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

Author

Listed:
  • Nimesh A. Patel

    (Harvard-Smithsonian Center for Astrophysics)

  • Salvador Curiel

    (Harvard-Smithsonian Center for Astrophysics
    Instituto de Astronomia, UNAM)

  • 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
    Academica Sinica Institute of Astronomy and Astrophysics)

  • José M. Torrelles

    (Consejo Superior de Investigaciones Científicas-IEEC
    Royal Observatory Edinburgh)

  • James M. Moran

    (Harvard-Smithsonian Center for Astrophysics)

  • José F. Gómez

    (Laboratorio de Astrofísica Espacial y Física Fundamental, INTA
    Instituto de Astrofísica de Andalucia, CSIC)

  • Guillem Anglada

    (Instituto de Astrofísica de Andalucia, CSIC)

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.

Suggested Citation

  • 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 & Guillem Anglada, 2005. "A disk of dust and molecular gas around a high-mass protostar," Nature, Nature, vol. 437(7055), pages 109-111, September.
    • Handle: RePEc:nat:nature:v:437:y:2005:i:7055:d:10.1038_nature04011
    DOI: 10.1038/nature04011
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