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    Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9-342058

    245837_245837.pdf (523.8Kb)
    Access Status
    Open access
    Authors
    Degenaar, N.
    Altamirano, D.
    Parker, M.
    Miller-Jones, James
    Miller, J.
    Heinke, C.
    Wijnands, R.
    Ludlam, R.
    Parikh, A.
    Hessels, J.
    Gusinskaia, N.
    Deller, A.
    Fabian, A.
    Date
    2016
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Degenaar, N. and Altamirano, D. and Parker, M. and Miller-Jones, J. and Miller, J. and Heinke, C. and Wijnands, R. et al. 2016. Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9-342058. Monthly Notices of the Royal Astronomical Society. 461 (4): pp. 4049-4058.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/stw1593
    ISSN
    0035-8711
    School
    Department of Physics and Astronomy
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/33719
    Collection
    • Curtin Research Publications
    Abstract

    RXS J180408.9–342058 is a transient neutron star low-mass X-ray binary that exhibited a bright accretion outburst in 2015. We present NuSTAR , Swift , and Chandra observations obtained around the peak brightness of this outburst. The source was in a soft X-ray spectral state and displayed an X-ray luminosity of L X _~(2–3) × 10 37 ( D / 5.8kpc) 2 ergs − 1 (0.5– 10 keV). The NuSTAR data reveal a broad Fe–K emission line that we model as relativistically broadened reflection to constrain the accretion geometry. We found that the accretion disc is viewed at an inclination of i _~27 ◦ –35 ◦ and extended close to the neutron star, down to R in _~5–7.5 gravitational radii (_~11–17 km). This inner disc radius suggests that the neutron star magnetic field strength is B ~<2 × 10 8 G. We find a narrow absorption line in the Chandra /HEG data at an energy of _~7.64 keV with a significance of _~4.8 σ. This feature could correspond to blueshifted Fe XXVI and arise from an accretion disc wind, which would imply an outflow velocity of v out _~0.086 c (_~25 800kms − 1 ). However, this would be extreme for an X-ray binary and it is unclear if a disc wind should be visible at the low inclination angle that we infer from our reflection analysis. Finally, we discuss how the X-ray and optical properties of 1RXS J180408.9–342058 are consistent with a relatively small ( P orb ~<3h) binary orbit

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