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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8669
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dc.contributor.authorBalu, Ajith-
dc.contributor.authorRoy, Kinjal-
dc.contributor.authorManikantan, Hemanth-
dc.contributor.authorTamang, Abhisek-
dc.contributor.authorPaul, Biswajit-
dc.date.accessioned2026-02-19T08:49:05Z-
dc.date.available2026-02-19T08:49:05Z-
dc.date.issued2024-12-02-
dc.identifier.citationAstronomy & Astrophysics, 2024, Vol. 692 (12), AR No. A47en_US
dc.identifier.issn1432-0746-
dc.identifier.urihttp://hdl.handle.net/2289/8669-
dc.descriptionOpen Access. Also available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractContext. Centaurus X-3 is a persistent high-mass X-ray binary with the long-term light curve from the source exhibiting orbit-to-orbit intensity variations with no apparent superorbital periodicity. Aims. We used ∼13.5 years of MAXI/GSC data to study the long-term behaviour of X-ray absorption caused by the stellar wind from the companion star and any absorbing structures present in the binary. Methods. We used orbital-phase-resolved spectroscopy to study the variation in the photoelectric absorption along the line of sight of the source for both the intensity-averaged data and intensity-resolved data after dividing all the data binned with orbital period into three intensity levels. Results. We find an asymmetric variation in the photoelectric absorption along the line of sight across an orbit of the source. The orbital-phase-resolved spectra show a clear increase in photoelectric absorption after ϕorb ∼ 0.5, which deviates from a spherically symmetric stellar wind model. The flux of Cen X-3 shows significant variation between consecutive orbits. An intensity-resolved spectral analysis of the source was performed, followed by an intensity-resolved and orbital-phase-resolved spectral analysis, which showed that at the medium and high intensity levels, the orbital-phase-resolved photoelectric absorption is slightly asymmetric with respect to mid-phase (ϕorb = 0.5). The asymmetry is very pronounced at the lowest intensity level and cannot be explained by a spherically symmetric wind from the companion star. Conclusions. The differences in the orbital phase-dependence of absorption for different intensity levels suggest that the presence of an accretion wake, photoionization wake, or tidal stream is more prominent at a lower intensity level for Centaurus X-3 than at a higher intensity level.en_US
dc.language.isoenen_US
dc.publisherAstronomy & Astrophysicsen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2024A&A...692A..47Ben_US
dc.relation.urihttps://doi.org/10.48550/arXiv.2410.17695en_US
dc.relation.urihttps://doi.org/10.1051/0004-6361/202451922en_US
dc.rights2024 The Authorsen_US
dc.subjectstars: mass-lossen_US
dc.subjectstars: neutronen_US
dc.subjectstars: windsen_US
dc.subjectoutflowsen_US
dc.subjectX-rays: binariesen_US
dc.subjectX-rays: individuals: Centaurus X-3en_US
dc.titleStudying the X-ray absorption characteristics of Centaurus X-3 using nearly 14 years of MAXI/GSC dataen_US
dc.typeArticleen_US
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