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dc.contributor.authorCastro Segura, N.
dc.contributor.authorKnigge, C.
dc.contributor.authorLong, K. S.
dc.contributor.authorAltamirano, D.
dc.contributor.authorArmas Padilla, M.
dc.contributor.authorBailyn, C.
dc.contributor.authorBuckley, D. A. H.
dc.contributor.authorBuisson, D. J. K.
dc.contributor.authorCasares, J.
dc.contributor.authorCharles, P.
dc.contributor.authorCombi, J. A.
dc.contributor.authorCúneo, V. A.
dc.contributor.authorDegenaar, N. D.
dc.contributor.authordel Palacio, S.
dc.contributor.authorDíaz Trigo, M.
dc.contributor.authorFender, R.
dc.contributor.authorGandhi, P.
dc.contributor.authorGeorganti, M.
dc.contributor.authorGutiérrez, C.
dc.contributor.authorHernandez Santisteban, J. V.
dc.contributor.authorJiménez-Ibarra, F.
dc.contributor.authorMatthews, J.
dc.contributor.authorMéndez, M.
dc.contributor.authorMiddleton, M.
dc.contributor.authorMuñoz-Darias, T.
dc.contributor.authorÖzbey Arabacı, M.
dc.contributor.authorPahari, M.
dc.contributor.authorRhodes, L.
dc.contributor.authorRussell, T. D.
dc.contributor.authorScaringi, S.
dc.contributor.authorvan den Eijnden, J.
dc.contributor.authorVasilopoulos, G.
dc.contributor.authorVincentelli, F. M.
dc.contributor.authorWiseman, P.
dc.date.accessioned2022-09-01T23:49:41Z
dc.date.available2022-09-01T23:49:41Z
dc.date.issued2022-03-03
dc.identifier.citationCastro Segura , N , Knigge , C , Long , K S , Altamirano , D , Armas Padilla , M , Bailyn , C , Buckley , D A H , Buisson , D J K , Casares , J , Charles , P , Combi , J A , Cúneo , V A , Degenaar , N D , del Palacio , S , Díaz Trigo , M , Fender , R , Gandhi , P , Georganti , M , Gutiérrez , C , Hernandez Santisteban , J V , Jiménez-Ibarra , F , Matthews , J , Méndez , M , Middleton , M , Muñoz-Darias , T , Özbey Arabacı , M , Pahari , M , Rhodes , L , Russell , T D , Scaringi , S , van den Eijnden , J , Vasilopoulos , G , Vincentelli , F M & Wiseman , P 2022 , ' A persistent ultraviolet outflow from an accreting neutron star binary transient ' , Nature , vol. 603 , no. 7899 , pp. 52-57 . https://doi.org/10.1038/s41586-021-04324-2en
dc.identifier.issn1476-4687
dc.identifier.otherPURE: 278276629
dc.identifier.otherPURE UUID: f5055925-a3da-4458-a3d7-99824605de90
dc.identifier.otherRIS: urn:F184AF908B333D076627BED9FBB490CE
dc.identifier.otherRIS: Castro Segura2022
dc.identifier.otherORCID: /0000-0002-6733-5556/work/110131904
dc.identifier.otherWOS: 000763605400010
dc.identifier.otherScopus: 85125614681
dc.identifier.urihttps://hdl.handle.net/10023/25936
dc.descriptionJ.V.H.S. acknowledges support from STFC grant ST/R000824/1.en
dc.description.abstractAll disc-accreting astrophysical objects produce powerful disc winds. In compact binaries containing neutron stars or black holes, accretion often takes place during violent outbursts. The main disc wind signatures during these eruptions are blue-shifted X-ray absorption lines, which are preferentially seen in disc-dominated ‘soft states’1,2. By contrast, optical wind-formed lines have recently been detected in ‘hard states’, when a hot corona dominates the luminosity3. The relationship between these signatures is unknown, and no erupting system has as yet revealed wind-formed lines between the X-ray and optical bands, despite the many strong resonance transitions in this ultraviolet (UV) region4. Here we report that the transient neutron star binary Swift J1858.6-0814 exhibits wind-formed, blue-shifted absorption lines associated with C iv, N v and He ii in time-resolved UV spectroscopy during a luminous hard state, which we interpret as a warm, moderately ionized outflow component in this state. Simultaneously observed optical lines also display transient blue-shifted absorption. Decomposing the UV data into constant and variable components, the blue-shifted absorption is associated with the former. This implies that the outflow is not associated with the luminous flares in the data. The joint presence of UV and optical wind features reveals a multi-phase and/or spatially stratified evaporative outflow from the outer disc5. This type of persistent mass loss across all accretion states has been predicted by radiation–hydrodynamic simulations6 and helps to explain the shorter-than-expected duration of outbursts7.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofNatureen
dc.rightsCopyright © 2022, The Author(s), under exclusive licence to Springer Nature Limited. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1038/s41586-021-04324-2.en
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subject3rd-DASen
dc.subjectACen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleA persistent ultraviolet outflow from an accreting neutron star binary transienten
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1038/s41586-021-04324-2
dc.description.statusPeer revieweden
dc.date.embargoedUntil2022-09-02
dc.identifier.urlhttps://arxiv.org/abs/2203.01372en
dc.identifier.grantnumberST/R00824/1en


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