SIMBAD references

2016ApJS..224...20Y - Astrophys. J., Suppl. Ser., 224, 20-20 (2016/June-0)

Comprehensive study of the X-ray flares from gamma-ray bursts observed by Swift.

YI S.-X., XI S.-Q., YU H., WANG F.Y., MU H.-J., LU L.-Z. and LIANG E.-W.

Abstract (from CDS):

X-ray flares are generally supposed to be produced by later activities of the central engine, and may share a similar physical origin with the prompt emission of gamma-ray bursts (GRBs). In this paper, we have analyzed all significant X-ray flares from the GRBs observed by Swift from 2005 April to 2015 March. The catalog contains 468 bright X-ray flares, including 200 flares with redshifts. We obtain the fitting results of X-ray flares, such as start time, peak time, duration, peak flux, fluence, peak luminosity, and mean luminosity. The peak luminosity decreases with peak time, following a power-law behavior L_{p}∝{T}_peak,z^{-1.27} . The flare duration increases with peak time. The 0.3-10 keV isotropic energy of the distribution of X-ray flares is a log-normal peaked at {10}^{51.2} erg. We also study the frequency distributions of flare parameters, including energies, durations, peak fluxes, rise times, decay times, and waiting times. Power-law distributions of energies, durations, peak fluxes, and waiting times are found in GRB X-ray flares and solar flares. These distributions could be well explained by a fractal-diffusive, self-organized criticality model. Some theoretical models based on magnetic reconnection have been proposed to explain X-ray flares. Our result shows that the relativistic jets of GRBs may be dominated by Poynting flux.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): gamma rays: general - radiation mechanisms: non-thermal

VizieR on-line data: <Available at CDS (J/ApJS/224/20): table1.dat>

Simbad objects: 204

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2016ApJS..224...20Y and select 'bookmark this link' or equivalent in the popup menu


2020.11.29-00:32:46

© Université de Strasbourg/CNRS

    • Contact