The spectral evolution of gamma-ray burst pulses

1996 ◽  
Author(s):  
V. E. Kargatis ◽  
E. P. Liang
Keyword(s):  
Gamma Ray ◽  
Spectral Evolution ◽  
Gamma Ray Burst

Spectral Evolution of Swift Gamma-ray Burst Tails: an Update

2010 ◽  
Author(s):  
V. Mangano ◽  
B. Sbarufatti ◽  
Nobuyuki Kawai ◽  
Shigehiro Nagataki
Keyword(s):  
Gamma Ray ◽  
Spectral Evolution ◽  
Gamma Ray Burst

scholarly journals SWIFT OBSERVATIONS OF GAMMA-RAY BURST PULSE SHAPES: GRB PULSE SPECTRAL EVOLUTION CLARIFIED

2015 ◽  
Vol 815 (2) ◽  
pp. 134 ◽  
Author(s):  
Jon Hakkila ◽  
Amy Lien ◽  
Takanori Sakamoto ◽  
David Morris ◽  
James E. Neff ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Spectral Evolution ◽  
Gamma Ray Burst ◽  
Burst Pulse

Physical Model of Gamma-Ray Burst Spectral Evolution

1997 ◽  
Vol 479 (1) ◽  
pp. L35-L38 ◽  
Author(s):  
Edison Liang ◽  
Masaaki Kusunose ◽  
I. A. Smith ◽  
A. Crider
Keyword(s):  
Physical Model ◽  
Gamma Ray ◽  
Spectral Evolution ◽  
Gamma Ray Burst

scholarly journals GRB 190114C: from prompt to afterglow?

2019 ◽  
Vol 626 ◽  
pp. A12 ◽  
Author(s):  
M. E. Ravasio ◽  
G. Oganesyan ◽  
O. S. Salafia ◽  
G. Ghirlanda ◽  
G. Ghisellini ◽  
...  
Keyword(s):  
Energy Range ◽  
Power Law ◽  
Gamma Ray ◽  
Spectral Energy Distribution ◽  
Onset Time ◽  
Lorentz Factor ◽  
Spectral Energy ◽  
Large Area ◽  
Spectral Evolution ◽  
Gamma Ray Burst

GRB 190114C is the first gamma-ray burst detected at very high energies (VHE, i.e., > 300 GeV) by the MAGIC Cherenkov telescope. The analysis of the emission detected by the Fermi satellite at lower energies, in the 10 keV–100 GeV energy range, up to ∼50 s (i.e., before the MAGIC detection) can hold valuable information. We analyze the spectral evolution of the emission of GRB 190114C as detected by the Fermi Gamma-Ray Burst Monitor (GBM) in the 10 keV–40 MeV energy range up to ∼60 s. The first 4 s of the burst feature a typical prompt emission spectrum, which can be fit by a smoothly broken power-law function with typical parameters. Starting on ∼4 s post-trigger, we find an additional nonthermal component that can be fit by a power law. This component rises and decays quickly. The 10 keV–40 MeV flux of the power-law component peaks at ∼6 s; it reaches a value of 1.7 × 10−5 erg cm−2 s−1. The time of the peak coincides with the emission peak detected by the Large Area Telescope (LAT) on board Fermi. The power-law spectral slope that we find in the GBM data is remarkably similar to that of the LAT spectrum, and the GBM+LAT spectral energy distribution seems to be consistent with a single component. This suggests that the LAT emission and the power-law component that we find in the GBM data belong to the same emission component, which we interpret as due to the afterglow of the burst. The onset time allows us to estimate that the initial jet bulk Lorentz factor Γ0 is about 500, depending on the assumed circum-burst density.

Sign in / Sign up

Export Citation Format

Share Document