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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8203
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dc.contributor.authorBeri, Aru-
dc.contributor.authorSharma, Rahul-
dc.contributor.authorRoy, Pinaki-
dc.contributor.authorGaur, Vishal-
dc.contributor.authorAltamirano, Diego-
dc.contributor.authorAndersson, Nils-
dc.contributor.authorGittins, Fabian-
dc.contributor.authorCelora, T.-
dc.date.accessioned2024-01-30T05:54:55Z-
dc.date.available2024-01-30T05:54:55Z-
dc.date.issued2023-03-24-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society,2023,Vol.521, p5904en_US
dc.identifier.issn0035-8711 (print)-
dc.identifier.issn1365-2966 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/8203-
dc.descriptionOpen Accessen_US
dc.description.abstractWe report results from a study of XTE J1739 −285, a transient neutron star low mass X-ray binary observed with AstroSat and NuSTAR during its 2019–2020 outburst. We detected accretion-powered X-ray pulsations at 386 Hz during very short intervals (0.5–1 s) of X-ray flares. These flares were observed during the 2019 observation of XTE J1739 −285. During this observation, we also observed a correlation between intensity and hardness ratios, suggesting an increase in hardness with the increase in intensity. Moreo v er, a thermonuclear X-ray burst detected in our AstroSat observation during the 2020 outburst revealed the presence of coherent burst oscillations at 383 Hz during its decay phase. The frequency drift of 3 Hz during X-ray burst can be explained with r modes. Thus, making XTE J1739 −285 belong to a subset of NS-LMXBs which exhibit both nuclear- and accretion-po wered pulsations. The po wer density spectrum created using the AstroSat - LAXPC observations in 2020 showed the presence of a quasi-periodic oscillation at ∼0.83 Hz. Our X-ray spectroscopy revealed significant changes in the spectra during the 2019 and 2020 outburst. We found a broad iron line emission feature in the X-ray spectrum during the 2020 observation, while this feature was relatively narrow and has a lower equivalent width in 2019, when the source was accreting at higher rates than 2020. Hard X-ray tail was observed during the 2019 observations, indicating the presence of non-thermal component in the X-ray spectra.en_US
dc.language.isoenen_US
dc.publisherRoyal Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2023MNRAS.521.5904B/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2303.13085en_US
dc.relation.urihttps://doi.org/10.1093/mnras/stad902en_US
dc.rights2023, The Author(s)en_US
dc.subjectAccretion,en_US
dc.subjectAccretion discs –stars:en_US
dc.subjectNeutron –X-ray:en_US
dc.subjectBinaries –X-rays:en_US
dc.subjectBursts –X-rays:en_US
dc.subjectIndividual (XTE J1739 −285)en_US
dc.titleAstroSat and NuSTAR obser v ations of XTE J1739 −285 during the 2019–2020 outbursten_US
dc.typeArticleen_US
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