J/ApJS/224/20 10yr of Swift/XRT obs. of GRBs (Yi+, 2016)
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., Liang E.-W.
<Astrophys. J. Suppl. Ser., 224, 20-20 (2016)>
=2016ApJS..224...20Y 2016ApJS..224...20Y (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; X-ray sources ; Redshifts
Keywords: gamma rays: general; radiation mechanisms: non-thermal
Abstract:
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
Lp∝Tpeak,z-1.27. The flare duration increases with peak
time. The 0.3-10keV isotropic energy of the distribution of X-ray
flares is a log-normal peaked at 1051.2erg. 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.
Description:
In this paper, we analyze the X-ray flare data of Swift/XRT over 10yrs
until the end of 2015 March, and study the distributions of energy,
duration, waiting time, rise time, decay time, peak time, and peak
flux.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 169 468 Fitting results of X-ray flares for 201 GRBs
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See also:
J/ApJ/800/16 : Swift-XRT long GRB durations (Boer+, 2015)
J/A+A/562/A2 : 100-month Swift catalogue of SFXTs (Romano+, 2014)
J/A+A/528/A122 : SwiftFT catalog (Puccetti+, 2011)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB Swift GRB Name (YYMMDDA)
9- 14 F6.4 --- z [0.2/8]? Redshift
16- 23 F8.1 s T-start Flare fitted start time
25- 35 F11.1 s e_T-start Uncertainty in T-start
37- 44 F8.1 s T-peak [59/806460] Flare fitted peak time
46- 57 F12.1 s e_T-peak Uncertainty in T-peak
59- 68 F10.1 s T-end Flare fitted end time
70- 82 F13.1 s e_T-end Uncertainty in T-end
84- 93 F10.6 10-13W/m2 Fp [0/962] Peak Flux, 10-10erg/cm2/s
95-107 F13.6 10-13W/m2 e_Fp [0/222504] Uncertainty in Fp
109-114 F6.2 10-11J/m2 SF [0.04/960] Fluence, 10-8erg/cm2
116-124 F9.2 10-11J/m2 e_SF [0.1/298878] Uncertainty in SF
126-136 F11.6 10+41W Lp [0/1852]? Peak luminosity, 10+48erg/s
138-151 F14.7 10+41W e_Lp [0/170551]? Uncertainty in Lp
153-158 F6.2 10+43J Ex-iso [0.07/985]? Isotropic energy, 10+50erg
160-169 F10.2 10+43J e_Ex-iso ? Uncertainty in Ex-iso
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 11-Jul-2016