Effects of CO molecules on the outer solar atmosphere - Dynamical models with opacity distribution functions

Details Effects of CO molecules on the outer solar atmosphere - Dynamical models with opacity distribution functions Effects of CO molecules on the outer solar atmosphere - Dynamical models with opacity distribution functions

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...201..138m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 201, no. 1, July 1988, p. 138-142.

Astronomy and Astrophysics

Astrophysics

14

Carbon Monoxide, Late Stars, Opacity, Radiation Transport, Solar Atmosphere, Stellar Models, Distribution Functions, Infrared Spectra, Spectral Bands, Temperature Gradients

Scientific paper

Carbon monoxide can be an important cooling agent in late-type stars. This paper expands previous theoretical work by extending the frequency set used in the radiation calculations, employing opacity distribution functions for the infrared bands of CO and 19 frequency points for the H(-) continuum. It is found that the net cooling rate due to CO decreases by a factor of about 3 due to the large optical depths in the line cores. The influence of the 2.2-micron CO band is small compared to the effect of the 4.6-micron band. An atmospheric structure with a sharp drop of the temperature in the outer photosphere, where CO cooling sets in, was found again. This temperature drop occurs higher in the atmosphere and is less steep than in the simpler models but is nevertheless steep enough to be convectively unstable. When CO cooling sets in, surface temperatures drop to very low values (T less than 3000 K) for radiative equilibrium models, even without including the effects of other molecules.

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