford University, 445 Via Palou, Stanford, CA 94305 United States
AU: Liu, Y
EM: yliu@quake.stanford.edu
AF: W.W.Hansen Experimental Physics Lab., Stanford University, 445 Via Palou, Stanford, CA 94305 United States
AB: As the proxy of the entire surface distribution of the photospheric magnetic field at a specific time, the synoptic frame of the photospheric magnetic field [Zhao et al., 1999] consists of a magnetogram that contains the real field configuration and newly emerging magnetic features at the observational time, and a part of synoptic charts around the time of interest. Recently we improve the synoptic frame by removing the effect of differential rotation existing in the part of synoptic charts around the specific time. In this work, we will present the results of the time-dependent three-dimensional MHD simulation using this improved synoptic frame of photospheric magnetic field. The MHD simulation code we have developed is based on the TVD-MUSCL strategy, and the projected normal characteristic method is used to deal with the sub-Alfvenic boundary at 1 R_s to obtain the trans-alfvenic nonlinear-MHD solution of the solar wind and corona. The calculated solar coronal quantities are compared with the observations, in terms of the magnetic field topology, such as the shape of the coronal hole.
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005