Jupiter's formation and its primordial internal structure

Abstract

The composition of Jupiter and the primordial distribution of the heavy elements are determined by its formation history. As a result, in order to constrain the primordial internal structure of Jupiter the growth of the core and the deposition and settling of accreted planetesimals must be followed in detail. In this paper we determine the distribution of the heavy elements in proto-Jupiter and determine the mass and composition of the core. We find that while the outer envelope of proto-Jupiter is typically convective and has an homogeneous composition, the innermost regions have compositional gradients. In addition, the existence of heavy elements in the envelope leads to much higher internal temperatures (several times 10${}^4$ K) than in the case of a hydrogen-helium envelope. The derived core mass depends on the actual definition of the core: if the core is defined as the region in which the heavy-element mass fraction is above some limit (say 0.5), then it can be much more massive ($\sim$ 15 M${}_{\oplus }$) and more extended (10\% of the planet's radius) than in the case where the core is just the region with 100\% heavy elements. In the former case Jupiter's core also consists of hydrogen and helium. Our results should be taken into account when constructing internal structure models of Jupiter and when interpreting the upcoming data from the {\it Juno} (NASA) mission.

32 pages, 12 figures

References in corpus (22)

• Solar Models with Helium and Heavy Element Diffusion
• Models of Giant Planet formation with migration and disc evolution
• The Interiors of Giant Planets: Models and Outstanding Questions
• The Interior Structure, Composition, and Evolution of Giant Planets
• Shock Compression of Deuterium and the Interiors of Jupiter and Saturn
• A Comparison of the Interiors of Jupiter and Saturn
• Models of Jupiter's Growth Incorporating Thermal and Hydrodynamic Constraints
• A new vision on giant planet interiors: the impact of double diffusive convection
• Ab initio Equation of State data for hydrogen, helium, and water and the internal structure of Jupiter
• A Massive Core in Jupiter Predicted From First-Principles Simulations
• Formation of Jupiter using opacities based on detailed grain physics
• Jupiter models with improved ab initio hydrogen EOS (H-REOS.2)
• Planet formation with envelope enrichment: new insights on planetary diversity
• Rocky core solubility in Jupiter and giant exoplanets
• Gas Giant Formation with Small Cores Triggered by Envelope Pollution by Icy Planetesimals
• The Effect of Composition on the Evolution of Giant and Intermediate-Mass Planets
• A Preliminary Jupiter Model
• The Evolution and Internal Structure of Jupiter and Saturn with Compositional Gradients
• Convection and Mixing in Giant Planet Evolution
• Measuring Jupiter's water abundance by Juno: the link between interior and formation models
• Dynamical Constraints on the Core Mass of Hot Jupiter HAT-P-13b
• Constraining the interior of extrasolar giant planets with the tidal Love number k_2 using the example of HAT-P-13b

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• Internal Structure of Giant and Icy Planets: Importance of Heavy Elements and Mixing
• Effects of Planetesimal Accretion on the Thermal and Structural Evolution of Sub-Neptunes
• Tidal dissipation in stratified and semi-convective regions of giant planets
• Further constraints on Jupiter's primordial structure
• Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-Accretion Model -II: The effect of Saturn
• No dilute core produced in simulations of giant impacts on to Jupiter
• The Effect of Accretion Rate and Composition on the Structure of Ice-rich Super-Earths
• Evidence of a gap in the envelope mass fraction of sub-Saturns
• On the Ordering of Exoplanet Systems
• Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-Accretion Model -III: The Contribution of Planetesimals Beyond Saturn
• Possible in situ formation of Uranus and Neptune via Pebble Accretion