Equations of state for solar and stellar modeling

Details Equations of state for solar and stellar modeling Equations of state for solar and stellar modeling

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..731....3d&link_type=abstract

EQUATION-OF-STATE AND PHASE-TRANSITION ISSUES IN MODELS OF ORDINARY ASTROPHYSICAL MATTER. AIP Conference Proceedings, Volume 73

Mathematics

Logic

Thermodynamic Processes, Conduction, Convection, Equations Of State, Magnetohydrodynamics And Plasmas, Helioseismology, Pulsations, And Shock Waves, Pulsations, Oscillations, And Stellar Seismology

Scientific paper

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.

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