2001ApJ...548..770B


Query : 2001ApJ...548..770B

2001ApJ...548..770B - Astrophys. J., 548, 770-786 (2001/February-3)

On the hardness-intensity correlation in gamma-ray burst pulses.

BORGONOVO L. and RYDE F.

Abstract (from CDS):

We study the hardness-intensity correlation (HIC) in gamma-ray bursts (GRBs). In particular, we analyze the decay phase of pulse structures in their light curves. The study comprises a sample of 82 long pulses selected from 66 long bursts observed by the Burst and Transient Source Experiment (BATSE) on the Compton Gamma-Ray Observatory. We find that at least 57% of these pulses have HICs that can be well described by a power law. A number of the other cases can still be explained with the power-law model if various limitations of the observations are taken into account. The distribution of the power-law indices γ, obtained by modeling the HIC of pulses from different bursts, is broad, with a mean of 1.9 and a standard deviation of 0.7. We also compare indices among pulses from the same bursts and find that their distribution is significantly narrower. The probability p of a random coincidence is shown to be very small (<2x10–5). In most cases, the indices are equal to within the uncertainties. These results demand a physical model to be able to reproduce multiple pulses with similar characteristics for an individual burst, but with a large diversity for pulses from an ensemble of bursts. This is particularly relevant when comparing the external versus the internal models. In our analysis, we also use a new method for studying the hardness-intensity correlation, in which the intensity is represented by the peak value of the EFE spectrum, where E is the energy and FE is the energy flux spectrum. We compare it to the traditional method in which the intensity over a finite energy range is used instead, which may be an incorrect measure of the bolometric intensity. This new method gives stronger correlations and is useful in the study of various aspects of the HIC. In particular, it produces a better agreement between indices of different pulses within the same burst. Also, we find that some pulses exhibit a track jump in their HICs, in which the correlation jumps between two power laws with the same index. We discuss the possibility that the track jump is caused by strongly overlapping pulses. Based on our findings, the constancy of the index is proposed to be used as a tool for pulse identification in overlapping pulses and examples of its application are given.

Abstract Copyright: ∼

Journal keyword(s): Gamma Rays: Bursts - Gamma Rays: Observations - Methods: Data Analysis

Simbad objects: 66

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Number of rows : 66
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 980306 gB 00 34 -46.2           ~ 21 0
2 3B 930425B gB 01 12.0 -35 11           ~ 20 0
3 4B 960531 gB 02 16.8 -28 30           ~ 10 0
4 3B 940429 gB 02 20.4 -57 31           ~ 18 0
5 4B 941121 gB 02 21.8 -66 22           ~ 21 0
6 4B 951016 gB 02 23.3 -24 22           ~ 25 0
7 GRB 950403B gB 02 25.6 +10 43           ~ 20 0
8 GRB 961001 gB 02 31 +59.4           ~ 20 0
9 1B 910927 gB 03 20.6 -39 39           ~ 41 0
10 4B 960124 gB 03 24.2 +54 03           ~ 17 0
11 GRB 950325B gB 03 31.2 +50 30           ~ 15 0
12 1B 910814C gB 03 52.0 +45 13           ~ 30 0
13 3B 931221 gB 06 04.1 -43 10           ~ 26 0
14 GRB 960912 gB 06 21 +78.8           ~ 20 0
15 GRB 980301 gB 06 45 -30.9           ~ 17 0
16 3B 930612 gB 06 52.3 -69 46           ~ 48 0
17 3B 940623 gB 07 13.5 +75 47           ~ 25 0
18 GRB 980821 gB 08 19 -13.7           ~ 10 0
19 GRB 961009 gB 09 02 -79.0           ~ 11 0
20 4B 951102 gB 09 14.3 +46 59           ~ 22 0
21 4B 960530 gB 09 33.6 -53 47           ~ 31 0
22 4B 970223 gB 09 38 +34.1           ~ 25 0
23 2B 921003 gB 10 01.3 -14 43           ~ 23 0
24 4B 961126 gB 10 05 +38.4           ~ 8 0
25 1B 910807 gB 10 15.4 +06 29           ~ 38 0
26 2B 920502 gB 10 19.3 +45 25           ~ 20 0
27 4B 960807 gB 10 30.1 +32 08           ~ 21 0
28 1B 911126 gB 10 37.6 +06 39           ~ 24 0
29 2B 920622 gB 10 48.4 +47 10           ~ 54 0
30 4B 950624 gB 11 01.5 +14 59           ~ 27 0
31 1B 911118 gB 11 08.1 -20 51           ~ 61 0
32 1B 911202 gB 11 30.0 -22 50           ~ 40 0
33 1B 920221 gB 12 16.6 +48 29           ~ 32 0
34 4B 950403 gB 12 18.6 +56 33           ~ 15 0
35 1B 910627 gB 13 12.0 -02 29           ~ 54 0
36 3B 940329B gB 13 39.6 -10 20           ~ 13 0
37 4B 941026 gB 13 43.8 -06 32           ~ 37 0
38 1B 911104 gB 14 09.8 +35 02           ~ 39 0
39 4B 970420 gB 14 11 58 -15 54.6           ~ 16 0
40 4B 950909 gB 14 25.4 -00 07           ~ 15 0
41 4B 960804 gB 14 34.7 +68 12           ~ 17 0
42 4B 960113 gB 15 21.1 +06 12           ~ 17 0
43 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 1012 1
44 GRB 970111 gB 15 28 15.0 +19 36 18           ~ 140 0
45 GRB 971127 gB 15 32 +32.2           ~ 24 0
46 4B 970815 gB 16 06 54.0 +81 30 34           ~ 56 0
47 3B 940410 gB 16 59.6 +30 48           ~ 26 0
48 2B 920830 gB 17 14.1 -73 59           ~ 38 0
49 GRB 961102 gB 17 53 +30.3           ~ 17 0
50 GRB 990102 gB 18 22 +39.7           ~ 25 0
51 4B 950818 gB 18 34.6 +33 52           ~ 33 0
52 2B 920902 gB 18 36.6 -20 42           ~ 39 0
53 4B 951213 gB 18 55.9 -06 49           ~ 26 0
54 1B 911031 gB 18 58.2 +21 20           ~ 45 0
55 2B 920718 gB 19 45.6 -55 59           ~ 36 0
56 2B 920525 gB 19 58.5 -42 03           ~ 53 0
57 1B 911016 gB 20 01.9 -03 47           ~ 47 0
58 3B 940708 gB 20 06.3 +24 40           ~ 26 0
59 4B 950104 gB 20 13.0 -15 38           ~ 18 0
60 2B 921207 gB 20 25.3 -42 56           ~ 47 0
61 4B 960708B gB 20 28.1 +09 48           ~ 6 0
62 GRB 970925 gB 22 02 -11.7           ~ 24 0
63 2B 930201 gB 22 14.1 +41 09           ~ 37 0
64 2B 921123 gB 22 17.0 -53 15           ~ 42 0
65 GRB 980306B gB 22 48 -58.6           ~ 20 0
66 GRB 980125 gB 23 31 +36.0           ~ 20 0

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