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dc.contributor.authorPradhan, Pragati-
dc.contributor.authorBozzo, E.-
dc.contributor.authorPaul, Biswajit-
dc.contributor.author+2 Co-Authors-
dc.date.accessioned2019-10-16T08:42:54Z-
dc.date.available2019-10-16T08:42:54Z-
dc.date.issued2019-10-01-
dc.identifier.citationThe Astrophysical Journal, 2019, Vol.883, p116en_US
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7319-
dc.descriptionOpen Accessen_US
dc.description.abstractSupergiant X-ray binaries usually comprise a neutron star accreting from the wind of an OB supergiant companion. They are classified as classical systems and supergiant fast X-ray transients (SFXTs). The different behavior of these subclasses of sources in X-rays, with SFXTs displaying much more pronounced variability, is usually (at least) partly ascribed to different physical properties of the massive star clumpy stellar wind. In the case of SFXTs, a systematic investigation of the effects of clumps on flares/outbursts of these sources has been reported by Bozzo et al. exploiting the capabilities of the instruments on board XMM-Newton to perform a hardness-resolved spectral analysis on timescales as short as a few hundreds of seconds. In this paper, we use six XMM-Newton observations of IGR J18027-2016 to extend the above study to a classical supergiant X-ray binary and compare the findings with those derived in the case of SFXTs. As these observations of IGR J18027-2016 span different orbital phases, we also study its X-ray spectral variability on longer timescales and compare our results with previous publications. Although obtaining measurements of the clump physical properties from X-ray observations of accreting supergiant X-ray binaries has already proven to be challenging, our study shows that similar imprints of clumps are found in the X-ray observations of the SFXTs and at least one classical system, i.e., IGR J18027-2016. This provides interesting perspectives to further extend this study to many XMM-Newton observations already performed in the direction of other classical supergiant X-ray binaries.en_US
dc.language.isoenen_US
dc.publisherIOP Sciences for The American Astronomical Societyen_US
dc.relation.urihttps://arxiv.org/abs/1908.03582en_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/ab3a40en_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2019ApJ...883..116P/abstracten_US
dc.rights2019, The American Astronomical Societyen_US
dc.subjectpulsars: individual: IGR J18027-2016en_US
dc.subjectX-rays: binariesen_US
dc.subjectAstrophysics - High Energy Astrophysical Phenomenaen_US
dc.titleProbing Clumpy Wind Accretion in IGR J18027-2016 with XMM-Newtonen_US
dc.typeArticleen_US
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