A tilted-dipole MHD model of the solar corona and solar wind

Details A tilted-dipole MHD model of the solar corona and solar wind A tilted-dipole MHD model of the solar corona and solar wind

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0504u&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0504

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2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2169 Sources Of The Solar Wind, 7536 Solar Activity Cycle (2162)

Scientific paper

We simulate the heliospheric structure during solar activity minimum as determined by boundary conditions at the coronal base and compare output from the model with Ulysses observations during its first fast latitude transition in 1994-1995. The polytropic MHD equations are solved for a steady coronal outflow and include Alfvén wave momentum and energy addition in the WKB approximation. A solution for the outflow in a tilted dipole magnetic field in the inner computational region (1-20 R&sun; ) is combined with a three-dimensional solution in the outer region which extends to 10 AU. The dipole orientation is chosen to match the one inferred from observations during the Ulysses observations. The bimodality of solar wind with a rapid change in flow parameters with latitude and the observed extension of the slower wind belt are reproduced fairly well.

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