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Title:
The Interior Structure, Composition, and Evolution of Giant Planets
Authors:
Fortney, Jonathan J.; Nettelmann, Nadine
Affiliation:
AA(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA), AB(Institut fur Physik, Universitat Rostock, Rostock, Germany)
Publication:
Space Science Reviews, Volume 152, Issue 1-4, pp. 423-447 (SSRv Homepage)
Publication Date:
05/2010
Origin:
SPRINGER
Keywords:
Giant planet interiors, Exoplanets
Abstract Copyright:
(c) 2010: Springer Science+Business Media B.V.
DOI:
10.1007/s11214-009-9582-x
Bibliographic Code:
2010SSRv..152..423F

Abstract

We discuss our current understanding of the interior structure and thermal evolution of giant planets. This includes the gas giants, such as Jupiter and Saturn, that are primarily composed of hydrogen and helium, as well as the ``ice giants,'' such as Uranus and Neptune, which are primarily composed of elements heavier than H/He. The effect of different hydrogen equations of state (including new first-principles computations) on Jupiter's core mass and heavy element distribution is detailed. This variety of the hydrogen equations of state translate into an uncertainty in Jupiter's core mass of 18 M ⊕ . For Uranus and Neptune we find deep envelope metallicities up to 0.95, perhaps indicating the existence of an eroded core, as also supported by their low luminosity. We discuss the results of simple cooling models of our solar system's planets, and show that more complex thermal evolution models may be necessary to understand their cooling history. We review how measurements of the masses and radii of the nearly 50 transiting extrasolar giant planets are changing our understanding of giant planets. In particular a fraction of these planets appear to be larger than can be accommodated by standard models of planetary contraction. We review the proposed explanations for the radii of these planets. We also discuss very young giant planets, which are being directly imaged with ground- and space-based telescopes.
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