On the energetics of the solar supergranulation

Details On the energetics of the solar supergranulation On the energetics of the solar supergranulation

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...288..795g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 288, Jan. 15, 1985, p. 795-800.

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11

Energy Dissipation, Solar Granulation, Convection, Kinetic Energy, Photosphere, Scale Height, Thermodynamic Properties

Scientific paper

Thermodynamic arguments demonstrate that kinetic energy dissipation must occur in the convection zone. The dissipation rate depends on the temperature gradient, which is at a minimum in the hydrogen ionization zone. As a result, the kinetic energy dissipation rate per density scale height shows a maximum just below the photosphere and another maximum beneath the ionization zone. It is proposed that intensified convection at these two levels is the explanation for the two distinct phenomena of granulation and supergranulation. The values of the scale heights at these maxima are consistent with the length scales of the granulation and the supergranulation. A moderate amount of a radial diffusion of kinetic energy does not alter this result.

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