Energy input into the solar wind

Details Energy input into the solar wind Energy input into the solar wind

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985esasp.235...11m&link_type=abstract

In ESA Future Missions in Solar, Heliospheric and Space Plasma Physics p 11-21 (SEE N86-27330 18-12)

Physics

Plasma Physics

2

Particle Flux Density, Solar Corona, Solar Magnetic Field, Solar Wind, Transport Theory, Coulomb Collisions, Damping, Interplanetary Medium, Magnetohydrodynamic Waves, Plasma Heating, Thermal Energy, Wave Interaction

Scientific paper

The energy input into the solar wind is discussed in terms of observation and fluid theory. Solar wind microphysics and transport are reviewed. In situ observations beyond 0.3 AU and the consequent constraints on solar wind expansion and energetics are treated. Energy and mass flux obtained by indirect means and remote optical sensing of the corona are considered. The need to revise the classical Coulomb collision model of transport is emphasized. Slow and fast mode wave damping, and nonlinear processes leading to damping of Alfven waves, used to explain ion heating in the corona and solar wind, are assessed.

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