Physics
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh13a1156h&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH13A-1156
Physics
7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma
Scientific paper
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 Rs 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.
Hayashi Kumiko
Liu Ya-Ying
Zhao Xiaopeng
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