A disk of dust and molecular gas around a high-mass protostar

Nimesh A. Patel (), Salvador Curiel, T. K. Sridharan, Qizhou Zhang, Todd R. Hunter, Paul T. P. Ho, José M. Torrelles, James M. Moran, José F. Gómez and Guillem Anglada
Additional contact information
Nimesh A. Patel: Harvard-Smithsonian Center for Astrophysics
Salvador Curiel: Harvard-Smithsonian Center for Astrophysics
T. K. Sridharan: Harvard-Smithsonian Center for Astrophysics
Qizhou Zhang: Harvard-Smithsonian Center for Astrophysics
Todd R. Hunter: Harvard-Smithsonian Center for Astrophysics
Paul T. P. Ho: Harvard-Smithsonian Center for Astrophysics
José M. Torrelles: Consejo Superior de Investigaciones Científicas-IEEC
James M. Moran: Harvard-Smithsonian Center for Astrophysics
José F. Gómez: Laboratorio de Astrofísica Espacial y Física Fundamental, INTA
Guillem Anglada: Instituto de Astrofísica de Andalucia, CSIC

Nature, 2005, vol. 437, issue 7055, 109-111

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/nature04011

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