On the lack of X-ray pulsation in most neutron star low-mass X-ray binaries

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dc.contributor.authorNiang, N.
dc.contributor.authorErtan, U.
dc.contributor.authorGencali, A. A.
dc.contributor.authorToyran, O.
dc.contributor.authorUlubay, A.
dc.contributor.authorDevlen, E.
dc.contributor.authorAlpar, M. A.
dc.date.accessioned2024-08-31T07:46:45Z
dc.date.available2024-08-31T07:46:45Z
dc.date.issued2024
dc.departmentEge Üniversitesien_US
dc.description.abstractWe have investigated whether the lack of X-ray pulsations from most neutron star (NS) low-mass X-ray binaries (LMXBs) could be due to the extension of their inner disc to the NS surface. To estimate the inner disc radii, we have employed the model, recently proposed to account for the torque reversals of LMXBs. In this model, the inner disc radius depends on the spin period as well as the dipole moment and the mass inflow rate of the disc. Our model results indicate that most LMXBs have mass accretion rates above the minimum critical rates required for the inner disc to reach down to the NS surface and thereby quench the pulsed X-ray emission. For most sources X-ray pulsations are allowed when the period decreases below a certain critical value. For the same parameters, the model is also consistent with the observed X-ray luminosity ranges of the individual accreting millisecond X-ray pulsars (AMXPs). The paucity of AMXPs compared to the majority population of non-pulsing LMXBs is explained, as well as the fact that AMXPs are transient sources.en_US
dc.description.sponsorshipSabancimath; University; TUEBIdot;TAK (The Scientific and Technological Research Council of Turkey) [123F083]; National Natural Science Foundation of China (NSFC) [11988101, QN2023061004L]en_US
dc.description.sponsorshipWe acknowledge research support from Sabanc & imath; University, and from TUEB & Idot;TAK (The Scientific and Technological Research Council of Turkey) through grant 123F083. EG is supported by National Natural Science Foundation of China (NSFC) programme 11988101 under the foreign talents grant QN2023061004L. DAS:No new data were analysed in support of this paper.en_US
dc.identifier.doi10.1093/mnras/stae1595
dc.identifier.endpage2142en_US
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue2en_US
dc.identifier.scopus2-s2.0-85198706819en_US
dc.identifier.scopusqualityQ1en_US
dc.identifier.startpage2133en_US
dc.identifier.urihttps://doi.org/10.1093/mnras/stae1595
dc.identifier.urihttps://hdl.handle.net/11454/104192
dc.identifier.volume532en_US
dc.identifier.wosWOS:001271725400008en_US
dc.identifier.wosqualityN/Aen_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherOxford Univ Pressen_US
dc.relation.ispartofMonthly Notices of The Royal Astronomical Societyen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.snmz20240831_Uen_US
dc.subjectAccretion, Accretion Discsen_US
dc.subjectStars: Neutronen_US
dc.titleOn the lack of X-ray pulsation in most neutron star low-mass X-ray binariesen_US
dc.typeArticleen_US

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