Sub-millimeter Interferometric Study of Circumstellar Disks Surrounding Optically Visible, Young High Mass Stars

Details Sub-millimeter Interferometric Study of Circumstellar Disks Surrounding Optically Visible, Young High Mass Stars Sub-millimeter Interferometric Study of Circumstellar Disks Surrounding Optically Visible, Young High Mass Stars

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.1005m&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #10.05; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

Observational evidence for circumstellar disks surrounding high mass (M > 8 M_sun) stars are currently limited to the deeply embedded, protostellar phase, where it is not clear if the central object is a single protostar, a multiple system or an unresolved star cluster. One of the ways to overcome the ambiguity about the central source is to search for the presence of disk around massive young stars at a less embedded, more evolved phase. We are carrying out an interferometric study of circumstellar disks surrounding optically visible, young high mass ( M = 8 18 M_sun) stars, which exhibit strong evidence for the presence of accreting disks associated with them. Here we present Sub-Millimeter Array (SMA) observations at 230 GHz of the circumstellar environment of a B1.5 star MWC 297, which, at a distance of 250 pc, is one of the closest massive (M=12 M_sun) star associated with a star forming cloud. Investigation of the structure and properties of circumstellar disks in these relatively 'evolved' systems has implications for the studies of disk evolution in massive young stars.

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