Planets in turbulent Disks

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Show simple item record Kley, Wilhelm Stoll, Moritz H.R. Picogna, Giovanni 2018-08-22T14:07:35Z 2018-08-22T14:07:35Z 2018-08-14
dc.identifier.other 510366511
dc.identifier.uri de_DE
dc.description.abstract Planets form in protoplanetary accretion disks around young protostars. These disks are driven by internal turbulence and the gas flow is in general not laminar but has stochastic components. For weakly ionized disks the turbulence can be generated purely hydrodynamically through the vertical shear instability (VSI). Planets, that are forming in such turbulent disks, experience random components in the torques acting on them, that will modify their migration behaviour. In this contribution we present results of our study of the impact that a turbulent disk has on an embedded planet. For that purpose we performed three-dimensional hydrodynamical simulations of a locally isothermal disk with embedded planets of various masses. For the lower mass planets (5 and 10 M ) we find that the inward migration rate can be faster than in the laminar case, while for the more massive planets (30 and 100 M ) the results agree well with the laminar results. en
dc.language.iso en de_DE
dc.publisher Universität Tübingen de_DE
dc.publisher Universität Tübingen de_DE
dc.rights ubt-podok de_DE
dc.rights.uri de_DE
dc.rights.uri en
dc.subject.classification Hochleistungsrechnen de_DE
dc.subject.ddc 000 de_DE
dc.subject.ddc 004 de_DE
dc.title Planets in turbulent Disks en
dc.type ConferencePaper de_DE
utue.publikation.fachbereich Zentrum für Datenverarbeitung de_DE
utue.publikation.fakultaet 7 Mathematisch-Naturwissenschaftliche Fakultät de_DE


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