2020/01/23 by D. Zargaryan, Zargaryan, Davit, C. Romoli +3
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Solar and Space Plasma Dynamics
paper · pdf · doi:10.48550/arxiv.2001.08843
openalex publication_date 2020/01/23 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present results of spectrometric studies based on the observations of very\nstrong 3C 279 flares in high and very-high-energy bands and discuss their\nimplications regarding the origin of radiation mechanisms. The FSRQ 3C 279\n(z=0.536) is one of the most luminous gamma-ray emitting AGN. It shows\nvariability on time scales down to minutes during strong flares detected by the\nFermi-LAT. We have analyzed LAT and Swift-XRT data for the flaring periods in\nJune 2015 and January 2018, when the flux above 100 MeV during hourly time\nintervals could exceed 3 \× 10-5 ph cm-2 s-1. The X-ray flux\nderived from Swift X-ray observations described by a very hard spectrum with\nphoton index ~1.5 is typically explained by Inverse Compton scattering of low\nenergy electrons and protons. Here we consider an alternative interpretation\nwhich describes the entire band from X-ray to very high energy as a results of\nsynchrotron emission by ultra relativistic electrons or protons.\n