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    Gamma Rays from Kilonova: A Potential Probe of r-process Nucleosynthesis

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    Korobkin_2020_ApJ_889_168.pdf
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    Author
    Korobkin, Oleg
    Hungerford, Aimee M.
    Fryer, Christopher L.
    Mumpower, Matthew R.
    Wendell Misch, G.
    Sprouse, Trevor M.
    Lippuner, Jonas
    Surman, Rebecca
    Couture, Aaron J.
    Bloser, Peter F.
    Shirazi, Farzane
    Even, Wesley P.
    Vestrand, W. Thomas
    Miller, Richard S.
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    Affiliation
    Univ Arizona
    Issue Date
    2020-02
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Korobkin, O., Hungerford, A. M., Fryer, C. L., Mumpower, M. R., Misch, G. W., Sprouse, T. M., ... & Miller, R. S. (2020). Gamma rays from kilonova: a potential probe of r-process nucleosynthesis. The Astrophysical Journal, 889(2), 168.
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2020. 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
    The mergers of compact binaries with at least one neutron star component are the potential leading sites of the production and ejection of r-process elements. Discoveries of galactic binary pulsars, short gamma-ray bursts, and gravitational-wave detections have all been constraining the rate of these events, while the gravitational wave plus broadband electromagnetic coverage of binary neutron star merger (GW170817) has also placed constraints on the properties (mass and composition) of the merger ejecta. But uncertainties and ambiguities in modeling the optical and infrared emission make it difficult to definitively measure the distribution of heavy isotopes in these mergers. In contrast, gamma rays emitted in the decay of these neutron-rich ejecta may provide a more direct measurement of the yields. We calculate the gamma production in remnants of neutron star mergers, considering two epochs: a kilonova epoch, lasting about two weeks, and a much later epoch of tens and hundreds of thousands of years after the merger. For the kilonova epoch, when the expanding ejecta is still only partially transparent to gamma radiation, we use 3D radiative transport simulations to produce the spectra. We show that the gamma-ray spectra associated with beta- and alpha-decay provide a fingerprint of the ejecta properties and, for a sufficiently nearby remnant, may be detectable, even for old remnants. We compare our gamma spectra with the potential detection limits of next generation detectors, including the Lunar Occultation Explorer (LOX), the All-sky Medium Energy Gamma-ray Observatory (AMEGO), and the Compton Spectrometer and Imager (COSI). We show that fission models can be discriminated via the presence of short-lived fission fragments in the remnant spectra.
    Note
    Immediate access
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/ab64d8
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab64d8
    Scopus Count
    Collections
    UA Faculty Publications

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