| Abstract : | Long GRB 190114C, identified on January 14th, 2019, was the first Gamma-ray Burst that substantially violated the defined 10 GeV energy limit of the Synchrotron model, with an observed emission between 0.2 to 1 TeV and a low redshift of z = 0.425. This research analyzes the immediate afterglow broadband spectrum from 1017 to 1026 Hz based on observations by the Swift X-ray Telescope (XRT), Fermi Gamma-Ray Burst Monitor (GBM), Swift Burst Alert Telescope (BAT), Fermi Large Area Telescope (LAT), and Major Atmospheric Gamma Imaging Cherenkov Telescope (MAGIC). We first calculate the physical characteristics necessary to understand the conditions in the emitting region of the burst, and then conduct temporal and spectral analyses by deriving the light curves and spectra using a chain polynomial best-fit in the context of the forward shock model. We find that the Bulk Lorentz Factor = 351 sufficiently explains the peak of the inverse Compton component at sub-TeV energy levels in the immediate afterglow, and that the Comptonization of the burst proceeds in the Klein-Nishina regime. The Spectral Energy Distributions are found to be double-peaked for ? + 68-180s, and we show that the distribution consists of a distinct Synchrotron component followed by an inverse Compton component explained by high-energy electrons up-scattering Synchrotron photons. We conclude that this further evidences Synchrotron self-Compton emission as the mechanism behind the production of Very-High-Energy photons in GRB 190114C. |
