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dc.contributor.authorPaliya, Vaidehi S.
dc.contributor.authorDiltz, Chris
dc.contributor.authorBöttcher, Markus
dc.contributor.authorStalin, C.S.
dc.contributor.authorBuckley, David
dc.date.accessioned2017-04-13T08:33:22Z
dc.date.available2017-04-13T08:33:22Z
dc.date.issued2016
dc.identifier.citationPaliya, V.S. et al. 2016. A hard gamma-ray flare from 3C 279 in 2013 December. Astrophysical journal, 817(1): Article no 61. [https://doi.org/10.3847/0004-637X/817/1/61]en_US
dc.identifier.issn1538-4357 (Online)
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/10394/21390
dc.identifier.urihttps://doi.org/10.3847/0004-637X/817/1/61
dc.identifier.urihttp://iopscience.iop.org/article/10.3847/0004-637X/817/1/61/pdf
dc.description.abstractThe blazar 3C 279 exhibited twin γ-ray flares of similar intensity in 2013 December and 2014 April. In this work, we present a detailed multi-wavelength analysis of the 2013 December flaring event. Multi-frequency observations reveal the uncorrelated variability patterns with X-ray and optical–UV fluxes peaking after the γ-ray maximum. The broadband spectral energy distribution (SED) at the peak of the γ-ray activity shows a rising γ-ray spectrum but a declining optical–UV flux. This observation along with the detection of uncorrelated variability behavior rules out the one-zone leptonic emission scenario. We, therefore, adopt two independent methodologies to explain the SED: a time-dependent lepto-hadronic modeling and a two-zone leptonic radiative modeling approach. In the lepto-hadronic modeling, a distribution of electrons and protons subjected to a randomly orientated magnetic field produces synchrotron radiation. Electron synchrotron is used to explain the IR to UV emission while proton synchrotron emission is used to explain the high-energy γ-ray emission. A combination of both electron synchrotron self-Compton emission and proton synchrotron emission is used to explain the X-ray spectral break seen during the later stage of the flare. In the two-zone modeling, we assume a large emission region emitting primarily in IR to X-rays and γ-rays to come primarily from a fast-moving compact emission region. We conclude by noting that within a span of four months, 3C 279 has shown the dominance of a variety of radiative processes over each other and this reflects the complexity involved in understanding the physical properties of blazar jets in generalen_US
dc.language.isoenen_US
dc.publisherIOPen_US
dc.subjectGalaxies: activeen_US
dc.subjectGalaxies: jetsen_US
dc.subjectGamma rays: galaxiesen_US
dc.subjectQuasars: individual (3C 279)en_US
dc.titleA hard gamma-ray flare from 3C 279 in 2013 Decemberen_US
dc.typeArticleen_US
dc.contributor.researchID24420530 - Böttcher, Markus
dc.contributor.researchID24915610 - Diltz, Chris


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