Comparing Jupiter interior structure models to <i>Juno</i> gravity measurements and the role of a dilute core

Wahl, S. M.; Hubbard, W. B.; Militzer, Burkhard; Guillot, T.; Miguel, Yamila; Movshovitz, N.; Kaspi, Yohai; Helled, Ravit; Reese, D. R.; Galanti, Eli; Levin, S. M.; Connerney, J. E. P.; Bolton, S. J.

doi:10.1002/2017gl073160

Cited by 360 publications

(419 citation statements)

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“…Some previously published interior models, characterized by different temperature, composition, and core mass and size, are close to agreement with the estimated zonal harmonics J 4 and J 6 within uncertainties [e.g., Nettelmann et al , ; Miguel et al , ] while others are not [e.g., Hubbard and Militzer , ]. While Jupiter interior models can be adjusted to fit the Juno estimates [e.g., Wahl et al , ], it is possible that differential rotation can produce a change to J 4 and J 6 expected for a uniformly rotating Jupiter that can affect their interpretation [e.g., Hubbard , ]. Differential rotation might also lead to small nonzero values of the odd zonal harmonics [ Kaspi , ].…”

Section: Discussionmentioning

confidence: 99%

Jupiter gravity field estimated from the first two Juno orbits

Folkner

Iess

Anderson

et al. 2017

Geophysical Research Letters

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The combination of the Doppler data from the first two Juno science orbits provides an improved estimate of the gravity field of Jupiter, crucial for interior modeling of giant planets. The low‐degree spherical harmonic coefficients, especially J4 and J6, are determined with accuracies better than previously published by a factor of 5 or more. In addition, the independent estimates of the Jovian gravity field, obtained by the orbits separately, agree within uncertainties, pointing to a good stability of the solution. The degree 2 sectoral and tesseral coefficients, C2,1, S2,1, C2,2, and S2,2, were determined to be statistically zero as expected for a fluid planet in equilibrium.

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Section: Discussionmentioning

confidence: 99%

Jupiter gravity field estimated from the first two Juno orbits

Folkner

Iess

Anderson

et al. 2017

Geophysical Research Letters

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“…The results of Vazan et al (2016) indicate that no full mixing occurs if the initial compositional gradient is strong enough. If the heavy element mass fraction as a function of enclosed mass Z(M) in a planet today (see the Juno spacecraft data, Wahl et al 2017) therefore reflects at least partially the structure during build-up, this would open an interesting avenue to constrain the ratio of the solid accretion to the gas accretion rate as a function of planet mass,Ṁ Z /Ṁ XY (M). This would obviously be of high interest in the context of the core-mass effect.…”

Section: Uncertainties Related To the Core-mass Effectmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

116

142

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Context. This paper continues a series in which we predict the main observable characteristics of exoplanets based on their formation. In Paper I we described our global planet formation and evolution model that is based on the core accretion paradigm. In Paper II we studied the planetary mass-radius relationship with population syntheses. Aims. In this paper we present an extensive study of the statistics of planetary luminosities during both formation and evolution. Our results can be compared with individual directly imaged extrasolar (proto)planets and with statistical results from surveys. Methods. We calculated three populations of synthetic planets assuming different efficiencies of the accretional heating by gas and planetesimals during formation. We describe the temporal evolution of the planetary mass-luminosity relation. We investigate the relative importance of the shock and internal luminosity during formation, and predict a statistical version of the post-formation mass vs. entropy "tuning fork" diagram. Because the calculations now include deuterium burning we also update the planetary mass-radius relationship in time.Results. We find significant overlap between the high post-formation luminosities of planets forming with hot and cold gas accretion because of the core-mass effect. Variations in the individual formation histories of planets can still lead to a factor 5 to 20 spread in the post-formation luminosity at a given mass. However, if the gas accretional heating and planetesimal accretion rate during the runaway phase is unknown, the post-formation luminosity may exhibit a spread of as much as 2-3 orders of magnitude at a fixed mass. As a key result we predict a flat log-luminosity distribution for giant planets, and a steep increase towards lower luminosities due to the higher occurrence rate of low-mass (M 10-40 M ⊕ ) planets. Future surveys may detect this upturn. Conclusions. Our results indicate that during formation an estimation of the planetary mass may be possible for cold gas accretion if the planetary gas accretion rate can be estimated. If it is unknown whether the planet still accretes gas, the spread in total luminosity (internal+accretional) at a given mass may be as large as two orders of magnitude, therefore inhibiting the mass estimation. Due to the core-mass effect even planets which underwent cold accretion can have large post-formation entropies and luminosities, such that alternative formation scenarios such as gravitational instabilities do not need to be invoked. Once the number of self-luminous exoplanets with known ages and luminosities increases, the resulting luminosity distributions may be compared with our predictions.

