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The Structure of a Stationary Atmosphere with a Heat Source or Sink

Published online by Cambridge University Press:  12 April 2016

Kyoji Nariai
Kyoji Nariai*
Affiliation:
Tokyo Astronomical Observatory, The University of Tokyo, Mitaka, Tokyo 181, Japan

Extract

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There are several methods for solving a structure of a stellar atmosphere in radiative equilibrium. Among them, the matrix method (Nariai and Shigeyama 1984, Nariai and Ito 1985) uses only the energy equation at the nodes; therefore, it is easy to extend this method to an atmosphere that is not in radiative equilibrium. The matrix method gives direct solutions for the cases of a gray model or a picket–fence model, and it is so effective that the calculation converges in 3 or 4 iterations in the case of a non-gray atmosphere with scattering even if the starting model is isothermal. In order to simplify the problem, in this paper, however, we will limit ourselves to the case of a gray atmosphere with pure absorption.

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 197 - 198
Copyright
Copyright © Springer-Verlag 1988

References

Nariai, K. and Shigeyama, T. 1984, Publ.Astron.Soc.Japan, 36, 593.Google Scholar
Nariai, K. and Ito, M. 1985, Publ.Astron.Soc.Japan, 37, 553.Google Scholar
Nariai, K. and Murata, Y. 1987, Publ.Astron.Soc.Japan, 39, 163.Google Scholar