Study of Jupiter's Interior: Comparison of 2, 3, 4, 5, and 6 Layer Models

Abstract

With the goal of matching spacecraft measurements from Juno and Galileo missions, we construct ensembles of 2, 3, 4, 5, and 6 layer models for Jupiter's interior. All except our two layer models can match the planet's gravity field as measured by the Juno spacecraft. We find, however, that some model types are more plausible than others. In the best three layer models, for example, the transition from molecular to metallic hydrogen needs to be at ~500 GPa while theory and experiments place this transition at ~100 GPa. Four layer models with a single sharp boundary between core and mantle would be short-lived due to rapid convective core erosion. For this reason, we favor our five layer models that include a dilute core surrounded by a stably stratified core transition layer. Six layer models with a small compact core are also possible but with an upper limit of 3 Earth masses for such a compact core. All models assume a 1 bar temperature of 166.1 K, employ physical equations of state, and are constructed with the nonperturbative Concentric Maclaurin Spheroid (CMS) method. We analyze the convergence of this method and describe technical steps that are needed to make this technique so efficient that ensembles of models can be generated.

11 figures, 1 table, one numerical method to find roots of N dimensional problems

References in corpus (20)

• Mass-Radius Relationships for Solid Exoplanets
• Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core
• A Massive Core in Jupiter Predicted From First-Principles Simulations
• Hydrogen-Helium Mixtures in the Interiors of Giant Planets
• New models of Jupiter in the context of Juno and Galileo
• Nuclear Quantum Effects and Nonlocal Exchange-Correlation Functionals Applied to Liquid Hydrogen at High Pressure
• First-Principles Equation of State Database for Warm Dense Matter Computation
• First Principles Calculations of Shock Compressed Fluid Helium
• The Formation of Jupiter's Diluted Core by a Giant Impact
• Jupiter's inhomogeneous envelope
• The Challenge of Forming a Fuzzy Core in Jupiter
• Revelations on Jupiter's Formation, Evolution and Interior: Challenges from Juno Results
• Understanding Jupiter's Interior
• Models of Saturn's Interior Constructed with Accelerated Concentric Maclaurin Spheroid Method
• Jupiter's interior from Juno: Equation-of-state uncertainties and dilute core extent
• Double-diffusive erosion of the core of Jupiter
• Combined magnetic and gravity measurements probe the deep zonal flows of the gas giants
• Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
• Tidal Response and Shape of Hot Jupiters
• Study of Jupiter's Interior with Quadratic Monte Carlo Simulations

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