Physical parameters of the Keplerian protoplanetary disk of DM Tauri
Stéphane Guilloteau and
Received 22 June 1998 / Accepted 24 August 1998
We present high sensitivity 3" aperture synthesis images of the DM Tau protoplanetary disk in the line. The images unambiguously reveal that the disk is rotating around the central star. To model the observations in terms of a rotating disk in hydrostatic equilibrium, we have developped a fitting procedure which allows derivation of the disk parameters and their errors. Dependencies among the disk parameters are discussed in detail. The disk is large, with an outer radius of 850 AU. We find that the rotation curve is essentially Keplerian, at least up to 600 AU. The stellar mass derived from the rotation curve is . The intrinsic local velocity dispersion in the disk is found to be essentially thermal, with a turbulent component of less than 30 % of the thermal width. Parameters derived from this observation are used to confirm the molecular abundances and depletion factors estimated for several simple organic molecules by Dutrey et al (1997) for DM Tau.
Key words: stars: individual: DM Tau circumstellar matter stars: pre-main sequence radio-lines: stars
Send offprint requests to: S. Guilloteau
© European Southern Observatory (ESO) 1998
Online publication: October 21, 1998