Ab Initio Equation of State Data for Hydrogen, Helium, and Water and the Internal Structure of Jupiter

By N. Nettelmann, B. Holst, A. Kietzmann, M. French, Ronald Redmer, David B. Blaschke. 2007

206 citations recorded by the source corpus.

The equation of state of hydrogen, helium, and water affects interior structure models of giant planets significantly. We present a new equation of state data table, LM-REOS, generated by large-scale quantum molecular dynamics simulations for hydrogen, helium, and water in the warm dense matter regime, i.e., for megabar pressures and temperatures of several thousand kelvins, and by advanced chemical methods in the complementary regions. The influence of LM-REOS on the structure of Jupiter is investigated and compared with state-of-the-art results within a standard three-layer model consistent with astrophysical observations of Jupiter. Our new Jupiter models predict an important impact of mixing effects of helium in hydrogen with respect to an altered compressibility and immiscibility.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/512b535e56c12dcce48afb78a2a3bb018c7d6cfb

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In Astronomy and Astrophysics

1. Jon Fortney
2. C. Mordasini
3. E. Lopez
4. Sara Seager
5. G. Marcy
6. Leslie A. Rogers
7. D. Charbonneau
8. J. Owen

In Geophysics

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

Citations in the corpus

• New indication for a dichotomy in the interior structure of Uranus and Neptune from the application of modified shape and rotation data (2012, methodology): “Podolak et al. (1995) apply physical equations of state of hydrogen, helium, the ices H2O, H2S, CH4, and NH3, and rocks, assuming sharp transitions between a gaseous outer envelope, an inner icy envelope, and a rock core.”
• 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).”
• The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “aptures a massive atmosphere of H and He from the protoplanetary disk. The mass of all giant planet cores but Jupiter is around 10 Earth masses (M ) (Guillot, 2005). Jupiter might have no core today (Nettelmann et al., 2008). However, there are several tens of Earth masses of \metals" (molecule”
• SUPER-EARTH ATMOSPHERES: SELF-CONSISTENT GAS ACCRETION AND RETENTION (2015, methodology): “…− 1 ] , (38) since Gyr old atmospheres are close to the maximum gas density (see Section 3.2.1), which we evaluate using the equation of state of Nettelmann et al. (2008) as ρmax ≈ 0.5 g cm−3 ( P Mbar )0.4 , (39) with the typical atmosphere pressure given by P = Matmg 4πR2 ≈ Mbar ( M M⊕ )2(…”
• UNDERSTANDING THE MASS–RADIUS RELATION FOR SUB-NEPTUNES: RADIUS AS A PROXY FOR COMPOSITION (2013, methodology): “In addition we consider the possibility of waterworlds and three component models using the H2O-REOS for water (Nettelmann et al. 2008).”
• The Interior Structure, Composition, and Evolution of Giant Planets (2009, methodology): “In Jupiter-size and Saturn-size planets, hydrogen, maybe helium too –depending on the EOS, metallizes giving rise to a strong magnetic field; in Neptune-size planets, water prefers (depending on the entropy) the ionically conducting superionic phase or the plasma phase (Nettelmann et al. 2008b).”
• 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).”
• 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).”
• FORMATION AND STRUCTURE OF LOW-DENSITY EXO-NEPTUNES (2011, background): “The effect of uncertainties in the H/He EOS (see e.g., Militzer et al. 2008; Nettelmann et al. 2008) will be small compared to the effect of uncertainties in the heavy element composition and distribution, for the low-mass planets we are considering.”
• 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 FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY TRANSITING PLANETS (2013, methodology): “We can use the methods of Nettelmann et al. (2008, 2013) to suggest possible interior structures.”
• The Properties of Hydrogen and Helium Under Extreme Conditions (2011, methodology): “Most current models of Jupiter and Saturn are based on the SCVH equations of state (Guillot, 1999; Guillot et al., 1994a,b, 1997), although recently, models for Jupiter have used equations of state derived from first-principles simulations (Militzer et al., 2008; Nettelmann et al., 2008).”
• JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2) (2011, methodology): “The corresponding Jupiter models were consistent with the available observational constraints (Nettelmann et al. 2008, hereafter N08).”
• ALL SIX PLANETS KNOWN TO ORBIT KEPLER-11 HAVE LOW DENSITIES (2013, background): “Most of the H2O would be in the vapor and molecular fluid phases, with the ionic fluid and plasma phases occurring at high pressures deep within these planets (Nettelmann et al. 2008, 2011).”