The Equation of State for Stellar Envelopes: Comparison of Theoretical Results

Details The Equation of State for Stellar Envelopes: Comparison of Theoretical Results The Equation of State for Stellar Envelopes: Comparison of Theoretical Results

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992rmxaa..23..141d&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 23, 141

Astronomy and Astrophysics

Astronomy

12

Scientific paper

RESUMEN. Una comparaci6n anterior de los parametros termodinamicos calculados respectivamente en los cuadros qufmico y fisico result6 en un renombrado acuerdo en las zonas de ionizaci6n del H y del He en el Sol, a pesar del tratamiento radicalmente diferente de los estados ligados en los dos formalismos. Este acuerdo se debi6 a un dominio inesperado del termino (dasico de la presi6n de Coulomb. En comparaciones recientes, a temperaturas y densi ades ma's altas y para una mezcla solar representativa (H, He y 0), se han encontrado grandes diferencias en las fracciones de ionizaci6n del 0. Los parametros termodina',micos tambien refiejan estas diferencias, a tal grado de estar al alcance de la heliosismologfa. ABSTRACT. A previous comparison of thermodynamical quantities, computed in the chemical and physical pictures, revealed a remarkable agreement in the H and He ionization zones of the Sun, despite the radically different treatment of bound states in the two formalisms. This agreement was due to an unexpectedly dominating (classical) Coulomb pressure term. New comparisons, for higher temperatures and densities, and for a representative solar mixture (H, He and 0), have demonstrated substantial differences in the 0-ionization fractions. Also, the thermodynamic quantities reflect these differences to a degree that is within reach of helioseismology. Key words: EQUATION OF STATE - STARS: INTERIOR

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