Study of Jupiter’s interior: Comparison of 2, 3, 4, 5, and 6 layer models

Militzer, Burkhard; Hubbard, William B.

doi:10.1016/j.icarus.2024.115955

Cited by 5 publications

(2 citation statements)

References 66 publications

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“…Whatever the generalization beyond the standard stellar evolution paradigms that we have followed to craft APPLE, the result would unlikely after ∼4.56 billion yr land on a suite of current J i values that could compete with the precision of the measured Juno values. We note that even the static models that have been employed to reproduce the Juno J i values (e.g., Wahl et al 2017 andHubbard 2024) have a range of inferred potential compositional and thermal profiles. Moreover, the thermal profiles are very poorly constrained in those inversions and the results are not one-to-one.…”

Section: Structure and Evolution Equationsmentioning

confidence: 99%

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APPLE: An Evolution Code for Modeling Giant Planets

Sur,

Su,

Tejada Arevalo

et al. 2024

ApJ

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We introduce APPLE, a novel planetary evolution code designed specifically for the study of giant exoplanet and Jovian planet evolution in the era of Galileo, Juno, and Cassini. With APPLE, state-of-the-art equations of state for hydrogen, helium, ice, and rock are integrated with advanced features to treat ice/rock cores and metals in the gaseous envelope; models for helium rain and hydrogen/helium immiscibility; detailed atmosphere boundary tables that also provide self-consistent albedos and spectra; and options to address envelope metal gradients and stably stratified regions. Our hope is that these purpose-built features of APPLE will help catalyze the development of the next generation of giant exoplanet and Jovian planet evolutionary models.

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Section: Structure and Evolution Equationsmentioning

confidence: 99%

“…, Mankovich & Fortney (2020),Militzer & Hubbard (2024), andMankovich & Fuller (2021) then used this EOS to infer the structure and composition of Jupiter and Saturn at the present age. Nevertheless, this EOS was computed for only one helium mass fraction (Y = 0.245) and requires extensions to accommodate other helium mass fractions.…”

mentioning

confidence: 99%

APPLE: An Evolution Code for Modeling Giant Planets

Sur,

Su,

Tejada Arevalo

et al. 2024

ApJ

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Ensemble Monte Carlo calculations with five novel moves

Militzer

2025

Computer Physics Communications

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Vapor equilibrium models of accreting rocky planets demonstrate direct core growth by pebble accretion

Steinmeyer,

Johansen

2024

A&A

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The gaseous envelope of an accreting rocky planet becomes hot enough to sublimate silicates and other refractory minerals. For this work, we studied the effect of the resulting envelope enrichment with a heavy vapor species on the composition and temperature of the envelope. For simplification, we used the gas-phase molecule SiO to represent the sublimation of silicate material. We solved the equilibrium structure equations in 1D for planets in the mass range of $0.1$ to $3\ The convective stability criterion was extended to take the stabilizing effect of the condensation of SiO clouds into account. We assumed that the envelope is both in hydrostatic equilibrium and in vapor equilibrium with the underlying magma ocean. This means that pebbles do not undergo sublimation in the envelope and therefore survive until they plunge into the magma ocean. We find that the emergence of an inner radiative region, where SiO condensation suppresses convection, increases the pressure and temperature in the inner envelope compared to pure H2 He envelopes once $ For $ the temperature and pressure close to the surface reach the supercritical point of SiO. The amount of SiO stored in the envelope is lower than the total planet mass for low mass planets. However, for $ all accreted pebble material must contribute to maintain the vapor equilibrium in the envelope. Therefore, the non-vapor mass of the planet ceases to increase beyond this threshold. Overall, our vapor equilibrium model of the planetary envelope allows for direct core growth by pebble accretion up to much higher masses than previously thought.

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Study of Jupiter’s interior: Comparison of 2, 3, 4, 5, and 6 layer models

Cited by 5 publications

References 66 publications

APPLE: An Evolution Code for Modeling Giant Planets

APPLE: An Evolution Code for Modeling Giant Planets

Ensemble Monte Carlo calculations with five novel moves

Vapor equilibrium models of accreting rocky planets demonstrate direct core growth by pebble accretion

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