Astrophys. J., 726, 45 (2011/January-1)
Detection of strong millimeter emission from the circumstellar dust disk around V1094 Sco: cold and massive disk around a T Tauri star in a quiescent accretion phase?
TSUKAGOSHI T., SAITO M., KITAMURA Y., MOMOSE M., SHIMAJIRI Y., HIRAMATSU M., IKEDA N., KAMEGAI K., WILSON G., YUN M.S., SCOTT K., AUSTERMANN J., PERERA T., HUGHES D., ARETXAGA I., MAUSKOPF P., EZAWA H., KOHNO K. and KAWABE R.
Abstract (from CDS):
We present the discovery of a cold massive dust disk around the T Tauri star V1094 Sco in the Lupus molecular cloud from the 1.1 mm continuum observations with AzTEC on ASTE. A compact (r ≲ 320 AU) continuum emission coincides with the stellar position having a flux density of 272 mJy, which is the largest among T Tauri stars in Lupus. We also present the detection of molecular gas associated with the star in the five-point observations in 12CO J = 3-2 and 13CO J = 3-2. Since our 12CO and 13CO observations did not show any signature of a large-scale outflow or a massive envelope, the compact dust emission is likely to come from a disk around the star. The observed spectral energy distribution (SED) of V1094 Sco shows no distinct turnover from near-infrared to millimeter wavelengths, can be well described by a flattened disk for the dust component, and no clear dip feature around 10 µm suggestive of the absence of an inner hole in the disk. We fit a simple power-law disk model to the observed SED. The estimated disk mass ranges from 0.03 M☉ to ≳ 0.12 M☉, which is one or two orders of magnitude larger than the median disk mass of T Tauri stars in Taurus. The resultant temperature is lower than that of a flared disk with well-mixed dust in hydrostatic equilibrium and is probably attributed to the flattened disk geometry for the dust which the central star cannot illuminate efficiently. From these results, together with the fact that there is no signature of an inner hole in the SED, we suggest that the dust grains in the disk around V1094 Sco sank into the midplane with grain growth by coalescence and are in the evolutional stage just prior to or at the formation of planetesimals.
circumstellar matter - stars: formation - stars: individual: V1094 Sco
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