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Abstract: We discuss the interior structure and composition of giant planets, and howthis structure changes as these planets cool and contract over time. Here wedefine giant planets as those that have an observable hydrogen-helium envelope,which includes Jupiter-like planets, which are predominantly H-He gas, andNeptune-like planets which are predominantly composed of elements heavier thanH-He. We describe the equations of state of planetary materials and theconstruction of static structural models and thermal evolution models. We applythese models to transiting planets close to their parent stars, as well asdirectly imaged planets far from their parent stars. Mechanisms that have beenpostulated to inflate the radii of close-in transiting planets are discussed.We also review knowledge gained from the study of the solar system-s giantplanets. The frontiers of giant planet physics are discussed with an eyetowards future planetary discoveries.



Author: Jonathan J. Fortney, Isabelle Baraffe, Burkhard Militzer

Source: https://arxiv.org/







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