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    The ALMA View of the OMC1 Explosion in Orion

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    Bally_2017_ApJ_837_60.pdf
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    Author
    Bally, John cc
    Ginsburg, Adam cc
    Arce, Hector cc
    Eisner, Josh A. cc
    Youngblood, Allison
    Zapata, Luis cc
    Zinnecker, Hans
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2017-03-03
    Keywords
    Herbig-Haro objects - ISM
    individual objects (Orion OMC1) - ISM
    jets and outflows stars - stars
    formation -stars
    massive
    
    Metadata
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    Publisher
    IOP PUBLISHING LTD
    Citation
    The ALMA View of the OMC1 Explosion in Orion 2017, 837 (1):60 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2017. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    Most massive stars form in dense clusters where gravitational interactions with other. stars may be common. The two nearest forming massive stars, the BN object and Source I, located behind the Orion Nebula, were ejected with velocities of similar to 29 and similar to 13 km s(-1) about 500 years ago by such interactions. This event generated an explosion in the gas. New ALMA observations show in unprecedented detail, a roughly spherically symmetric distribution of over a hundred (CO)-C-12 J = 2-1 streamers with velocities extending from V-LSR = -150 to +145 km s(-1) The streamer radial velocities increase (or decrease) linearly with projected distance from the explosion center, forming a '' Hubble Flow '' confined to within 50 ''. of the explosion center. They point toward the high proper-motion, shock-excited H-2 and [Fe II] '' fingertips '' and lower-velocity CO in the H-2 wakes comprising Orion's '' fingers.'' In some directions, the H-2 '' fingers '' extend more than a factor of two farther from the ejection center than the CO streamers. Such deviations from spherical symmetry may be caused by ejecta running into dense gas or the dynamics of the N-body interaction that ejected the stars and produced the explosion. This similar to 10(48) erg event may have been powered by the release of gravitational potential energy associated with the formation of a compact binary or a protostellar merger. Orion may be the prototype for a new class of stellar explosiozn responsible for luminous infrared transients in nearby galaxies.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aa5c8b
    Version
    Final published version
    Sponsors
    National Science Foundation (NSF) [AST-1009847]; ALMA [2013.1.00546.S]; CONACyT, Mexico; DGAPA; UNAM
    Additional Links
    http://stacks.iop.org/0004-637X/837/i=1/a=60?key=crossref.5965b77c3c782a63e13e00b95c848a1e
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aa5c8b
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    UA Faculty Publications

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