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.
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References
B. Rutily, Multiple scattering theory and integral equations, this volume, 211–232.
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© 2004 Springer Science+Business Media New York
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Chevallier, L. (2004). Stellar Atmosphere Modeling. In: Constanda, C., Largillier, A., Ahues, M. (eds) Integral Methods in Science and Engineering. Birkhäuser, Boston, MA. https://doi.org/10.1007/978-0-8176-8184-5_7
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DOI: https://doi.org/10.1007/978-0-8176-8184-5_7
Publisher Name: Birkhäuser, Boston, MA
Print ISBN: 978-1-4612-6479-8
Online ISBN: 978-0-8176-8184-5
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