Microinstabilities and models of the solar wind

Details Microinstabilities and models of the solar wind Microinstabilities and models of the solar wind

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981soph...74..179r&link_type=abstract

(ESA and European Physical Society, ESLAB Symposium on Physics of Solar Variations, 14th, Scheveningen, Netherlands, Sept. 16-19

Physics

1

Collisionless Plasmas, Magnetohydrodynamic Stability, Solar Wind, Two Fluid Models, Heat Flux, Solar Corona, Solar Protons, Stellar Models

Scientific paper

The collision-dominated two-fluid plasma models of the solar wind are shown to become collisionless and subject to microinstabilities at a few solar radii. Assuming that once the plasma is unstable it stays close to marginal stability models of the solar wind are constructed including waves and proton heating. The resulting models have higher velocities and proton temperatures than the collision dominated two fluid models.

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