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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6756
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dc.contributor.authorBeri, Aru-
dc.contributor.authorPaul, Biswajit-
dc.date.accessioned2017-10-04T07:05:30Z-
dc.date.available2017-10-04T07:05:30Z-
dc.date.issued2017-10-
dc.identifier.citationNew Astronomy, 2017, Vol. 56, p94-101en_US
dc.identifier.issn1384-1076-
dc.identifier.urihttp://hdl.handle.net/2289/6756-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractWe report here a pulse profile evolution study of an accreting X-ray pulsar LMC X–4 during and after the large X-ray flares using data from the two observatories XMM-Newton and RXTE. During the flares, the pulse profiles were found to have a significant phase offset in the range of 0.2–0.5 compared to the pulse profiles immediately before or after the flare. Investigating the pulse profiles for about 105 s after the flares, it was found that it takes about 2000–4000 s for the modified accretion column to return to its normal structure and formation of an accretion stream that causes a dip in the pulse profile of LMC X–4. We have also carried out pulse phase resolved spectroscopy of LMC X–4 in narrow phase bins using data from EPIC-pn and spectroscopically confirmed the pulsating nature of the soft spectral component, having a pulse fraction and phase different from that of the power-law component.en_US
dc.language.isoenen_US
dc.publisherElsevier B. V.en_US
dc.relation.urihttp://adsabs.harvard.edu/abs/2017NewA...56...94Ben_US
dc.relation.urihttp://arxiv.org/abs/1705.05205en_US
dc.relation.urihttp://dx.doi.org/10.1016/j.newast.2017.05.001en_US
dc.rights2017 Elesvier B.V.en_US
dc.subjectX-ray neutron starsen_US
dc.subjectpulsarsen_US
dc.subjectKMC X-4en_US
dc.titlePost-flare formation of the accretion stream and a dip in pulse profiles of LMC X-4en_US
dc.typeArticleen_US
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