The Interior Structure, Composition, and Evolution of Giant Planets - Astrophysics > Earth and Planetary AstrophysicsReportar como inadecuado




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Abstract: We discuss our current understanding of the interior structure and thermalevolution of giant planets. This includes the gas giants, such as Jupiter andSaturn, that are primarily composed of hydrogen and helium, as well as the -icegiants,- such as Uranus and Neptune, which are primarily composed of elementsheavier than H-He. The effect of different hydrogen equations of stateincluding new first-principles computations on Jupiter-s core mass and heavyelement distribution is detailed. This variety of the hydrogen equations ofstate translate into an uncertainty in Jupiter-s core mass of 18 M Earth. ForUranus and Neptune we find deep envelope metallicities up to 0.95, perhapsindicating the existence of an eroded core, as also supported by their lowluminosity. We discuss the results of simple cooling models of our solarsystem-s planets, and show that more complex thermal evolution models may benecessary to understand their cooling history. We review how measurements ofthe masses and radii of the ~50 transiting extrasolar giant planets arechanging our understanding of giant planets. In particular a fraction of theseplanets appear to be larger than can be accommodated by standard models ofplanetary contraction. We review the proposed explanations for the radii ofthese planets. We also discuss very young giant planets, which are beingdirectly imaged with ground- and space-based telescopes.



Autor: Jonathan J. Fortney, Nadine Nettelmann

Fuente: https://arxiv.org/







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