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dc.contributor.authorvan den Eijnden, J
dc.contributor.authorDegenaar, N
dc.contributor.authorRussell, T D
dc.contributor.authorMiller-Jones, J C A
dc.contributor.authorEscorial, A Rouco
dc.contributor.authorWijnands, R
dc.contributor.authorSivakoff, G R
dc.contributor.authorSantisteban, J V Hernández
dc.date.accessioned2022-10-06T15:30:01Z
dc.date.available2022-10-06T15:30:01Z
dc.date.issued2022-11
dc.identifier.citationvan den Eijnden , J , Degenaar , N , Russell , T D , Miller-Jones , J C A , Escorial , A R , Wijnands , R , Sivakoff , G R & Santisteban , J V H 2022 , ' Radio monitoring of transient Be/X-ray binaries and the inflow-outflow coupling of strongly-magnetized accreting neutron stars ' , Monthly Notices of the Royal Astronomical Society , vol. 516 , no. 4 , 516 , pp. 4844–4861 . https://doi.org/10.1093/mnras/stac2518en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 281525362
dc.identifier.otherPURE UUID: 079730cc-3772-496e-899d-975ee0e3149f
dc.identifier.otherJisc: 608308
dc.identifier.otherORCID: /0000-0002-6733-5556/work/120052336
dc.identifier.otherWOS: 000857956100009
dc.identifier.otherScopus: 85159078470
dc.identifier.urihttps://hdl.handle.net/10023/26151
dc.descriptionFunding information: JvdE is supported by a Lee Hysan Junior Research Fellowship awarded by St. Hilda’s College. TDR acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.0. GRS is supported by NSERC Discovery Grants RGPIN-2016-06569 and RGPIN-2021-04001.en
dc.description.abstractStrongly-magnetized (B ≥ 1012 G) accreting neutron stars (NSs) are prime targets for studying the launching of jets by objects with a solid surface; while classical jet-launching models predict that such NSs cannot launch jets, recent observations and models argue otherwise. Transient Be/X-ray binaries (BeXRBs) are critical laboratories for probing this poorly-explored parameter space for jet formation. Here, we present the coordinated monitoring campaigns of three BeXRBs across four outbursts: giant outbursts of SAX 2103.5+4545, 1A 0535+262, and GRO J1008-57, as well as a Type-I outburst of the latter. We obtain radio detections of 1A 0535+262 during ten out of twenty observations, while the other targets remained undetected at typical limits of 20–50μJy. The radio luminosity of 1A 0535+262 positively correlates with its evolving X-ray luminosity, and inhabits a region of the LX–LR plane continuing the correlation observed previously for the BeXRB Swift J0243.6+6124. We measure a BeXRB LX–LR coupling index of β = 0.86 ± 0.06 (LX ∝ LßR ), similar to the indices measured in NS and black hole low-mass X-ray binaries. Strikingly, the coupling’s LR normalization is ∼275 and ∼6.2 × 103 times lower than in those two comparison samples, respectively. We conclude that jet emission likely dominates during the main peak of giant outbursts, but is only detectable for close-by or super-Eddington systems at current radio sensitivities. We discuss these results in the broader context of X-ray binary radio studies, concluding that our results suggest how supergiant X-ray binaries may host a currently unidentified additional radio emission mechanism.
dc.format.extent18
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © The Author(s) 2022. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.en
dc.subjectAccretion, accretion discsen
dc.subjectDtars: neutronen
dc.subjectX-rays: binariesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subjectMCCen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleRadio monitoring of transient Be/X-ray binaries and the inflow-outflow coupling of strongly-magnetized accreting neutron starsen
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/stac2518
dc.description.statusPeer revieweden


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