Equation of state and phase diagram of water at ultrahigh pressures as in planetary interiors

By M. French, T. Mattsson, N. Nettelmann, Ronald Redmer. 2009

172 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/352529303c0ca7117d4e6cfe878116881c507499

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

1. Jon Fortney
2. E. Lopez
3. N. Nettelmann
4. C. Mordasini
5. Ronald Redmer
6. K. Zahnle
7. D. Sasselov
8. Andreas Becker

In Geophysics

1. N. Nettelmann
2. Jon Fortney
3. Ronald Redmer
4. Andreas Becker
5. M. French
6. E. Lopez
7. D. Sasselov
8. L. Zeng

Citations in the corpus

• HOW THERMAL EVOLUTION AND MASS-LOSS SCULPT POPULATIONS OF SUPER-EARTHS AND SUB-NEPTUNES: APPLICATION TO THE KEPLER-11 SYSTEM AND BEYOND (2012, methodology): “Meanwhile for water we use the ab initio H2O-REOS EOS developed by Nettelmann et al. (2008) and French et al. (2009), which was recently confirmed up to 7 Mbar in laboratory experiments (Knudson et al. 2012).”
• The phase diagram of water and the magnetic fields of Uranus and Neptune (2011, methodology): “Up to 512 electrons can routinely be considered in the cubic simulation box with periodic boundary conditions; we have used up to 54 molecules for the calculation of the water EOS (Nettelmann et al., 2008; French et al., 2009).”
• A Detailed Model Grid for Solid Planets from 0.1 through 100 Earth Masses (2013, methodology): “Theoretically, the EOS could be calculated by Quantum-Mechanical Molecular Dynamics Ab Initio Simulation such as the VASP (Vienna Ab initio Simulation Package) (Kresse & Hafner 1993, 1994; Kresse & Furthmüller 1996; French et al. 2009).”
• JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2) (2011, methodology): “Heavy elements in the envelopes are represented by the water equation of state H2O-REOS (French et al. 2009; N08), for helium we use He-REOS (Kietzmann et al. 2007; N08), and for rocks the formula given in Hubbard & Marley (1989).”
• Composition and fate of short-period super-Earths: The case of CoRoT-7b (2009, unknown): “The EOS used for water vapor is obtained from a combination of data obtained from a finite temperature molecular dynamics (FT-DFT-MD) simulation by French et al. (2009) and of the Sesame 7150 EOS (see Kerley 1972).”
• AB INITIO SIMULATIONS FOR MATERIAL PROPERTIES ALONG THE JUPITER ADIABAT (2012, methodology): “Note that ab initio EOS data cover the pressure region above ∼0.08 Mbar for H, ∼0.1 Mbar for He, (Kietzmann et al. 2007), and ∼0.1 Mbar for H2O (French et al. 2009); see also Figures 1–3 in Nettelmann et al. (2008).”
• The Interior Structure, Composition, and Evolution of Giant Planets (2009, methodology): “FVT+ combines fluid variational theory, a minimization method for the free energy of neutral hydrogen, with Pade formulas for fully ionized hydrogen taking into account ionization equilibrium.”
• A FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY TRANSITING PLANETS (2013, methodology): “The core mass fraction Mc is varied from 0.9 to 0.7, while the Zenv is varied from 0.5 to 0.8, using a water EOS (French et al. 2009).”