HR: 1340h
AN: SH13A-1156    [Abstracts]
TI: Time-dependent Three-dimensional MHD Simulation of Solar Corona and Solar Wind at Solar Minimum Activity Phase
AU: * Hayashi, K
EM: keiji@quake.stanford.edu
AF: Stanford University, W.W.Hansen Experimental Physics Laboratory 455 Via Palou, Stanford, CA 94305 United States
AU: Liu, Y
AF: Stanford University, W.W.Hansen Experimental Physics Laboratory 455 Via Palou, Stanford, CA 94305 United States
AU: Zhao, X
AF: Stanford University, W.W.Hansen Experimental Physics Laboratory 455 Via Palou, Stanford, CA 94305 United States
AB: We will present results of time-dependent three-dimensional MHD simulation of solar corona and solar wind at the solar minimum activity phase using the boundary treatment that can limit mass flux flowing outward through the subsonic/Alfvenic solar surface. The aim of limiting mass flux is for obtaining simulated solar wind well matching Ulysses data and good contrast of density near the sun. The MHD simulation code we have developed is based on the concept of TVD-MUSCL method and the treatments of boundary at 1 $R_s$ is based on the normal projected characteristic method. To specify the solar surface boundary magnetic field, the potential field model and the synoptic map format data of WSO and MDI solar photospheric magnetic field data are used.
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
DE: 2134 Interplanetary magnetic fields
DE: 2164 Solar wind plasma
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting