Disk-driven rotating bipolar outflow in Orion Source i

Tomoya Hirota, Masahiro N. Machida, Yuko Matsushita, Kazuhito Motogi, Naoko Matsumoto, Mi Kyoung Kim, Ross A. Burns, Mareki Honma

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88 Citations (Scopus)


One of the outstanding problems in star formation theory concerns the transfer of angular momentum so that mass can accrete onto a newly born young stellar object (YSO). From a theoretical standpoint, outflows and jets are predicted to play an essential role in the transfer of angular momentum 1,2,3,4 and their rotations have been reported for both low-5 and high-mass 6,7 YSOs. However, little quantitative discussion on outflow launching mechanisms has been presented for high-mass YSOs due to a lack of observational data. Here we present a clear signature of rotation in the bipolar outflow driven by Orion Source I, a high-mass YSO candidate, using the Atacama Large Millimeter/Submillimeter Array (ALMA). A rotational transition of silicon monoxide (Si 18 O) reveals a velocity gradient perpendicular to the outflow axis, which is consistent with that of the circumstellar disk traced by a high excitation water line. The launching radii and outward velocity of the outflow are estimated to be >10 au and 10 km s â '1, respectively. These parameters rule out the possibility that the observed outflow is produced by the entrainment of a high-velocity jet 8, and that contributions from the stellar wind 9 or X-wind 10, which have smaller launching radii, are significant in the case of Source I. Thus these results provide convincing evidence of a rotating outflow directly driven by the magneto-centrifugal disk wind launched by a high-mass YSO candidate 6,11.

Original languageEnglish
Article number0146
JournalNature Astronomy
Publication statusPublished - Mar 2 2017

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics


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