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

Abstract

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.

14 pages, A&A in press

References in corpus (5)

• Large grains in the disk of CQ Tau
• Molecular line study of the very young protostar IRAM 04191 in Taurus: Infall, rotation, and outflow
• Non-Keplerian rotation in the nucleus of NGC 1068: evidence for a massive accretion disk?
• A Keplerian disk around the Herbig Ae star HD 34282
• Astrometric signatures of self-gravitating protoplanetary discs

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• 2-D simulations of FU Orionis disk outbursts
• Massive planets in FU Orionis discs: implications for thermal instability models
• Millimeter imaging of HD 163296: probing the disk structure and kinematics
• A 1.3 mm SMA Survey of 29 Variable Young Stellar Objects
• The Blackhole-Dark Matter Halo Connection
• Nuclear and Extended Spectra of NGC 1068 - I: Hints from Near-Infrared Spectroscopy
• On Estimating the Mass of Keplerian Accretion Disks in H2O Maser Galaxies