Convective Energy Transport in Stellar Atmospheres. III: Multi-Stream Atmospheres

Details Convective Energy Transport in Stellar Atmospheres. III: Multi-Stream Atmospheres Convective Energy Transport in Stellar Atmospheres. III: Multi-Stream Atmospheres

Oct 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970ap%26ss...9...80u&link_type=abstract

Astrophysics and Space Science, Volume 9, Issue 1, pp.80-96

Astronomy and Astrophysics

Astrophysics

15

Scientific paper

We discuss a theoretical method of computing the temperature structure of hot and cool streams in convective stellar atmospheres. The method is based on the model that the streams are due to organized cells whose diameters are greater than the thickness of the photosphere. The excess thermal energy of matter rising from the deeper layers, where the entropy is higher than in the photosphere, is converted to radiation in a steady front. This model, applied to the solar case, exhibits a peak-to-peak contrast of 30 40% between granules and lanes. This contrast agrees with the Stratoscope data reduced by Namba and Diemel (1969). As a necessary part of the theory, we obtain an expression for the perturbation in radiative heat exchange which may be used in a medium with a strongly preferred direction such as a stellar atmosphere.

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