scholarly journals Detailed study of the GRB 190114C spectral lags in the energy range of 5 keV – 2 MeV

2021 ◽  
Vol 2103 (1) ◽  
pp. 012005
Author(s):  
V A Dranevich ◽  
P B Dmitriev
Keyword(s):  
Energy Range ◽  
Measurement Errors ◽  
Arrival Time ◽  
Gamma Ray ◽  
Recording Device ◽  
Gamma Ray Burst ◽  
Physical Conditions ◽  
Radiation Generation ◽  
The Difference ◽  
Energy Channels

Abstract The spectral lags of gamma ray bursts are defined as the difference in the registration time of the same radiation pulse in different energy channels of the recording device. This parameter can characterize both the mechanism of radiation generation by the source and the physical conditions of radiation propagation from the source to the observer. In this paper, the dependence of the arrival time of photons on their energy for the gamma ray burst GRB 190114C is obtained from the data of the Gamma ray Burst Monitor (NaI detectors) of the Fermi Gamma ray Space Telescope. It is shown that this dependence is mainly due to the back edges of the light curve pulses. The spectral lags of the leading edges of the pulses are small and comparable in magnitude to the measurement errors. The observed anomaly in the energy range from 5 to 20 keV is probably related to the quasi-thermal radiation of the source.

Gamma‐Ray Burst Arrival Time Localizations: Simultaneous Observations by Pioneer Venus Orbiter , Compton Gamma ‐ Ray Observatory , and Ulysses

1998 ◽  
Vol 118 (2) ◽  
pp. 391-399 ◽  
Author(s):  
J. G. Laros ◽  
K. C. Hurley ◽  
E. E. Fenimore ◽  
R. W. Klebesadel ◽  
M. S. Briggs ◽  
...  
Keyword(s):  
Arrival Time ◽  
Gamma Ray ◽  
Gamma Ray Burst

scholarly journals Importance of the High Energy Channel for the Gamma-Ray Burst Data

1998 ◽  
Vol 188 ◽  
pp. 461-462
Author(s):  
A. Mészáros ◽  
Z. Bagoly ◽  
L. G. Balázs ◽  
I. Horváth ◽  
P. Mészáros
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Statistical Information ◽  
Initial Number ◽  
Data Bases ◽  
Energy Channel ◽  
Gamma Ray Burst ◽  
Peak Flux ◽  
Burst Data ◽  
Energy Channels

Extensive data bases on Gamma-Ray Burst (GRB) properties such as the BATSE 3B catalog (Meegan et al. 1996) contain a wealth of statistical information. The nine entries of the 3B database for each GRB consist of two durations, T50, T90, which contain 50% and 90% of the burst energy, respectively; four fluences (time-integrated energy fluxes) F1, F2, F3, F4, defined over different energy channels; and three measures of the peak flux (each summed over the four energy channels), measured over three different resolution timescales (64 ms, 256 ms and 1024 ms). Thus the initial number of variables is n = 9. There is, of course, some incompleteness in the catalog. There are 625 GRBs having all 9 non-zero quantities, and only they are considered here.

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.

scholarly journals A Detailed Study on the Equal Arrival Time Surface Effect in Gamma-Ray Burst Afterglows

2007 ◽  
Vol 7 (3) ◽  
pp. 397-404 ◽  
Author(s):  
Yong-Feng Huang ◽  
Ye Lu ◽  
Anna Yuen Lam Wong ◽  
Kwong Sang Cheng
Keyword(s):  
Arrival Time ◽  
Gamma Ray ◽  
Surface Effect ◽  
Gamma Ray Burst

scholarly journals Gamma‐Ray Burst Arrival‐Time Localizations: Simultaneous Observations byUlysses,Pioneer Venus Orbiter, SIGMA, WATCH, and PHEBUS

2000 ◽  
Vol 533 (2) ◽  
pp. 884-889 ◽  
Author(s):  
K. Hurley ◽  
J. Laros ◽  
S. Brandt ◽  
E. E. Fenimore ◽  
R. W. Klebesadel ◽  
...  
Keyword(s):  
Arrival Time ◽  
Gamma Ray ◽  
Gamma Ray Burst

scholarly journals Linear line spectropolarimetry as a new window to measure 2D and 3D wind geometries

2014 ◽  
Vol 9 (S307) ◽  
pp. 359-364
Author(s):  
Jorick S. Vink
Keyword(s):  
Angular Momentum ◽  
Mass Loss ◽  
Rotation Rate ◽  
Gamma Ray ◽  
Stellar Rotation ◽  
Gamma Ray Burst ◽  
Latitudinal Dependence ◽  
The Difference ◽  
2D And 3D

AbstractVarious theories have been proposed to predict how mass loss depends on the stellar rotation rate, both in terms of its strength, as well as its latitudinal dependence, crucial for our understanding of angular momentum evolution. Here we discuss the tool of linear spectropolarimetry that can probe the difference between mass loss from the pole versus the equator. Our results involve several groups of O stars and Wolf-Rayet stars, involving Oe stars, Of?p stars, Onfp stars, as well as the best candidate gamma-ray burst progenitors identified to date.

Surface of equal arrival time and gamma-ray burst afterglow

2000 ◽  
Vol 24 (1) ◽  
pp. 30-35 ◽  
Author(s):  
Zhou Li ◽  
Zi-gao Dai ◽  
Tan Lu
Keyword(s):  
Arrival Time ◽  
Gamma Ray ◽  
Gamma Ray Burst
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