Constraints on the HL Tauri Protostellar Disk from Millimeter- and Submillimeter-Wave Interferometry

Details Constraints on the HL Tauri Protostellar Disk from Millimeter- and Submillimeter-Wave Interferometry Constraints on the HL Tauri Protostellar Disk from Millimeter- and Submillimeter-Wave Interferometry

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...489..917l&link_type=abstract

Astrophysical Journal v.489, p.917

Astronomy and Astrophysics

Astronomy

62

Stars: Circumstellar Matter, Infrared: Stars, Stars: Individual Constellation Name: Hl Tauri, Stars: Pre-Main-Sequence, Techniques: Interferometric

Scientific paper

Millimeter and submillimeter interferometry is used to probe the dusty accretion disks around young protostars. New 460 GHz ( lambda = 650 mu m) data from the Caltech Submillimeter Observatory and the James Clerk Maxwell Telescope CSO-JCMT Interferometer are combined with previous 345 GHz ( lambda = 870 mu m) data from CSO-JCMT, 220 GHz ( lambda = 1.4 mm) data from the Owens Valley Radio Observatory (OVRO) Millimeter Array, 110 GHz ( lambda = 2.7 mm) data from the Berkeley-Illinois-Maryland Association Array (BIMA), and 43 GHz ( lambda = 7 mm) data from the VLA, in order to constrain the nature of the protostellar disk around HL Tau on size scales of 50 AU and above. A power-law disk model is fitted directly to the measured visibility data, and probability distributions are derived for the parameters. The effects of instrumental uncertainties are included in a consistent way. The position angle of the major axis of the emission is determined to be 127 deg +/- 5 deg and the inclination 42 deg +/- 5 deg (where 0 deg is face-on), assuming the disk is thin, flat, and circular. A strongly flared disk that is close to edge-on cannot be ruled out, however. The CSO-JCMT and OVRO data favor centrally concentrated distributions of the surface density Sigma , where Sigma ~ r-p, and p > 1. This is not compatible with the relatively large sizes measured at lower frequency by BIMA and the VLA. No simple power-law disk model can be found that reproduces all of the millimeter and submillimeter data well. Such a model, with radial power laws in the surface density and temperature, and a single dust component, is therefore unlikely to be a good representation of the actual disk structure. One possibility that would help to reconcile the model with the data is the existence of more than one dust component, i.e., a range of grain sizes or structures in the disk and no unique value of the emissivity index beta . Future models should allow for this as well as for disk geometries that are not thin and flat.

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