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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6875
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dc.contributor.authorBeri, Aru-
dc.contributor.authorPaul, Biswajit-
dc.contributor.authorDewangan, Gulab C-
dc.date.accessioned2018-05-02T19:05:08Z-
dc.date.available2018-05-02T19:05:08Z-
dc.date.issued2018-03-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2018, Vol. 475, p999-1009en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 - (online)-
dc.identifier.urihttp://hdl.handle.net/2289/6875-
dc.descriptionOpen Accessen_US
dc.description.abstractWe report results from an observation with the XMM–Newton observatory of a unique X-ray pulsar 4U 1626−67. European Photon Imaging Camera-pn data during the current spin-up phase of 4U 1626−67 have been used to study pulse phase dependence of low-energy emission lines. We found strong variability of low-energy emission line at 0.915 keV with the pulse phase, varying by a factor of 2, much stronger than the continuum variability. Another interesting observation is that behaviour of one of the low-energy emission lines across the pulse phase is quite different from that observed during the spin-down phase. This indicates that the structures in the accretion disc that produce pulse phase dependence of emission features have changed from spin-down to spin-up phase. This is well supported by the differences in the timing characteristics (like pulse profiles, quasi periodic oscillations, etc.) between spin-down and spin-up phases. We have also found that during the current spin-up phase of 4U 1626−67, the X-ray pulse profile below 2 keV is different compared to the spin-down phase. The X-ray light curve also shows flares which produce a feature around 3 mHz in power density spectrum of 4U 1626−67. Since flares are dominant at lower energies, the feature around 3 mHz is prominent at low energies.en_US
dc.language.isoenen_US
dc.publisherOxford University Press for The Royal Astronomical Societyen_US
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1711.11305en_US
dc.relation.urihttp://arxiv.org/abs/1711.11305en_US
dc.relation.urihttp://dx.doi.org/10.1093/mnras/stx3121en_US
dc.rights2018 The authors & the Royal Astronomical Society.en_US
dc.subjectpulsarsen_US
dc.titleChanges in the pulse phase dependence of X-ray emission lines in 4U 1626-67 with a torque reversal.en_US
dc.typeArticleen_US
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