Equation of state and opacity.
Abstract
The three most important physical ingredients of stellar models are the nuclear-energy generation rates, the equation of state and the opacity. The authors begin this chapter with a discussion of the equation of state, not only because the equation of state plays an important role in stellar structure, but also because it is by itself a fundamental part of any opacity calculation. Furthermore, the computation of the equation of state is the simpler problem. There are two reasons for this. First, already at lower densities, where atoms exist (i.e. where many-body effects can be neglected), it suffices for the equation of state to know the energy levels of atoms (and their occupation). Second, at higher densities, where many-body effects become important (and where one cannot speak of atoms), there are at least roads to a correct treatment of the equation of state (the authors will show some of them in this chapter). Extending these techniques to opacity calculations faces the difficulty that again more detailed information about the quantum-mechanical many-body states is required.
- Publication:
-
Solar Interior and Atmosphere
- Pub Date:
- 1991
- Bibcode:
- 1991sia..book..112D
- Keywords:
-
- Equations Of State;
- Opacity;
- Stellar Models;
- Stellar Physics;
- Stellar Interiors;
- Stellar Structure;
- Astrophysics