EDP Sciences
Free Access
Volume 389, Number 2, July II 2002
Page(s) 464 - 474
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20020608
Published online 27 June 2002

A&A 389, 464-474 (2002)
DOI: 10.1051/0004-6361:20020608

Vertical structure models of T Tauri and Herbig Ae/Be disks

C. P. Dullemond, G. J. van Zadelhoff and A. Natta

Max Planck Institut für Astrophysik, PO Box 1317, 85741 Garching, Germany
    e-mail: dullemon@mpa-garching.mpg.de Leiden Observatory, PO Box 9513, 2300 Leiden, The Netherlands
    e-mail: zadelhof@strw.leidenuniv.nl Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy

(Received 12 February 2002 / Accepted 15 April 2002)

In this paper we present detailed models of the vertical structure (temperature and density) of passive irradiated circumstellar disks around T Tauri and Herbig Ae/Be stars. In contrast to earlier work, we use full frequency- and angle-dependent radiative transfer instead of the usual moment equations. We find that this improvement of the radiative transfer has a strong influence on the resulting vertical structure of the disk, with differences in temperature as large as 70%. However, the spectral energy distribution (SED) is only mildly affected by this change. In fact, the SED compares reasonably well with that of improved versions of the Chiang & Goldreich (CG) model. This shows that the latter is a reasonable model for the SED, in spite of its simplicity. It also shows that from the SED alone, little can be learned about the vertical structure of a passive circumstellar disk. The molecular line emission from these disks is more sensitive to the vertical temperature and density structure, and we show as an example how the intensity and profiles of various CO lines depend on the adopted disk model. The models presented in this paper can also serve as the basis of theoretical studies of e.g. dust coagulation and settling in disks.

Key words: accretion, accretion disks -- stars: circumstellar matter -- stars: formation -- stars: pre-main sequence -- infrared: stars

Offprint request: C. P. Dullemond, dullemon@mpa-garching.mpg.de

© ESO 2002

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