Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7885
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dc.contributor.authorPaliya, Vaidehi S-
dc.contributor.authorBöttcher, M-
dc.contributor.authorGurwell, Mark-
dc.contributor.authorStalin, C. S-
dc.date.accessioned2021-12-16T04:05:46Z-
dc.date.available2021-12-16T04:05:46Z-
dc.date.issued2021-12-
dc.identifier.citationThe Astrophysical Journal Supplement Series, Vol. 257, No. 2, 37en_US
dc.identifier.issn0067-0049-
dc.identifier.urihttp://hdl.handle.net/2248/7885-
dc.descriptionRestricted Accessen_US
dc.description.abstractThe origin of γ-ray flares observed from blazars is one of the major mysteries in jet physics. We have attempted to address this problem following a novel spectral energy distribution (SED) fitting technique that explored the flaring patterns identified in the broadband SEDs of two γ-ray bright blazars, 3C 279 (z = 0.54) and 3C 454.3 (z = 0.86), using near-simultaneous radio-to-γ-ray observations. For both sources, the γ-ray flux strongly correlates with the separation of the SED peaks and the Compton dominance. We propose that spectral hardening of the radiating electron population and/or enhancement of the Doppler factor can naturally explain these observations. In both cases, magnetic reconnection may play a pivotal role in powering the luminous γ-ray flares.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.3847/1538-4365/ac365d-
dc.rights© American Astronomical Society-
dc.subjectRelativistic jetsen_US
dc.subjectBlazarsen_US
dc.subjectGamma ray astronomyen_US
dc.subjectRadiative processesen_US
dc.titleOn the Origin of Gamma-Ray Flares from Bright Fermi Blazarsen_US
dc.typeArticleen_US
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