Probing the rotation curve of the outer accretion disk in FU Orionis objects with long-wavelength spectroscopy

Details Probing the rotation curve of the outer accretion disk in FU Orionis objects with long-wavelength spectroscopy Probing the rotation curve of the outer accretion disk in FU Orionis objects with long-wavelength spectroscopy

2003-07-07

arxiv.org/abs/astro-ph/0307122v1

Astron.Astrophys.408:1015-1028,2003

Astronomy and Astrophysics

Astrophysics

14 pages, A&A in press

Scientific paper

10.1051/0004-6361:20031045

Studies of the Spectral Energy Distribution of Young Stellar Objects suggest that the outer disk of FU Orionis objects might be self-gravitating. In this paper we propose a method to test directly whether, in these objects, significant deviations from Keplerian rotation occur. In a first approach, we have used a simplified model of the disk vertical structure that allows us to quickly bring out effects related to the disk self-gravity. We find that the often studied optical and near-infrared line profiles are produced too close to the central object to provide significant evidence for non-Keplerian rotation. Based on parameters relevant for the case of FU Ori, we show that high-resolution long-wavelength spectroscopy, of the far-infrared H$_2$ pure rotational lines (sometimes observed in ``passive'' protostellar disks) and sub-mm CO lines, should be well suited to probe the rotation curve in the outer disk, thus measuring to what extent it is affected by the disk self-gravity. The results of the present exploratory paper should be extended soon to a more realistic treatment of the disk vertical structure.

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