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Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-34396

Boley, A C; Hayfield, T; Mayer, L; Durisen, R H (2010). Clumps in the outer disk by disk instability: Why they are initially gas giants and the legacy of disruption. Icarus, 207(2):509-516.

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We explore the initial conditions for fragments in the extended regions (r≳50AU) of gravitationally unstable disks. We combine analytic estimates for the fragmentation of spiral arms with 3D SPH simulations to show that initial fragment masses are in the gas giant regime. These initial fragments will have substantial angular momentum, and should form disks with radii of a few AU. We show that clumps will survive for multiple orbits before they undergo a second, rapid collapse due to H2 dissociation and that it is possible to destroy bound clumps by transporting them into the inner disk. The consequences of disrupted clumps for planet formation, dust processing, and disk evolution are discussed. We argue that it is possible to produce Earth-mass cores in the outer disk during the earliest phases of disk evolution


92 citations in Web of Science®
93 citations in Scopus®
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Additional indexing

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Date:June 2010
Deposited On:03 Mar 2011 15:06
Last Modified:16 Jun 2014 14:00
Publisher DOI:10.1016/j.icarus.2010.01.015
Related URLs:http://arxiv.org/abs/0909.4543

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