EDP Sciences
Free access
Volume 410, Number 2, November I 2003
Page(s) 611 - 621
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20031279

A&A 410, 611-621 (2003)
DOI: 10.1051/0004-6361:20031279

Rosseland and Planck mean opacities for protoplanetary discs

D. Semenov1, Th. Henning2, Ch. Helling3, M. Ilgner4 and E. Sedlmayr3

1  Astrophysical Institute and University Observatory, Schillergäßchen 2-3, 07745 Jena, Germany
2  Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
3  Center for Astronomy and Astrophysics, TU Berlin, Hardenbergstraße 36, 10623 Berlin, Germany
4  Institute of Astronomy and Astrophysics, Auf der Morgenstelle 10, 72076 Tübingen, Germany

(Received 1 April 2003 / Accepted 8 August 2003 )

In this paper, we present mean gas and dust opacities relevant to the physical conditions typical of protoplanetary discs. As the principal absorber for temperatures below ~1500 K, we consider spherical and aggregate dust particles of various sizes, chemical structure, and porosity, consisting of ice, organics, troilite, silicates, and iron. For higher temperatures, ions, atoms, molecules, and electrons are included as the main opacity sources. Rosseland and Planck mean opacities are calculated for temperatures between 5 K and $10\,000$ K and gas densities ranging from 10-18 g cm -3 to 10-7 g cm -3. The dependence on the adopted model of dust grains is investigated. We compare our results with recent opacity tables and show how different opacity models affect the calculated hydrodynamical structure of accretion discs.

Key words: accretion, accretion discs -- hydrodynamics -- atomic processes -- molecular processes -- stars: planetary systems: protoplanetary discs

Offprint request: D. Semenov, dima@astro.uni-jena.de

© ESO 2003