Evidence for disks around young high-mass stars

Details Evidence for disks around young high-mass stars Evidence for disks around young high-mass stars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011bsrsl..80..217c&link_type=abstract

Société Royale des Sciences de Liège, Bulletin, vol. 80, p. 217-222 (Proceedings of the 39th Liège Astrophysical Colloquium, hel

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The formation of high-mass stars remains a poorly understood process despite growing observational evidence in favour of accretion from a circumstellar disk onto a protostellar core. The high fraction of multiple stellar systems among the most massive stars and the fact that these stars are usually born in dense clusters can alternatively be explained by merging of intermediate-mass stars. Here we review some observations that provide direct evidence for large (˜ 10,000 - 20,000 AU) disks and/or dusty envelopes seen in emission and absorption around high-mass stars. The objects are all members of the young cluster in M 17 and have been investigated by multicolor photometry and spectroscopy.

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