Physics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42b0524h&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH42B-0524
Physics
2100 Interplanetary Physics, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind
Scientific paper
We will present the results of the experimental time-dependent MHD simulation of the solar corona, with various boundary treatments based on the concept of characteristics projection method. This method allows us to make the choices of the boundary treatment rather arbitrarily, and it is possible that the results may depend on them. We examined this point using TVD-MUSCL MHD code and found that, among the choice we made, a two-stage boundary treatment, where (i) the plasma density and temperature are fixed if 0 <= Vr <= Vc and (ii) the radial flow speed is reset to be Vc and instead the temperature is changeable if Vr >= Vc, with the criteria flow speed Vc = 5.0 km/s, provides the steady solar wind best matching the reality, for example, the uniform plasma and magnetic field at the high heliographic latitude regions. This study is a part of our effort to construct the three-dimensional MHD simulation model of solar corona using SOHO/MDI data.
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