Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8335
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dc.contributor.authorMondal, Santanu-
dc.contributor.authorSalgundi, Anirudh-
dc.contributor.authorChatterjee, Debjit-
dc.contributor.authorJana, Arghajit-
dc.contributor.authorChang, H. K-
dc.contributor.authorNaik, Sachindra-
dc.date.accessioned2024-01-11T05:25:38Z-
dc.date.available2024-01-11T05:25:38Z-
dc.date.issued2023-12-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Vol. 526, No. 3, pp. 4718-4724en_US
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2248/8335-
dc.descriptionOpen Accessen_US
dc.descriptionThis is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.-
dc.description.abstractThe black hole X-ray binary GX 339-4 showed an X-ray outburst during 2021. The AstroSat captured this outburst when the source entered into the intermediate flux state while the count rate was declining. The source showed an alternating flux profile in a time-scale of 100 ks, where the hard energy band was more variable than the soft band. The energy-dependent timing study showed that the observed quasi-periodic oscillation (QPO) was prominent in the low-energy bands, with its nearly sub-harmonic and harmonic components. These components appear and disappear with time, as observed in the orbit-wise QPO study. The Q-value, fractional rms, and 4.8–5.6 Hz frequency infer the QPOs as type-B and the spectral state as soft intermediate. The rms spectra of all orbits exhibiting QPOs show an increase in amplitude till ∼10 keV, beyond which it starts decreasing. This may indicate that ∼10 keV photons contributed relatively more in QPOs than other energy band photons. The Lorentzian normalization of the type-B QPO in different energy bands is consistent with the 10 keV peak. The energy-dependent time lag is complex and could be associated with the Comptonizing corona or jet. Finally, we discuss possible reasons behind the origin of different timing properties observed.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of Royal Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.1093/mnras/stad3079-
dc.rights© 2023 The Author(s)-
dc.subjectAccretion, accretion discsen_US
dc.subjectBlack hole physicsen_US
dc.subjectX-rays: binariesen_US
dc.subjectX-rays: individual: GX 339-4en_US
dc.titleEvolution of low-frequency quasi-periodic oscillations in GX 339-4 during its 2021 outburst using AstroSat dataen_US
dc.typeArticleen_US
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