2022ApJ...933...18G

Query : 2022ApJ...933...18G

2022ApJ...933...18G - Astrophys. J., 933, 18-18 (2022/July-1)

GRB Prompt Emission with Anisotropic Electron Distribution.

GOTO R. and ASANO K.

Abstract (from CDS):

The typical spectrum of the prompt emission of gamma-ray bursts (GRBs) indicates that the electron cooling is suppressed in spite of the strong magnetic field in the standard synchrotron model. Recent particle-in-cell simulations show that the particle acceleration by magnetic reconnection in a magnetically dominated plasma can lead to small pitch angles especially in a low-energy region. Such a small pitch angle prevents electrons from cooling via synchrotron radiation. In this paper, taking into account the effects of the synchrotron cooling and the adiabatic cooling, we numerically calculate the synchrotron spectra with anisotropic electron distributions. If we require a Poynting flux larger than 1050 erg s–1 as the model is motivated by magnetic reconnection, the bulk Lorentz factor of ∼1000 and the electron minimum Lorentz factor of γmin ∼ 104 are required to reproduce the typical GRB spectrum.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Gamma-ray bursts

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 GRB 121024A gB 04 41 53.31 -12 17 26.1           ~ 143 0

Query : 2022ApJ...933...18G

Basic data :
GRB 121024A -- Gamma-ray Burst
Other object types: otypes_help 		gB (GRB)
ICRS coord. (ep=J2000) : 		04 41 53.31 -12 17 26.1 (X-ray) [ 1500 1500 0 ] D SWIFT
FK4 coord. (ep=B1950 eq=1950) : 		04 39 33.32 -12 23 06.0 [ 1500 1500 0 ]
Gal coord. (ep=J2000) : 		209.51986 -34.25332 [ 1500 1500 0 ]
Radial velocity / Redshift / cz : 		V(km/s) 249309 [~] / z(spectroscopic) 2.2980 [~] / cz 688923 [~]
   (Opt) C 2019ApJ...884...66G
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Identifiers (1) :
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GRB 121024A

References (143 between 1850 and 2026) (Total 143)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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