A new equation of state for dense hydrogen-helium mixtures II: taking into account hydrogen-helium interactions

Abstract

In a recent paper (Chabrier et al. 2019), we have derived a new equation of state (EOS) for dense hydrogen/helium mixtures which covers the temperature-density domain from solar-type stars to brown dwarfs and gaseous planets. This EOS is based on the so-called additive volume law and thus does not take into account the interactions between the hydrogen and helium species. In the present paper, we go beyond these calculations by taking into account H/He interactions, derived from quantum molecular dynamics simulations. These interactions, which eventually lead to H/He phase separation, become important at low temperature and high density, in the domain of brown dwarfs and giant planets. The tables of this new EOS are made publicly available.

To be published in The Astrophysical Journal

References in corpus (5)

• New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit
• Hydrogen-Helium Mixtures in the Interiors of Giant Planets
• New models of Jupiter in the context of Juno and Galileo
• A new equation of state for dense hydrogen-helium mixtures
• Jupiter internal structure: the effect of different equations of state

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