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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6634
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dc.contributor.authorAftab, Nafisa-
dc.contributor.authorIslam, Nazma-
dc.contributor.authorPaul, Biswajit-
dc.date.accessioned2017-03-13T13:45:47Z-
dc.date.available2017-03-13T13:45:47Z-
dc.date.issued2016-12-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2016, Vol. 463, p2032-2038en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 - (online)-
dc.identifier.urihttp://hdl.handle.net/2289/6634-
dc.descriptionOpen Accessen_US
dc.description.abstractWe report the results from pulsations and spectral analysis of a large number of observations of the high-mass X-ray binary pulsar IGR J18027−2016 with Swift X-ray Telescope (XRT), carried out at different orbital phases. In some orbital phases, as seen in different XRT observations, the X-ray intensity is found to vary by a large factor, of about ∼50. In all the observations with sufficient number of source X-ray photons, pulsations have been detected around the previously known pulse period of ∼140 s. When detected, the pulse profiles do not show any significant variation over a flux difference of a factor of ∼3. The absorption column density is found to be large before and after the eclipse. We discuss various possible reasons for intensity and spectral variations in IGR J18027−2016, such as clumpy wind and hydrodynamic instabilities.en_US
dc.language.isoenen_US
dc.publisherOxford University Press for The Royal Astronomical Societyen_US
dc.relation.urihttp://adsabs.harvard.edu/abs/2016MNRAS.463.2032Aen_US
dc.relation.urihttp://arxiv.org/abs/1608.06297en_US
dc.relation.urihttp://dx.doi.org/10.1093/mnras/stw2037en_US
dc.rights2016 The authors & the Royal Astronomical Societyen_US
dc.titleVariability study of the High Mass X-ray binary IGR J18027-2016 with Swift-XRT.en_US
dc.typeArticleen_US
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