Microphysics: Equation of State

Details Microphysics: Equation of State Microphysics: Equation of State

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998ssrv...85...49d&link_type=abstract

Space Science Reviews, v. 85, Issue 1/2, p. 49-60 (1998).

Mathematics

Logic

6

Helioseismology, Equation Of State, Helium Abundance, Excited States

Scientific paper

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.

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