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    National Tsing Hua University Institutional Repository > 理學院 > 天文研究所 > 期刊論文 >  Forming an early O-type star through gas accretion?


    Please use this identifier to cite or link to this item: http://nthur.lib.nthu.edu.tw/dspace/handle/987654321/53952


    Title: Forming an early O-type star through gas accretion?
    Authors: Zapata, L. A.;Palau, A.;Ho, P. T. P.;Schilke, P.;Garrod, R. T.;Rodriguez, L. F.;Menten, K.
    教師: 賀曾樸
    Date: 2008
    Publisher: EDP Sciences
    Relation: ASTRONOMY & ASTROPHYSICS,Volume: 479,Issue: 2,Pages: L25-L28,Published: FEB 2008
    Keywords: W51 MASSIVE CORES
    H2O MASER SOURCES
    DYNAMICAL COLLAPSE
    MOLECULAR OUTFLOW
    Abstract: We present high angular resolution (similar to 3 '') and sensitive 1.3 mm continuum, cyanogen (CN) and vinyl cyanide (C2H3CN) line observations made with the Submillimeter Array (SMA) toward one of most highly obscured objects of the W51 IRS2 region, W51 North. We find that the CN line exhibits a pronounced inverse P-Cygni profile indicating that the molecular gas is falling into this object with a mass accretion rate between 4 and 7 x 10(-2) M-circle dot yr(-1). The C2H3CN traces an east- west rotating molecular envelope that surrounds either a single obscured (proto) star with a kinematic mass of 40 M-circle dot or a small central cluster of B-type stars and that is associated with a compact high velocity bipolar outflow traced by H2O masers and SiO molecular emission. We thus confirm that the W51 North region is part of the growing list of young massive star forming regions that have been associated with infalling motion and with high mass accretion rates (similar to 10(-2)-10(-4) M-circle dot yr(-1)), strengthening the evidence that massive stars can form with very high accretion rates sufficient to quench the formation of a UCHII region.
    URI: http://publications.edpsciences.org/
    http://nthur.lib.nthu.edu.tw/dspace/handle/987654321/53952
    Appears in Collections:[天文研究所] 期刊論文

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