Microphysics: Equation of State

To Veronika and her Hometown
  • Werner Däppen
Conference paper
Part of the Space Sciences Series of ISSI book series (SSSI, volume 5)

Abstract

The equation of state is one of the three fundamental ingredients used to construct stellar models. The plasma of the interiors of stars such as the Sun is only slightly non-ideal. However, the extraordinary accuracy of the helioseismological data requires refined equations of state. It turned out to be necessary to include a Coulomb correction, commonly evaluated in the Debye-Hückel approximation. Higher-order non-ideal effects have implications as well, both for plasma physics and for solar physics. As a typical example, the recently studied thermodynamic consequence of excited states in compound particles is discussed. This effect is of considerable relevance in the helioseismic determination of the helium abundance in the solar convection zone.

Key words

helioseismology equation of state helium abundance excited states 
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Copyright information

© Springer Science+Business Media Dordrecht 1998

Authors and Affiliations

  • Werner Däppen
    • 1
  1. 1.Department of Physics and AstronomyUniversity of Southern CaliforniaLos AngelesUSA

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