On the viscous attenuation of Alfvenic fluctuations in the solar wind

Details On the viscous attenuation of Alfvenic fluctuations in the solar wind On the viscous attenuation of Alfvenic fluctuations in the solar wind

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984chjss...4r...1t&link_type=abstract

Chinese Journal of Space Science, vol. 4, Jan. 1984, p. 1-10. In Chinese, with abstract in English.

Computer Science

Magnetohydrodynamic Waves, Solar Wind, Wave Attenuation, Wentzel-Kramer-Brillouin Method, Magnetic Fields, Viscosity

Scientific paper

The possibility of viscous attenuation of the Alfvenic fluctuation in the solar wind is discussed in terms of a viscous WKB solution of incompressible Alfven waves, the wavelengths of which are larger than the mean free path. Because the proton gyrofrequency is much larger than the collision frequency in the solar wind, viscous attenuation should be proportional to the component of the fluctuation parallel to the average magnetic field vector. If the ratio between the amplitudes of the parallel component and the perpendicular component is a constant with respect to the heliocentric distance, no viscous attenuation occurs for r between 0.3 AU and 1.0 AU, whereas for r less than 20 earth radii, the Alfvenic fluctuation will suffer some viscous attenuation that may accelerate the solar wind.

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