Hydrogen-Helium Mixtures in the Interiors of Giant Planets

By J. Vorberger, I. Tamblyn, B. Militzer, S. Laboratory, Carnegie Institution of Washington, Usa, D. Physics, Atmospheric Science, D. University, Canada.. 2006

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Equilibrium properties of hydrogen-helium mixtures under conditions similar to the interior of giant gas planets are studied by means of first principle density functional molecular dynamics simulations. We investigate the molecular and atomic fluid phase of hydrogen with and without the presence of helium for densities between ρ = 0.19 gcm 3 and ρ = 0.66 gcm 3 and temperatures from T = 500K to T = 8000 K. Helium has a crucial influence on the ionic and electronic structure of the liquid. Hydrogen molecule bonds are shortened as well as strengthened which leads to more stable hydrogen molecules compared to pure hydrogen for the same thermodynamic conditions. The ab initio treatment of the mixture enables us to investigate the validity of the widely used linear mixing approximation. We find deviations of up to 8% in energy and volume from linear mixing at constant pressure in the region of molecular dissociation.

Subfields: Atomic and Molecular Physics, and Optics, Geophysics

View Paper: https://www.semanticscholar.org/paper/f4020056babaaf1eb085840f487427da2fc7c60e

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Citations in the corpus

The Interior Structure, Composition, and Evolution of Giant Planets (2009, methodology): “The He EOS He-SCVH is described in Saumon et al. (1995), He-Sesame-K04 in Kerley (2004a), He-REOS in Nettelmann et al. (2008a), and DFTMD in Vorberger et al. (2007), respectively.”
AB INITIO SIMULATIONS FOR MATERIAL PROPERTIES ALONG THE JUPITER ADIABAT (2012, methodology): “…of hydrogen and helium under extreme conditions has been investigated using ab initio simulations (see, e.g., Desjarlais 2003; Militzer 2006, 2009; Vorberger et al. 2007; Kietzmann et al. 2007; Holst et al. 2008, 2011; Stixrude & Jeanloz 2008; Lorenzen et al. 2009, 2010, 2011; Morales et al.…”
Ab initio simulation of warm dense matter (2019, background): “[8–13] and the outer crust of neutron stars [14, 15].”
JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2) (2011, methodology): “This is surprising as non-linear H-He mixing effects, which have been shown to decrease the density of the mixed phase (Vorberger et al. 2007) compared to the linear mixture that we apply, are already included in the H-He EOS of the M08 Jupiter models.”
The Properties of Hydrogen and Helium Under Extreme Conditions (2011, methodology): “These system sizes are comparable to the one used in (Scandolo, 2003) and (Bonev et al., 2004a) with CPMD, and considerably larger than the one used in (Vorberger et al., 2007b) and (Holst et al., 2008) with BOMD.”
Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core (2017, background): “Significant progress has been made in understanding hydrogen-helium mixtures at planetary conditions [Saumon et al., 1995; Saumon and Guillot, 2004; Vorberger et al., 2007; Militzer et al., 2008; Fortney and Nettelmann, 2010; Nettelmann et al., 2012; Militzer, 2013; Becker et al., 2013; Militzer et…”