Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-32075
Boley, A C (2009). The two modes of gas giant planet formation. Astrophysical Journal Letters, 695(1):L53-L57.
I argue for two modes of gas giant planet formation and discuss the conditions under which each mode operates. Gas giant planets at disk radii r>100 AU are likely to form in situ by disk instability, while core accretion plus gas capture remains the dominant formation mechanism for r < 100 AU. During the mass accretion phase, mass loading can push disks toward fragmentation conditions at large r. Massive, extended disks can fragment into clumps of a few to tens of Jupiter masses. This is confirmed by radiation hydrodynamics simulations. The two modes of gas giant formation should lead to a bimodal distribution of gas giant semimajor axes. Because core accretion is expected to be less efficient in low-metallicity systems, the ratio of gas giants at large r to planets at small r should increase with decreasing metallicity.
|Item Type:||Journal Article, refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute of Theoretical Physics|
|Deposited On:||25 Feb 2010 17:32|
|Last Modified:||28 Nov 2013 00:29|
|Publisher:||Institute of Physics Publishing|
|Citations:||Web of Science®. Times Cited: 105|
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