AB INITIO SIMULATIONS FOR MATERIAL PROPERTIES ALONG THE JUPITER ADIABAT
By M. French, Andreas Becker, W. Lorenzen, N. Nettelmann, Mandy Bethkenhagen, Johannes Wicht, Ronald Redmer. Astrophysical Journal Supplement Series, 2012
221 citations recorded by the source corpus.
We determine basic thermodynamic and transport properties of hydrogen–helium–water mixtures for the extreme conditions along Jupiter's adiabat via ab initio simulations, which are compiled in an accurate and consistent data set. In particular, we calculate the electrical and thermal conductivity, the shear and longitudinal viscosity, and diffusion coefficients of the nuclei. We present results for associated quantities like the magnetic and thermal diffusivity and the kinematic shear viscosity along an adiabat that is taken from a state-of-the-art interior structure model. Furthermore, the heat capacities, the thermal expansion coefficient, the isothermal compressibility, the Grüneisen parameter, and the speed of sound are calculated. We find that the onset of dissociation and ionization of hydrogen at about 0.9 Jupiter radii marks a region where the material properties change drastically. In the deep interior, where the electrons are degenerate, many of the material properties remain relatively constant. Our ab initio data will serve as a robust foundation for applications that require accurate knowledge of the material properties in Jupiter's interior, e.g., models for the dynamo generation.
Subfields: Astronomy and Astrophysics, Molecular Biology
View Paper: https://www.semanticscholar.org/paper/4b23d511d54b491dd287ad5a1eb953fc5cc3ea58
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Citations in the corpus
- Tidal Dissipation in Stars and Giant Planets (2014, background): “Ogilvie & Lin (2007) applied a similar idea to the host stars of hot Jupiters, where the stellar rotation is slow compared to the orbit, and the eccentricity is negligible; they found that, for a model based on the present Sun, a companion of more than about 3 Jupiter masses would generate waves tha”
- AB INITIO EQUATIONS OF STATE FOR HYDROGEN (H-REOS.3) AND HELIUM (He-REOS.3) AND THEIR IMPLICATIONS FOR THE INTERIOR OF BROWN DWARFS (2014, unknown): “…least the entropy, within the H-REOS.3 and He-REOS.3, to construct a reasonable EOS covering a similar density-temperature range that represents heavier elements, e.g., by water, and to provide material properties along the adiabats of GPs and BDs as it was done by French et al. (2012) for Jupiter.”