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Equation of State of Stellar Plasmas

Published online by Cambridge University Press:  12 April 2016

Forrest J. Rogers
Forrest J. Rogers*
Affiliation:
Lawrence Livermore National Laboratory, Livermore, CA 94550

Abstract

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The equation of state (EOS) of astrophysical plasmas is, for a wide range of stars, nearly ideal; with only small non-ideal Coulomb corrections. Calculating the EOS of an ionizing plasma from a ground state ion, ideal gas model is easy, whereas, fundamental methods to include the small Coulomb corrections are difficult. Attempts to include excited bound states are also complicated by plasma screening and microfield phenomena that weaken and broaden these states. Nevertheless, the high quality of current observational data, particularly seismic, dictates that the best possible models should be used. The present article discusses these issues and describes how they are resolved by fundamental many-body quantum statistical methods. Particular emphasis is placed on the activity expansion method that is the basis of the OPAL opacity code. Some comparisons with standard methods are given.

Type
Reviews
Information
International Astronomical Union Colloquium , Volume 147: The Equation of State in Astrophysics , 1994 , pp. 16 - 42
Copyright
Copyright © Cambridge University Press 1994

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