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dc.contributor.authorvan den Eijnden, J
dc.contributor.authorDegenaar, N
dc.contributor.authorRussell, T D
dc.contributor.authorWijnands, R
dc.contributor.authorBahramian, A
dc.contributor.authorMiller-Jones, J C A
dc.contributor.authorSantisteban, J V Hernández
dc.contributor.authorGallo, E
dc.contributor.authorAtri, P
dc.contributor.authorPlotkin, R M
dc.contributor.authorMaccarone, T J
dc.contributor.authorSivakoff, G
dc.contributor.authorMiller, J M
dc.contributor.authorReynolds, M
dc.contributor.authorRussell, D M
dc.contributor.authorMaitra, D
dc.contributor.authorHeinke, C O
dc.contributor.authorPadilla, M Armas
dc.contributor.authorShaw, A W
dc.identifier.citationvan den Eijnden , J , Degenaar , N , Russell , T D , Wijnands , R , Bahramian , A , Miller-Jones , J C A , Santisteban , J V H , Gallo , E , Atri , P , Plotkin , R M , Maccarone , T J , Sivakoff , G , Miller , J M , Reynolds , M , Russell , D M , Maitra , D , Heinke , C O , Padilla , M A & Shaw , A W 2021 , ' A new radio census of neutron star X-ray binaries ' , Monthly Notices of the Royal Astronomical Society , vol. 507 , no. 3 , pp. 3899–3922 .
dc.identifier.otherPURE: 276086348
dc.identifier.otherPURE UUID: eaa1fc83-3297-46d1-b820-de30a1624194
dc.identifier.otherJisc: b20a891d6be945188f65084a5c235ea1
dc.identifier.otherORCID: /0000-0002-6733-5556/work/100901678
dc.descriptionFunding: JvdE is supported by a Lee Hysan Junior Research Fellowship awarded by St. Hilda’s College, and, together with ND, by an NWO Vidi grant awarded to ND. COH is supported by NSERC Discovery Grant RGPIN-2016-04602. TDR acknowledges financial contribution from ASI-INAF n.2017-14-H.0, an INAF main stream grant.en
dc.description.abstractWe report new radio observations of a sample of thirty-six neutron star (NS) X-ray binaries, more than doubling the sample in the literature observed at current-day sensitivities. These sources include thirteen weakly-magnetised (B < 1010 G) and twenty-three strongly-magnetised (B ≥ 1010 G) NSs. Sixteen of the latter category reside in high-mass X-ray binaries, of which only two systems were radio-detected previously. We detect four weakly and nine strongly-magnetised NSs; the latter are systematically radio fainter than the former and do not exceed LR ≈ 3 × 1028 erg/s. In turn, we confirm the earlier finding that the weakly-magnetized NSs are typically radio fainter than accreting stellar-mass black holes. While an unambiguous identification of the origin of radio emission in high-mass X-ray binaries is challenging, we find that in all but two detected sources (Vela X-1 and 4U 1700-37) the radio emission appears more likely attributable to a jet than the donor star wind. The strongly-magnetised NS sample does not reveal a global correlation between X-ray and radio luminosity, which may be a result of sensitivity limits. Furthermore, we discuss the effect of NS spin and magnetic field on radio luminosity and jet power in our sample. No current model can account for all observed properties, necessitating the development and refinement of NS jet models to include magnetic field strengths up to 1013 G. Finally, we discuss jet quenching in soft states of NS low-mass X-ray binaries, the radio non-detections of all observed very-faint X-ray binaries in our sample, and future radio campaigns of accreting NSs.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. 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 final published version of the work, which was originally published at
dc.subjectStars: neutronen
dc.subjectAccretion discsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleA new radio census of neutron star X-ray binariesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.description.statusPeer revieweden

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