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“…Either way, it is clear that QMC implies a denser EOS for H at Jupiter's conditions, which translates to an envelope that is poor in heavy elements. If this is indeed the case, it introduces new challenges in understanding Jupiter's current structure and origin 4,6,36 .…”

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Phase Diagram of Hydrogen and a Hydrogen-Helium Mixture at Planetary Conditions by Quantum Monte Carlo Simulations

2018

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Understanding planetary interiors is directly linked to our ability of simulating exotic quantum mechanical systems such as hydrogen (H) and hydrogen-helium (H-He) mixtures at high pressures and temperatures 1 . Equations of State (EOSs) tables based on Density Functional Theory (DFT), are commonly used by planetary scientists, although this method allows only for a qualitative description of the phase diagram 2 , due to an incomplete treatment of electronic interactions 3 . Here we report Quantum Monte Carlo (QMC) molecular dynamics simulations of pure H and H-He mixture. We calculate the first QMC EOS at 6000 K for an H-He mixture of a proto-solar composition, and show the crucial influence of He on the H metallization pressure. Our results can be used to calibrate other EOS calculations and are very timely given the accurate determination of Jupiter's gravitational field from the NASA Juno mission and the effort to determine its structure 4 .Since a few decades the link between the uncertainty of the H EOS and the internal structure of Jupiter (and other gaseous planets) has been investigated and many efforts to model Jupiter's interior have been carried 1,5-7 . The computation of an EOS from first principles requires to solve a many-body quantum mechanical problem, a task which is beyond the currently available theoretical and computational capabilities. In practice, we must resort to several approximations. The first is to decouple the ionic and electronic problems and consider the ions as classical or quantum particles, determining their motion by following the Born-Oppenheimer potential energy surface. The second approximation concerns the description of the electronic interaction and the exchange one, due to the Pauli exclusion principle.The standard approach to EOS calculations relies on Density Functional Theory (DFT), which targets the tridimensional electronic density rather than the (N e electrons) many-body wave-function. Its success and simplicity have lead to a widespread application in materials science and to the development of several software packages which allow fast and reproducible calculations 8 . Although DFT is formally exact, the explicit functional form to describe the exchange and correlation (XC) effects between electrons remains approximated 3 . Indeed, a systematic and efficient route to improve XC functional is still lacking. Therefore, in practical solid state calculations, benchmarks against experimental data, are often required to validate the XC functional used to describe the system in a satisfactory manner.Dense hydrogen systems, both in the low temperature solid and in the liquid phase remain a challenge to DFT simulations due to the interplay of strong correlation and non-covalent interactions between the atoms. DFT calculations with different functionals produce different results with the expected metallization pressure varying over a range of 100-200 GPa (Fig. 1) 12,13 . Since experimental data are limited, it is not possible to identify a posteriori the best functional...

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Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core

Cited by 360 publications

References 61 publications

Jupiter gravity field estimated from the first two Juno orbits

Jupiter gravity field estimated from the first two Juno orbits

Characterization of exoplanets from their formation

Phase Diagram of Hydrogen and a Hydrogen-Helium Mixture at Planetary Conditions by Quantum Monte Carlo Simulations

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