The heating of the solar wind by Alfvenic fluctuations

Details The heating of the solar wind by Alfvenic fluctuations The heating of the solar wind by Alfvenic fluctuations

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984chjss...4..277t&link_type=abstract

Chinese Journal of Space Science, vol. 4, Oct. 1984, p. 277-284. In Chinese, with abstract in English.

Astronomy and Astrophysics

Astronomy

1

Magnetohydrodynamic Turbulence, Magnetohydrodynamic Waves, Plasma Heating, Plasma Temperature, Solar Protons, Solar Wind, Astronomical Models, Energy Dissipation, Gyrofrequency, Helios 1, Helios 2

Scientific paper

The theory of heating of solar wind by Alfvenic fluctuation and a viscous model and wave energy cascading model for the attenuation of that fluctuation have been tested against observational data from Helios 1 and 2. The calculated radial variation of the temperature of the solar wind protons is found to agree with observational results, while the rate of energy dissipation of the fluctuations predicted by the viscous model differs from observational results by about eight orders of magnitude. The rate of energy dissipation predicted by the wave energy cascading model agrees with observational results. Thus, a possible mechanism of the heating of solar wind protons is the dissipation of the energy cascading to the frequency range of the proton gyrofrequency.

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