Second viscosity of the gas in the outer solar envelope

Details Second viscosity of the gas in the outer solar envelope Second viscosity of the gas in the outer solar envelope

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...348..328c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 348, Jan. 1, 1990, p. 328-332.

Astronomy and Astrophysics

Astrophysics

3

Gas Viscosity, Photosphere, Recombination Reactions, Solar Corona, Stellar Envelopes, Atomic Energy Levels, Chromosphere, Convection, Magnetohydrodynamics, Optical Thickness

Scientific paper

The theory of second viscosity is applied to the gas in the outer solar envelope. It is assumed that this viscosity arises because of the finite relaxation time characterizing the exchange of translational energy of electrons and the internal, binding energy of the electrons in hydrogen atoms. Radiative and three-body recombinations with electrons, and charge exchange with H(-) are assumed to be the dominant processes determining the relaxation times. The second viscosity so calculated is seven orders of magnitude larger than the ordinary viscosity in the upper photosphere (log Pg = 3.2). Some 2000 km below this level, it is still nearly 2 orders of magnitude larger, according to current estimates.

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