Microphysics: Equation of State |
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Authors: | Werner Däppen |
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Institution: | (1) Department of Physics and Astronomy, University of Southern California, USA |
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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.
This revised version was published online in June 2006 with corrections to the Cover Date. |
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Keywords: | helioseismology equation of state helium abundance excited states |
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