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Title:
An Evolved Disk Surrounding the Massive Main-Sequence Star MWC 297?
Authors:
Manoj, P.; Ho, Paul T. P.; Ohashi, Nagayoshi; Zhang, Qizhou; Hasegawa, Tatsuhiko; Chen, Huei-Ru; Bhatt, H. C.; Ashok, N. M.
Affiliation:
AA(Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan.), AB(Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan.; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA.), AC(Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan.), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA.), AE(Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan.), AF(Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan.), AG(Indian Institute of Astrophysics, II Block, Koramangala, Bangalore, India.), AH(Physical Research Laboratory, Ahmedabad, India.)
Publication:
The Astrophysical Journal, Volume 667, Issue 2, pp. L187-L190. (ApJL Homepage)
Publication Date:
10/2007
Origin:
UCP
ApJ Keywords:
Stars: Circumstellar Matter, Stars: Planetary Systems: Protoplanetary Disks, Stars: Early-Type, Stars: Emission-Line, Be, Stars: Individual: Alphanumeric: MWC 297
DOI:
10.1086/522424
Bibliographic Code:
2007ApJ...667L.187M

Abstract

We present the results of the interferometric observations of the circumstellar disk surrounding MWC 297 in the continuum at 230 GHz (1.3 mm) and in the (J=2-1) rotational transitions of 12CO,13CO, and C18O using the Submillimeter Array. At a distance of 250 pc, MWC 297 is one of the closest, young massive stars (M*~10 Msolar) to us. Compact continuum emission is detected toward MWC 297 from which we estimate a disk mass (gas+dust) of 0.07 Msolar and a disk radius of <=80 AU. Our result demonstrates that circumstellar disks can survive around massive stars well into their main-sequence phase even after they have become optically visible. Complementing our observations with the data compiled from the literature, we find the submillimeter dust opacity index β to be between 0.1 and 0.3. If the emission is optically thin, the low value of β indicates the presence of relatively large grains in the disk, possibly because of grain growth. We do not detect any CO emission associated with the continuum source. We argue that the 13CO emission from the disk is likely optically thin, in which case we derive an upper limit to the gas mass that implies significant depletion of molecular gas in the disk. The mass of this disk and the evolutionary trends observed are similar to those found for intermediate-mass Herbig Ae stars and low-mass T Tauri stars.
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