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

John J. Tobin (), Lee Hartmann, Hsin-Fang Chiang, David J. Wilner, Leslie W. Looney, Laurent Loinard, Nuria Calvet and Paola D’Alessio
Additional contact information
John J. Tobin: National Radio Astronomy Observatory
Lee Hartmann: University of Michigan
Hsin-Fang Chiang: University of Illinois
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
Nuria Calvet: University of Michigan
Paola D’Alessio: Centro de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico

Nature, 2012, vol. 492, issue 7427, 83-85

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.

Date: 2012
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DOI: 10.1038/nature11610

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