A circumstellar disk associated with a massive protostellar object

Zhibo Jiang (), Motohide Tamura, Misato Fukagawa, Jim Hough, Phil Lucas, Hiroshi Suto, Miki Ishii and Ji Yang
Additional contact information
Zhibo Jiang: Chinese Academic of Sciences
Motohide Tamura: National Astronomical Observatories of Japan
Misato Fukagawa: National Astronomical Observatories of Japan
Jim Hough: University of Hertfordshire, College Lane
Phil Lucas: University of Hertfordshire, College Lane
Hiroshi Suto: National Astronomical Observatories of Japan
Miki Ishii: National Astronomical Observatories of Japan
Ji Yang: Chinese Academic of Sciences

Nature, 2005, vol. 437, issue 7055, 112-115

Abstract: Reach for the stars There are two competing theories to explain how high-mass stars form: either they arise from mergers of low-mass younger stellar objects or, like low-mass stars, they arise by accretion from a circumstellar disk. The latter theory gets a boost from new observations of disks of dust and molecular gas around two high-mass protostars. A 15-solar-mass protostar in the Cepheus A region, and the 7-solar-mass Becklin–Neugebauer object in the famous star-forming region in Orion appear well on the way to star formation by accretion.

Date: 2005
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DOI: 10.1038/nature04012

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