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    Potential cooling of an accretion-heated neutron star crust in the low-mass X-ray binary 1RXS J180408.9-342058

    254826.pdf (867.4Kb)
    Access Status
    Open access
    Authors
    Parikh, A.
    Wijnands, R.
    Degenaar, N.
    Ootes, L.
    Page, D.
    Altamirano, D.
    Cackett, E.
    Deller, A.
    Gusinskaia, N.
    Hessels, J.
    Homan, J.
    Linares, M.
    Miller, J.
    Miller-Jones, James
    Date
    2017
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Parikh, A. and Wijnands, R. and Degenaar, N. and Ootes, L. and Page, D. and Altamirano, D. and Cackett, E. et al. 2017. Potential cooling of an accretion-heated neutron star crust in the low-mass X-ray binary 1RXS J180408.9-342058. Monthly Notices of the Royal Astronomical Society. 466 (4): pp. 4074-4082.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/stw3388
    ISSN
    0035-8711
    School
    Department of Physics and Astronomy
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    URI
    http://hdl.handle.net/20.500.11937/55765
    Collection
    • Curtin Research Publications
    Abstract

    We have monitored the transient neutron star low-mass X-ray binary 1RXS J180408.9−342058 in quiescence after its ∼4.5 month outburst in 2015. The source has been observed using Swift and XMM–Newton. Its X-ray spectra were dominated by a thermal component. The thermal evolution showed a gradual X-ray luminosity decay from ∼18 × 1032 to ∼4 × 1032 (D/5.8 kpc)2 erg s−1 between ∼8 and ∼379 d in quiescence, and the inferred neutron star surface temperature (for an observer at infinity; using a neutron star atmosphere model) decreased from ∼100 to ∼71 eV. This can be interpreted as cooling of an accretion-heated neutron star crust. Modelling the observed temperature curve (using nscool) indicated that the source required ∼1.9 MeV per accreted nucleon of shallow heating in addition to the standard deep crustal heating to explain its thermal evolution. Alternatively, the decay could also be modelled without the presence of deep crustal heating, only having a shallow heat source (again ∼1.9 MeV per accreted nucleon was required). However, the XMM–Newton data statistically required an additional power-law component. This component contributed ∼30 per cent of the total unabsorbed flux in 0.5–10 keV energy range. The physical origin of this component is unknown. One possibility is that it arises from low-level accretion. The presence of this component in the spectrum complicates our cooling crust interpretation because it might indicate that the smooth luminosity and temperature decay curves we observed may not be due to crust cooling but due to some other process.

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