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dc.contributor.authorDegenaar, N.
dc.contributor.authorAltamirano, D.
dc.contributor.authorParker, M.
dc.contributor.authorMiller-Jones, James
dc.contributor.authorMiller, J.
dc.contributor.authorHeinke, C.
dc.contributor.authorWijnands, R.
dc.contributor.authorLudlam, R.
dc.contributor.authorParikh, A.
dc.contributor.authorHessels, J.
dc.contributor.authorGusinskaia, N.
dc.contributor.authorDeller, A.
dc.contributor.authorFabian, A.
dc.date.accessioned2017-01-30T13:38:52Z
dc.date.available2017-01-30T13:38:52Z
dc.date.created2016-10-05T19:30:21Z
dc.date.issued2016
dc.identifier.citationDegenaar, 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.
dc.identifier.urihttp://hdl.handle.net/20.500.11937/33719
dc.identifier.doi10.1093/mnras/stw1593
dc.description.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

dc.publisherOxford University Press
dc.titleDisc 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
dc.typeJournal Article
dcterms.source.volume461
dcterms.source.number4
dcterms.source.startPage4049
dcterms.source.endPage4058
dcterms.source.issn0035-8711
dcterms.source.titleMonthly Notices of the Royal Astronomical Society
curtin.note

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.

curtin.departmentDepartment of Physics and Astronomy
curtin.accessStatusOpen access


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