2006MNRAS.368.1351P


Query : 2006MNRAS.368.1351P

2006MNRAS.368.1351P - Mon. Not. R. Astron. Soc., 368, 1351-1358 (2006/May-3)

A test of the power-law relationship between gamma-ray burst pulse-width ratio and energy expected in fireballs and uniform jets.

PENG Z.-Y., QIN Y.-P., ZHANG B.-B., LU R.-J., JIA L.-W. and ZHANG Z.-B.

Abstract (from CDS):

A power-law relationship between the pulse width and energy of gamma-ray bursts (GRBs) has been found by many authors. Recently, under the assumption that the Doppler effect of the relativistically expanding fireball surface (or, in some papers, the curvature effect) is important, Qin et al. showed that, in most cases, this power-law relationship would exist in a certain energy range, and, within a similar range, a power-law relationship of an opposite trend between the ratio of the rising width to the decaying width and energy would be expected for the same burst. We check this prediction with two GRB samples that contain well-identified pulses. A power-law anticorrelation between the full pulse width and energy and a power-law correlation between the pulse-width ratio and energy are seen in the light curves of the majority (around 65 per cent) of bursts of the two samples within the energy range of BATSE, suggesting that these bursts probably arise from the emission associated with the shocks occurring on a relativistically expanding fireball surface. For the rest of the bursts, the relationships between these quantities had not been predicted previously. We propose considering other spectral evolutionary patterns or other radiation mechanisms such as a varying synchrotron or Comptonized spectrum to check whether the observed relationships for these bursts can also be accounted for by the Doppler model. In addition, we find that the upper limits of the width ratio for the two samples do not exceed 0.9, in agreement with what has previously been predicted by the Doppler model. The plateau/power law/plateau and the peaked features predicted and detected previously by Qin et al. are generally observed, with exceptions noticed only in a few cases. According to the distinct values of two power-law indices, αFWHMand αratio, we divide the bursts into three subsets that are located in different areas of the αFWHM-αratioplane. We suspect that different locations of (αFWHM, αratio) might correspond to different mechanisms.

Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS

Journal keyword(s): relativity - gamma-rays: bursts - gamma-rays: theory

Simbad objects: 22

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Number of rows : 22
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 4B 951016 gB 02 23.3 -24 22           ~ 25 0
2 1B 910826 gB 04 36.5 +48 31           ~ 14 0
3 4B 960624 gB 06 35.8 +32 03           ~ 16 0
4 3B 930612 gB 06 52.3 -69 46           ~ 48 0
5 3B 940313 gB 07 17.8 -14 28           ~ 18 0
6 1B 911022 gB 08 15.6 +70 20           ~ 29 0
7 3B 931128 gB 09 30.6 +18 13           ~ 27 0
8 1B 920216 gB 10 27.7 +01 10           ~ 35 0
9 4B 951019 gB 10 46.0 -87 49           ~ 22 0
10 4B 951102B gB 12 38.6 -35 14           ~ 15 0
11 2B 930214B gB 12 59.2 +26 46           ~ 32 0
12 4B 941026 gB 13 43.8 -06 32           ~ 37 0
13 GRB 940529C gB 14 19.4 +58 56           ~ 34 0
14 4B 960114 gB 14 24.8 -29 44           ~ 23 0
15 GRB 971127 gB 15 32 +32.2           ~ 24 0
16 3B 940904 gB 16 13.5 +44 05           ~ 12 0
17 2B 920830 gB 17 14.1 -73 59           ~ 38 0
18 3B 930807 gB 18 18.0 -57 50           ~ 15 0
19 4B 950818 gB 18 34.6 +33 52           ~ 33 0
20 4B 951213 gB 18 55.9 -06 49           ~ 26 0
21 1B 910721 gB 21 02.1 -14 17           ~ 33 0
22 2B 920307 gB 23 42.3 -45 09           ~ 28 0

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