JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2)

By N. Nettelmann, Andreas Becker, B. Holst, Ronald Redmer. 2011

152 citations recorded by the source corpus.

The amount and distribution of heavy elements in Jupiter gives indications on the process of its formation and evolution. Core mass and metallicity predictions, however, depend on the equations of state (EOSs) used and on model assumptions. We present an improved ab initio hydrogen EOS, H-REOS.2, and compute the internal structure and thermal evolution of Jupiter within the standard three-layer approach. The advance over our previous Jupiter models with H-REOS.1 by Nettelmann et al. is that the new models are also consistent with the observed ≳ 2 times solar heavy element abundances in Jupiter's atmosphere. Such models have a rock core mass Mc = 0–8 M⊕, total mass of heavy elements MZ = 28–32 M⊕, a deep internal layer boundary at ⩾4 Mbar, and a cooling time of 4.4–5.0 Gyr when assuming homogeneous evolution. We also calculate two-layer models in the manner of Militzer et al. and find a comparable large core of 16–21 M⊕, out of which ∼11 M⊕ is helium, but a significantly higher envelope metallicity of 4.5 times solar. According to our preferred three-layer models, neither the characteristic frequency (ν0 ∼ 156 μHz) nor the normalized moment of inertia (λ ∼0.276) is sensitive to the core mass but accurate measurements could well help to rule out some classes of models.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/6523dbf93b93400f6832003a7e844723e2fc6dd2

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Molecular Biology

Citations in the corpus

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, methodology): “These data led to interior models of Jupiter published in Nettelmann et al. (2008) and Nettelmann et al. (2012).”
New Models of Jupiter in the Context of Juno and Galileo (2019, background): “, Rosenblum et al. (2011)).”
Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core (2017, background): “…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 al., 2016], but interior model predictions are still sensitive to the…”
New indication for a dichotomy in the interior structure of Uranus and Neptune from the application of modified shape and rotation data (2012, methodology): “Under the assumption of adiabatic, homogeneous cooling, Saturn’s theoretical cooling time is systematically too short by 2-2.5 Gyrs (Guillot et al., 1995; Fortney and Hubbard, 2003), while Jupiter’s is often found to be a little too long (Saumon et al., 1992; Guillot et al., 1995; Fortney et al., 20”
AB INITIO SIMULATIONS FOR MATERIAL PROPERTIES ALONG THE JUPITER ADIABAT (2012, methodology): “The Vienna Ab initio Simulation Package (VASP; Kresse & Hafner 1993, 1994; Kresse & Furthmüller 1996) was used to calculate the EOS of hydrogen (Nettelmann et al. 2012).”