Abstract
Although the plasma of envelopes of normal stars is only weakly non-ideal, the inadequacy of simple equations of state has been clearly demonstrated by helioseismology. Solar and stellar applications put high demands on the precision and consistency of the realization of any physical formalism. The three principal non-ideal effects are due to internal partition functions of bound systems, to pressure ionization, and to collective interactions of the charged particles. Comparisons between different formalisms help to find the astrophysical observables that can discriminate between equations of state that are based on different treatments of non-ideal effects. A first set of astrophysical observables is provided by helioseismology, which is becoming sufficiently accurate to put constraints on the equation of state.
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© 1992 B. G. Teubner Verlagsgesellschaft, Leipzig
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Däppen, W. (1992). The Equation of State for Stellar Envelopes. In: Ebeling, W., Förste, A., Radtke, R. (eds) Physics of Nonideal Plasmas. TEUBNER-TEXTE zur Physik, vol 26. Vieweg+Teubner Verlag, Wiesbaden. https://doi.org/10.1007/978-3-322-99736-4_36
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DOI: https://doi.org/10.1007/978-3-322-99736-4_36
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