2011A&A...526A..27B


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.16CET23:39:23

2011A&A...526A..27B - Astronomy and Astrophysics, volume 526A, 27-27 (2011/2-1)

Gamma-ray burst long lasting X-ray flaring activity.

BERNARDINI M.G., MARGUTTI R., CHINCARINI G., GUIDORZI C. and MAO J.

Abstract (from CDS):

One of the most intriguing features revealed by the Swift satellite are flares that are superimposed on the gamma-ray burst (GRB) X-ray light curves. The vast majority of flares occurs before 1000 s, but some of them can be found up to 106s after the main event. We shed light on late-time (i.e. with peak time tpk >1000s) flaring activity. We address the morphology and energetic of flares in the window ∼ 103-106s to put constraints on the temporal evolution of the flare properties and to identify possible differences in the mechanism producing the early and late-time flaring emission, if any. This requires the complete understanding of the observational biases affecting the detection of X-ray flares superimposed on a fading continuum at t>1000s. We consider all Swift GRBs that exhibit late-time flares. Our sample consists of 36 flares, 14 with redshift measurements. We inherit the strategy of data analysis from Chincarini et al. (2010) in order to make a direct comparison with the early-time flare properties. The morphology of the flare light curve is the same for both early-time and late-time flares, but they differ energetically. The width of late-time flares increases with time similarly to the early-time flares. Simulations confirmed that the increase of the width with time is not owing to the decaying statistics, at least up to 104s. The energy output of late-time flares is one order of magnitude lower than the early-time flare one,and is ∼1% Eprompt. The evolution of the peak luminosity as well as the distribution of the peak-flux-to-continuum ratio for late-time flares indicate that the flaring emission is decoupled from the underlying continuum, differently from early-time flares/steep decay. A sizable fraction of late-time flares are compatible with afterglow variability. The internal shock origin seems the most promising explanation for flares. However, some differences that emerge between late- and early-time flares suggest that there could be no unique explanation about the nature of late-time flares.

Abstract Copyright:

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

Simbad objects: 23

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Number of rows : 23

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 GRB 071031 gB 00 25 37.40 -58 03 33.9           ~ 138 0
2 GRB 071112C gB 02 36 50.89 +28 22 16.9           ~ 124 0
3 GRB 060906 gB 02 43 00.900 +30 21 42.12     19.84     ~ 113 0
4 GRB 060312 gB 03 03 05.920 +12 50 02.00           ~ 41 0
5 GRB 070318 gB 03 13 56.830 -42 56 46.30 18.27 16.23 15.49     ~ 137 0
6 GRB 060223A gB 03 40 49.560 -17 07 48.40     17.90     ~ 74 0
7 GRB 050916 gB 09 03 57.270 -51 25 42.51           ~ 38 0
8 GRB 050502B gB 09 30 10.024 +16 59 48.07           ~ 146 0
9 GRB 070107 gB 10 37 36.350 -53 12 47.51 18.37 18.49 17.44     ~ 41 0
10 GRB 050416 gB 12 33 54.600 +21 03 26.69     19.12     ~ 246 1
11 GRB 091130B gB 13 32 35.62 +34 05 18.8           ~ 28 0
12 GRB 080319A gB 13 45 19.97 +44 04 49.1           ~ 65 0
13 GRB 090417B gB 13 58 44.8 +47 00 55           ~ 94 1
14 GRB 051117A gB 15 13 34.020 +30 52 12.30 18.66 19.81       ~ 60 0
15 GRB 050724 gB 16 24 44.400 -27 32 27.90     19.70     ~ 368 1
16 GRB 090807 gB 18 14 57.80 +10 16 45.9           ~ 28 0
17 GRB 090422 gB 19 38 59.92 +40 23 04.0           ~ 35 0
18 GRB 060105 gB 19 50 00.680 +46 20 55.40           ~ 76 0
19 GRB 070429A gB 19 50 48.900 -32 24 17.01           ~ 34 0
20 GRB 090809 gB 21 54 43.2 -00 05 02           ~ 59 0
21 GRB 081102 gB 22 04 42.60 +52 59 27.7           ~ 46 0
22 GRB 071021 gB 22 42 34.34 +23 43 05.4           ~ 77 0
23 GRB 050803 gB 23 22 37.910 +05 47 09.00           ~ 99 0

    Equat.    Gal    SGal    Ecl

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2019.11.16-23:39:23

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