EDP Sciences Journals List
Advanced Search
Subscriber Authentication Point
Home All issues Volume 430/3 Article
Free access article

Issue A&A
Volume 430, Number 3, February II 2005
Page(s) 1133 - 1138
Section Planets and planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20041692



A&A 430, 1133-1138 (2005)
DOI: 10.1051/0004-6361:20041692

Formation of giant planets in disks with different metallicities

K. Kornet1, P. Bodenheimer2, M. Rózyczka1 and T. F. Stepinski3

1  Nicolaus Copernicus Astronomical Center, Bartycka 18, Warsaw, 00-716, Poland
    e-mail: [kornet;mnr]@camk.edu.pl
2  UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
    e-mail: peter@ucolick.org
3  Lunar and Planetary Institute, 3600 Bay Area Blvd., Houston, TX 77058, USA
    e-mail: tom@lpi.usra.edu

(Received 20 July 2004 / Accepted 20 September 2004)

Abstract
We present the first results from simulations of processes leading to planet formation in protoplanetary disks with different metallicities. For a given metallicity, we construct a two-dimensional grid of disk models with different initial masses and radii ( M0,  R0). For each disk, we follow the evolution of gas and solids from an early evolutionary stage, when all solids are in the form of small dust grains, to the stage when most solids have condensed into planetesimals. Then, based on the core accretion - gas capture scenario, we estimate the planet-bearing capability of the environment defined by the final planetesimal swarm and the still evolving gaseous component of the disk. We define the probability of planet-formation,  $P_{\rm p}$, as the normalized fractional area in the ( M0,  $\log R_0$) plane populated by disks that have formed planets inside 5 AU. With such a definition, and under the assumption that the population of planets discovered at  R < 5 AU is not significantly contaminated by planets that have migrated from  R > 5 AU, our results agree fairly well with the observed dependence between the probability that a star harbors a planet and the star's metal content. The agreement holds for the disk viscosity parameter  $\alpha$ ranging from  10-3 to  10-2, and it becomes much poorer when the redistribution of solids relative to the gas is not allowed for during the evolution of model disks.


Key words: accretion, accretion disks -- stars: planetary systems: protoplanetary disks -- stars: planetary systems: formation




© ESO 2005


What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access. An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.
  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account. In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.