dc.contributor.author | Paliya, Vaidehi S. | |
dc.contributor.author | Diltz, Chris | |
dc.contributor.author | Böttcher, Markus | |
dc.contributor.author | Stalin, C.S. | |
dc.contributor.author | Buckley, David | |
dc.date.accessioned | 2017-04-13T08:33:22Z | |
dc.date.available | 2017-04-13T08:33:22Z | |
dc.date.issued | 2016 | |
dc.identifier.citation | Paliya, 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.issn | 1538-4357 (Online) | |
dc.identifier.issn | 0004-637X | |
dc.identifier.uri | http://hdl.handle.net/10394/21390 | |
dc.identifier.uri | https://doi.org/10.3847/0004-637X/817/1/61 | |
dc.identifier.uri | http://iopscience.iop.org/article/10.3847/0004-637X/817/1/61/pdf | |
dc.description.abstract | The 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 general | en_US |
dc.language.iso | en | en_US |
dc.publisher | IOP | en_US |
dc.subject | Galaxies: active | en_US |
dc.subject | Galaxies: jets | en_US |
dc.subject | Gamma rays: galaxies | en_US |
dc.subject | Quasars: individual (3C 279) | en_US |
dc.title | A hard gamma-ray flare from 3C 279 in 2013 December | en_US |
dc.type | Article | en_US |
dc.contributor.researchID | 24420530 - Böttcher, Markus | |
dc.contributor.researchID | 24915610 - Diltz, Chris | |