The acceleration of the solar wind

Details The acceleration of the solar wind The acceleration of the solar wind

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382...72a&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 72-

Physics

2

Particle Emission, Solar Wind, Electric And Magnetic Fields, Solar Magnetism, Magnetohydrodynamic Waves

Scientific paper

We review the observed properties of the solar wind with the aim of finding a simple and straightforward understanding of its origin and acceleration. A theory is developed for the high speed solar wind based on a simple dissipation length assumption for hydromagnetic wave heating of the coronal plasma close to the Sun. Solutions with the correct particle and energy fluxes and with a realistic magnetic field, match the requirements on the density at the base of the corona provided the dissipation length is relatively small (~0.25-0.5 solar radii). The significant features are that the acceleration is rapid, with the sonic point within ~2 solar radii, and the proton temperatures are high, namely 8-10×106 K. Such efficient dissipation requires any Alfven waves responsible to have frequencies in the range 0.01 Hz-10 kHz. This has implications for the nature of the plasma and energy source in the supergranular network.

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