Clumps in the outer disk by disk instability: Why they are initially gas giants and the legacy of disruption |
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Authors: | Aaron C Boley Tristen Hayfield Richard H Durisen |
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Institution: | a Institute for Theoretical Physics, University of Zurich, Winterthurerstrasse 190, Zurich CH-8057, Switzerland b Astronomy Department, University of Florida, 211 Bryant Space Science Center, P.O. Box 112055, USA c Physics Department, ETH Zürich, CH-8093 Zürich, Switzerland d Department of Astronomy, Indiana University, 727 East 3rd Street, Bloomington, IN 47405, USA |
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Abstract: | We explore the initial conditions for fragments in the extended regions 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. |
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Keywords: | Disks Planetary formation Planets Migration Planetesimals |
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