A dynamic model of the three-fluid solar wind: Equilibrium structures and fluxes

Details A dynamic model of the three-fluid solar wind: Equilibrium structures and fluxes A dynamic model of the three-fluid solar wind: Equilibrium structures and fluxes

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...64r&link_type=abstract

California Univ., International Solar Wind 8 Conference, p. 64

Statistics

Computation

Dynamic Models, Solar Wind, Mass Transfer, Energy Transfer, Alpha Particles, Electron Energy, Steady State, Electric Fields, Momentum, Equilibrium Equations, Plasma Equilibrium, Transport Properties, Solar Wind Velocity, Coulomb Collisions, Solar Flux

Scientific paper

We report results from a dynamic approach to equilibrium for a three fluid solar-wind model in spherical 1D. We advance the mass, momentum and energy transport equations for protons, alpha particles and electrons, with full interspecies coulomb coupling and the simplifications recommended by Burgi (1992). They include no ion heat conduction and an ambipolar electric field in place of the negligible electron momentum coupling. At the inner boundary (the solar surface) we specify the inflow velocity, mass flux, and temperature for each species, and at the outer boundary at large radius we allow the fluids to flow freely from the computational domain. Starting from an initial wind model (e.g.. single fluid) we evolve to a three-fluid steady state. We will describe comparisons with Burgi's static equilibrium results. and examine the stability of the discontinuities which appear in his derived parameter variations.

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