Solar wind models with Alfven waves

Details Solar wind models with Alfven waves Solar wind models with Alfven waves

Dec 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...226..632j&link_type=abstract

Astrophysical Journal, Part 1, vol. 226, Dec. 1, 1978, p. 632-649.

Astronomy and Astrophysics

Astrophysics

36

Magnetohydrodynamic Waves, Solar Wind, Stellar Models, Heat Flux, Plasma Heating, Solar Protons, Wave Propagation

Scientific paper

Solutions to the one-fluid solar-wind equations that include pressure and heating due to outwardly propagating Alfven waves are presented. The solutions are given for two forms of the heat flux: the classical Spitzer (1962) formula and a 'collisional' heat flux. Both high-speed and low-speed solar-wind streams are considered. A comparison of solutions with and without waves shows that the solutions without waves cannot come close to reproducing observations of total mass and energy flux at 1 AU, while those with waves are capable of bringing nearly all flow variables into reasonable agreement with the observations. The required wave flux is found to be about 100,000 erg/sq cm per sec for the high-speed streams and an order of magnitude less for the low-speed streams. It is concluded that the pressure and heating due to outwardly propagating Alfven waves are important elements of solar-wind dynamics that cannot be neglected and that wave heating is especially important for the protons in high-speed streams.

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