Mathematics
Scientific paper
Jun 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.confr..66o&link_type=abstract
Oslo Univ., International Solar Wind 8 Conference, p. 66
Mathematics
Solar Wind, Energy Budgets, Conductive Heat Transfer, Conservation Equations, Distribution Functions, Boltzmann Transport Equation, Heat Flux, Kinetic Energy, Plasma Density, Plasma-Particle Interactions, Momentum, Energy Transfer, Mass Transfer, Mathematical Models
Scientific paper
Heat conduction from the corona is important in the solar wind energy budget. Until now all hydrodynamic solar wind models have been using the collisionally dominated gas approximation for the heat conductive flux. Observations of the solar wind show particle distribution functions which deviate significantly from a Maxwellian, and it is clear that the solar wind plasma is far from collisionally dominated. We have developed a numerical model for the solar wind which solves the full equation for the heat conductive flux together with the conservation equations for mass, momentum, and energy. The equations are obtained by taking moments of the Boltzmann equation, using an 8-moment approximation for the distribution function. For low-density solar winds the 8-moment approximation models give results which differ significantly from the results obtained in models assuming the gas to be collisionally dominated. The two models give more or less the same results in high density solar winds.
Leer Egil
Lyngdal Olsen Espen
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