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The numerous complexities underlying large tables of thermodynamic quantities act as a deterrent to a careful evaluation of their reliability. As a consequence, equations of state are often used as black boxes. To clarify this situation, some of the more critical issues of equation of state physics are discussed from the point of view of the user. They are illustrated by a comparison of four equations of state for hydrogen. The flaws and disagreements thus brought into light are explained and evaluated with simple physical arguments.
Les tables d'équations d'état utilisées en astrophysique découlent de modèles d'une complexité telle qu'il est souvent difficile d'en évaluer la fiabilité. Il en résulte une situation où les équations d'état sont souvent utilisées sans une analyse critique de leur contenu physique ni de leur précision. Dans le but de remédier à cette situation, une discussion des principaux éléments physiques des équations d'état est présentée dans l'optique de l'utilisateur. Quatre équations d'état de l'hydrogène développées pour être appliquées à des problèmes d'astrophysique stellaire sont comparées de façon critique. Cette comparaison illustre l'importance de certains éléments clés des équations d'état et la nature des problèmes qui subsistent. Les déefauts et les différences observés entre ces quatre équations d'état sont élucidés en termes de physique de base.
Introduction
The richness of stellar phenomena exposed by modern observational techniques calls for a quantitative understanding of more subtle, “second order” effects in stellar structure.
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