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A ∼0.2-solar-mass protostar with a Keplerian disk in the very young L1527 IRS system

Author

Listed:
  • John J. Tobin

    (National Radio Astronomy Observatory)

  • Lee Hartmann

    (University of Michigan)

  • Hsin-Fang Chiang

    (University of Illinois
    Institute for Astronomy and NASA Astrobiology Institute, University of Hawaii at Manoa)

  • David J. Wilner

    (Harvard-Smithsonian Center for Astrophysics)

  • Leslie W. Looney

    (University of Illinois)

  • Laurent Loinard

    (Centro de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico
    Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany)

  • Nuria Calvet

    (University of Michigan)

  • Paola D’Alessio

    (Centro de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico)

Abstract

In the earliest stage of star formation, protostars accrete mass from their surrounding envelopes through circumstellar disks; observations of the protostar L1527 IRS find a large, rotating proto-planetary disk from which the protostellar mass is measured to be 0.19 solar masses, with a protostar-to-envelope mass ratio of about 0.2.

Suggested Citation

  • John J. Tobin & Lee Hartmann & Hsin-Fang Chiang & David J. Wilner & Leslie W. Looney & Laurent Loinard & Nuria Calvet & Paola D’Alessio, 2012. "A ∼0.2-solar-mass protostar with a Keplerian disk in the very young L1527 IRS system," Nature, Nature, vol. 492(7427), pages 83-85, December.
    • Handle: RePEc:nat:nature:v:492:y:2012:i:7427:d:10.1038_nature11610
    DOI: 10.1038/nature11610
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