Equation of State for the Internal Structure of Solar-Type Stars
Abstract
The physical basis for thermodynamical modeling of plasma under the conditions typical of moderate-mass stars is considered. We apply the method of thermodynamic potentials to introduce chemical and physical plasma models that represent basic, modern descriptions of a nondegenerate, weakly nonideal plasma. Ionization of an ideal multicomponent plasma at low temperatures is used as a basic approximation for the solar convection zone and in the corresponding chemical picture. The effects of Coulomb free-free and bound-free electron interactions are classified according to their appearance in the solar interior. Modeling internal stellar structure requires a formalism with nonideal ionization at high densities (frequently called pressure ionization). Perspectives for describing such ionization are considered in the framework of several models.
- Publication:
-
Astronomy Reports
- Pub Date:
- August 2003
- DOI:
- 10.1134/1.1601637
- Bibcode:
- 2003ARep...47..685B