Understanding Jupiter's Interior

TL;DR

This paper reviews how models of Jupiter's interior are constructed, integrating observational data, experimental results, and simulations to understand its layered structure, composition, and evolution, especially in light of recent Juno mission data.

Contribution

It provides a comprehensive overview of current interior models of Jupiter, highlighting recent advances and the potential of new data from the Juno spacecraft to refine these models.

Findings

Discussion of three-layer interior models with a core and hydrogen-helium layers

Comparison of equations of state with shock wave experiments

Potential insights from Juno's gravitational measurements

Abstract

This article provides an overview of how models of giant planet interiors are constructed. We review measurements from past space missions that provide constraints for the interior structure of Jupiter. We discuss typical three-layer interior models that consist of a dense central core and an inner metallic and an outer molecular hydrogen-helium layer. These models rely heavily on experiments, analytical theory, and first-principle computer simulations of hydrogen and helium to understand their behavior up to the extreme pressures ~10 Mbar and temperatures ~10,000 K. We review the various equations of state used in Jupiter models and compare them with shock wave experiments. We discuss the possibility of helium rain, core erosion and double diffusive convection may have important consequences for the structure and evolution of giant planets. In July 2016 the Juno spacecraft entered orbit around Jupiter, promising high-precision measurements of the gravitational field that will allow us to test our understanding of gas giant interiors better than ever before.