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Equation of state of stellar plasmas [electronic resource].

Published
Washington, D.C. : United States. Dept. of Energy, 1993.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy.
Physical Description
29 pages : digital, PDF file
Additional Creators
Lawrence Livermore National Laboratory, United States. Department of Energy, and United States. Department of Energy. Office of Scientific and Technical Information
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Summary
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.
Report Numbers
E 1.99:ucrl-jc--115702
E 1.99: conf-9306287--1
conf-9306287--1
ucrl-jc--115702
Subject(s)
Other Subject(s)
Note
Published through SciTech Connect.
06/01/1993.
"ucrl-jc--115702"
" conf-9306287--1"
"DE94004186"
Equation of state in astrophysics workshop,Saint-Malo (France),14-18 Jun 1993.
Rogers, F.J.
Funding Information
W-7405-ENG-48
View MARC record | catkey: 13825790