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Stellar Atmosphere Modeling

  • Loïc Chevallier

Abstract

In this note, the formalism used to compute a simple stellar atmosphere model is described. The definition of a stellar atmosphere is strongly connected with the radiation field crossing the boundary layers of a star: the atmosphere is composed of those layers where photons interact with matter for the last time before leaving the star. The goal of a model is to calculate the radiation field at all frequencies, depths and directions consistent with the properties of matter (temperature, number densities, pressure, etc.) at all depths.

Keywords

Radiation Field Electron Number Density Radiative Transfer Equation Stellar Atmosphere Statistical Equilibrium Equation 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. 1.
    B. Rutily, Multiple scattering theory and integral equations, this volume, 211–232.Google Scholar

Copyright information

© Springer Science+Business Media New York 2004

Authors and Affiliations

  • Loïc Chevallier

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