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dc.contributor.authorvan den Eijnden, J.
dc.contributor.authorDegenaar, N.
dc.contributor.authorSchulz, N. S.
dc.contributor.authorNowak, M. A.
dc.contributor.authorWijnands, R.
dc.contributor.authorRussell, T. D.
dc.contributor.authorHernández Santisteban, J. V.
dc.contributor.authorBahramian, A.
dc.contributor.authorMaccarone, T. J.
dc.contributor.authorKennea, J. A.
dc.contributor.authorHeinke, C. O.
dc.date.accessioned2019-09-11T10:30:03Z
dc.date.available2019-09-11T10:30:03Z
dc.date.issued2019-08
dc.identifier.citationvan den Eijnden , J , Degenaar , N , Schulz , N S , Nowak , M A , Wijnands , R , Russell , T D , Hernández Santisteban , J V , Bahramian , A , Maccarone , T J , Kennea , J A & Heinke , C O 2019 , ' Chandra reveals a possible ultrafast outflow in the super-Eddington Be/X-ray binary Swift J0243.6+6124 ' Monthly Notices of the Royal Astronomical Society , vol. 487 , no. 3 , pp. 4355-4371 . https://doi.org/10.1093/mnras/stz1548en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 261032641
dc.identifier.otherPURE UUID: 96ff89f9-9959-4a66-a5f1-a1cfbe377690
dc.identifier.otherBibCode: 2019MNRAS.487.4355V
dc.identifier.otherORCID: /0000-0002-6733-5556/work/61370247
dc.identifier.urihttp://hdl.handle.net/10023/18458
dc.description.abstractAccretion at super-Eddington rates is expected to be accompanied by strong outflows. Such outflows are observed in Galactic X-ray binaries and extragalactic ultraluminous X-ray sources (ULXs). However, due to their large source distances, ULX outflows are challenging to detect and study in detail. Galactic neutron stars accreting from a Be-star companion at super-Eddington rates show many similarities to ULX pulsars, and therefore offer an alternative approach to study outflows in this accretion regime. Here, we present Chandra high-resolution spectroscopy of such a super-Eddington accreting neutron star, Swift J0243.6+6124, to search for wind outflow signatures during the peak of its 2017/2018 giant outburst. We detect narrow emission features at rest from Ne, Mg, S, Si, and Fe. In addition, we detect a collection of absorption features which can be identified in two ways: either as all Fe transitions at rest (with a possible contribution from Mg), or a combination of three blue-shifted Ne and Mg lines at ∼0.22c, while the remaining lines are at rest. The second scenario would imply an outflow with a velocity similar to those seen in ULXs, including the ULX pulsar NGC 300 ULX-1. This result would also imply that Swift J0243.6+6124 launches both a jet, detected in radio and reported previously, and an ultrafast wind outflow simultaneously at super-Eddington accretion rates.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © The Author(s) 2019. Published by Oxford University Press on behalf of The Royal Astronomical Society. This is an Open Access article distributed under the terms of the CreativeCommons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium,provided the original work is properly citeden
dc.subjectAccretionen
dc.subjectAccretion discsen
dc.subjectStars: neutronen
dc.subjectPulsars: individual: Swift J0243.6+6124en
dc.subjectX-rays: binariesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleChandra reveals a possible ultrafast outflow in the super-Eddington Be/X-ray binary Swift J0243.6+6124en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz1548
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1906.01597en
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019MNRAS.487.4355Ven


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