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Gravitational instability and the formation of giant planets by core accretion

Published online by Cambridge University Press:  02 May 2006

K. Kornet
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: kornet@mpia-hd.mpg.de, swolf@mpia-hd.mpg.de
S. Wolf
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: kornet@mpia-hd.mpg.de, swolf@mpia-hd.mpg.de
M. Różyczka
Affiliation:
Nicolaus Copernicus Astronomical Center, Bartycka 18, Warsaw, 00-716, Poland email: mnr@camk.edu.pl
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Abstract

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We investigate the problem of giant planet formation around stars with various masses based on the core accretion/gas capture model. At first, we follow the evolution of gas and solids from the moment when all solids are in the form of small grains to the stage when most of them have reached planetesimal size. We show that the surface density of a planetesimal swarm tends to be higher around less massive stars. Subsequently, we derive the minimum surface density of the planetesimal swarm required for the formation of giant planets, both in a numerical and in an approximate analytical approach. We combine these results by calculating a set of representative disk models, characterized by different masses, sizes, and metallicities. This allows us to quantify the probability of each individual disk model to form giant planets. Furthermore, we take the fact into account, that in some of these models, the outer regions of the disks become gravitationally unstable.

Type
Contributed Papers
Copyright
© 2006 International Astronomical Union