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    New Circumstellar Sources of PO and PN: The Increasing Role of Phosphorus Chemistry in Oxygen-rich Stars

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    Ziurys_2018_ApJ_856_169.pdf
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    Author
    Ziurys, L. M.
    Schmidt, D. R.
    Bernal, J. J.
    Affiliation
    Univ Arizona, Dept Chem & Biochem, 1305 E 4th St, Tucson, AZ 85719 USA
    Univ Arizona, Arizona Radio Observ, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA
    Issue Date
    2018-04-01
    Keywords
    astrochemistry
    circumstellar matter
    ISM: molecules
    methods: observational
    stars: abundances
    submillimeter: stars
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    The Astrophysical Journal, 856:169 (11pp), 2018 April 1
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2018. 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
    PO and PN have been newly identified in several oxygen-rich circumstellar envelopes, using the Submillimeter Telescope of the Arizona Radio Observatory. The J = 5 -> 4 and J = 6 -> 5 transitions of PN near 235 and 282 GHz, and the lambda doublets originating in the J = 5.5 -> 4.5 and J = 6.5 -> 5.5 lines of PO at 240 and 284 GHz, have been detected toward the shells of asymptotic giant branch (AGB) stars TX Cam and R Cas. A similar set of lines has been observed toward the supergiant NML Cyg, and new transitions of these two molecules were also measured toward the AGB star IK Tau. Along with the previous data from VY Canis Majoris (VY CMa), these spectral lines were analyzed using the non-local thermodynamic equilibrium (non-LTE) circumstellar modeling code, ESCAPADE. For the AGB stars, peak abundances found for PN and PO were f similar to (1-2) x 10(-8) and (0.5-1) x 10(-7), respectively, while those for the supergiants were f(PN) (0.3-0.7) x 10(-8) and f(PO) similar to (5-7) x 10(-8). PN was well modeled with a spherical radial distribution, suggesting formation near the stellar photosphere, perhaps enhanced by shocks. PO was best reproduced by a shell model, indicating a photochemical origin, except for VY CMa. Overall, the abundance of PO is a factor of 5-20 greater than that of PN. This study suggests that phosphorus-bearing molecules are common in O-rich envelopes, and that a significant amount of phosphorus (>20%) remains in the gas phase.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aaafc6
    Version
    Final published version
    Sponsors
    NSF [AST1515568, AST-1140030]; NSF University Radio Observatories (URO) program [AST-1140030]; NASA [NNX15AD94G]
    Additional Links
    http://stacks.iop.org/0004-637X/856/i=2/a=169?key=crossref.4f275cf63fe688f3f7d57d74245ee3bf
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aaafc6
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