Equations of state for solar and stellar modeling
Abstract
Helioseismology has become the most successful diagnosis of the equation of state for the plasma of stellar interiors. Although in the solar interior the plasma is only weakly coupled and weakly degenerate, the great observational accuracy of the helioseismological observations puts nevertheless strong constraints on the nonideal part of the equation of state. For solar and stellar modeling, a high-quality equation of state is crucial. But the inverse is also true: the astrophysical data put constraints on the physical formalisms, making the Sun and the stars novel laboratories for plasma physics.
- Publication:
-
Equation-of-State and Phase-Transition in Models of Ordinary Astrophysical Matter
- Pub Date:
- October 2004
- DOI:
- 10.1063/1.1828391
- Bibcode:
- 2004AIPC..731....3D
- Keywords:
-
- 95.30.Tg;
- 95.30.Qd;
- 96.60.Ly;
- 97.10.Sj;
- Thermodynamic processes conduction convection equations of state;
- Magnetohydrodynamics and plasmas;
- Helioseismology pulsations and shock waves;
- Pulsations oscillations and stellar seismology