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Formation of Giant Planets
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Giant planets dominate the mass of many planetary systems, including the Solar System, and represent the best-characterized class of extrasolar planets. Understanding the formation of giant planets bridges the high mass end of the planet formation process and the low mass end of processes that produce stellar and brown dwarf companions. This review examines the latest evidence supporting the formation of Solar System giant planets and most extrasolar giant planets by core accretion. Key elements of this theory and recent advances are discussed, along with the role of gravitational fragmentation of gas disks -- a mechanism more likely to produce brown dwarfs and/or similarly massive binary companions.
Forward citations
Cited by 3 Pith papers
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Atmospheric Signatures of Common Envelope Evolution in White Dwarf Planets
During common-envelope evolution, engulfed giant planets can accrete enough stellar material to measurably brighten their thermal emission, offering a new atmospheric diagnostic of their dynamical history.
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The Longest-period Young Transiting Exoplanets. A Duo of Puffy Giants inside a Debris Disk
HD 114082 hosts two puffy, moderate-to-low-mass giants on nearly circular, coplanar, near-resonant orbits of 225.55 and ~314 days, the longest-period young transiting exoplanets known.
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Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
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