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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8202
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dc.contributor.authorDas, Avik Kumar-
dc.contributor.authorMondal, Sandeep Kumar-
dc.contributor.authorPrince, Raj-
dc.date.accessioned2024-01-30T05:52:59Z-
dc.date.available2024-01-30T05:52:59Z-
dc.date.issued2023-03-07-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society,2023,Vol.521, p3451en_US
dc.identifier.issn0035-8711 (print)-
dc.identifier.issn1365-2966 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/8202-
dc.descriptionOpen Accessen_US
dc.description.abstractWe study the long-term behaviour of the bright gamma-ray blazar PKS 0402-362. We collected approximately 13 yr of Fermi- LAT data between August 2008 to January 2021 and identified three bright γ-ray activity epochs. The second was found to be the brightest epoch ever seen in this source. We observed most of the γ-ray flare peaks to be asymmetric in profile suggesting a slow cooling time of particles or the varying Doppler factor as the main cause of these flares. The γ-ray spectrum is fitted with PL and LP spectral models, and in both cases, the spectral index is very steep. The γ-ray spectrum does not extend beyond 10 GeV energy suggesting the emission is produced within the BLR. The absence of time lags between optical-IR and γ-ray suggest one zone emission model. Using the abo v e information, we hav e modelled the broad-band SED with a simple one-zone emission model using the publicly available code ‘GAMERA’. The particle distribution index is found to be the same as expected in dif fusi ve shock acceleration suggesting it as the main mechanism of particle acceleration to very high energy up to 4–6 GeV. Throughout the various flux phases, we noticed that the optical emission is dominated by the thermal disc, suggesting it to be a good source to examine the disc-jet coupling. We postulate that the observed broad-band flares could be linked with perturbation produced in the disc, which propagates to the jet and interacts with the standing shock. Ho we ver, a more detailed examination is requireden_US
dc.language.isoenen_US
dc.publisherRoyal Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2023MNRAS.521.3451D/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2303.03039en_US
dc.relation.urihttps://doi.org/10.1093/mnras/stad702en_US
dc.rights2023, The Author(s)en_US
dc.subjectGalaxiesen_US
dc.subjectActi ve-galaxiesen_US
dc.subjectIndividualen_US
dc.subjectPKS 0402-362en_US
dc.subjectGamma raysen_US
dc.subjectGalaxiesen_US
dc.titleGamma-ray flares and broadband spectral study of PKS 0402-362en_US
dc.typeArticleen_US
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