Giant Planet Interior Structure and Thermal Evolution

Abstract

We discuss the interior structure and composition of giant planets, and how this structure changes as these planets cool and contract over time. Here we define giant planets as those that have an observable hydrogen-helium envelope, which includes Jupiter-like planets, which are predominantly H/He gas, and Neptune-like planets which are predominantly composed of elements heavier than H/He. We describe the equations of state of planetary materials and the construction of static structural models and thermal evolution models. We apply these models to transiting planets close to their parent stars, as well as directly imaged planets far from their parent stars. Mechanisms that have been postulated to inflate the radii of close-in transiting planets are discussed. We also review knowledge gained from the study of the solar system's giant planets. The frontiers of giant planet physics are discussed with an eye towards future planetary discoveries.

Invited chapter, in press for the Arizona Space Science Series book "Exoplanets," edited by S. Seager

References in corpus (2)

• HAT-P-13b,c: a transiting hot Jupiter with a massive outer companion on an eccentric orbit
• Inflating and Deflating Hot Jupiters: Coupled Tidal and Thermal Evolution of Known Transiting Planets

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• Implications of the interstellar object 1I/'Oumuamua for planetary dynamics and planetesimal formation
• Investigating hot-Jupiter inflated radii with hierarchical Bayesian modelling
• WASP-31b: a low-density planet transiting a metal-poor, late-F-type dwarf star
• Non-radial Oscillations in Rotating Giant Planets with Solid Cores: Application to Saturn and its Rings
• Finding the Needles in the Haystacks: High-Fidelity Models of the Modern and Archean Solar System for Simulating Exoplanet Observations
• The K2-ESPRINT Project IV: A Hot Jupiter in a Prograde Orbit with a Possible Stellar Companion
• Atmospheric characterization of cold exoplanets using a 1.5-m coronagraphic space telescope
• Inflation of Migrated Hot Jupiters