X-ray flare in XRF 050406: evidence for prolonged engine activity

Romano, P.; Moretti, A.; Banat, P.; Burrows, D. N.; Campana, S.; Chincarini, G.; Covino, S.; Malesani, D.; Tagliaferri, G.; Falcone, A.; Capalbi, M.; Cusumano, G.; Giommi, P.; Parola, V. La; Mangano, V.; Perri, M.; Pagani, C.

doi:10.1063/1.2207956

Cited by 6 publications

(3 citation statements)

References 32 publications

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“…These properties generally favor the interpretation that most of them are not associated with external-shock related events. Rather they are the manifestations of times, which requires restarting the GRB central engine (Burrows et al, 2005a,b;Zhang et al, 2006;Fan and Wei, 2005;Ioka et al, 2005;Wu et al, 2006;Falcone et al, 2006;Romano et al, 2006;Lazzati and Perna, 2007). Compared with the external shock related models, the late internal dissipation models have the following two major advantages .…”

Section: X-ray Flares: Restarting the Central Enginementioning

confidence: 96%

“…Sometimes multiple flares harbor in one GRB. Typically have very steep rising and decaying slopes (Burrows et al, 2005b;Falcone et al, 2006;Romano et al, 2006) with dt/t ( 1. Appear in both long-duration (Falcone et al, 2006) and short-duration GRBs (Barthelmy et al, 2005b;Campana et al, 2006a), and both hard GRBs and soft X-ray flashes (Romano et al, 2006).…”

Section: A Canonical Lightcurve Of X-ray Afterglowsmentioning

confidence: 98%

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Gamma-ray burst afterglows

Zhang

2007

Advances in Space Research

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Extended, fading emissions in multi-wavelength are observed following Gamma-ray bursts (GRBs). Recent broad-band observational campaigns led by the Swift Observatory reveal rich features of these GRB afterglows. Here we review the latest observational progress and discuss the theoretical implications for understanding the central engine, composition, and geometric configuration of GRB jets, as well as their interactions with the ambient medium.Comment: References added, accepted for publication in Advances in Space Researc

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Section: X-ray Flares: Restarting the Central Enginementioning

confidence: 96%

Section: A Canonical Lightcurve Of X-ray Afterglowsmentioning

confidence: 98%

Gamma-ray burst afterglows

Zhang

2007

Advances in Space Research

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“…Various models have been proposed to explain the flares, such as the fragmentation of a collapsing star [34], fragmentation of an accretion disk [35], and the magnetic reconnection process [20,36]. Another similar schemes can be referred to [11,28,[37][38][39][40][41].…”

Section: Introductionmentioning

confidence: 99%

Statistical Properties of X-ray Flares in Gamma-ray Bursts

et al. 2022

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X-ray flares are frequently detected in the X-ray afterglow light curves and are highly correlated with the prompt emission of gamma-ray bursts (GRBs). We compile a comprehensive sample of X-ray flares up to 2021 April, comprising 697 flares. We classify the total sample into four types: early flares (tp≤103 s), late flares (tp>103 s), long gamma-ray burst (LGRB) flares and short gamma-ray burst (SGRB) flares, and analyze the distributions and relationships of the flare parameters. It is found that the early flares have a higher frequency, shorter duration, and more asymmetrical structure. In addition, the distributions of the morphological parameters of the SGRB flares are similar to those of the LGRB flares. We also find that the durations and rising (decay) times of the early flares are positively correlated with the peak times, but the late flares follow the different dependent relations. There is a strong anti-correlation between the peak luminosities (LX,P) and the peak times of the flares, e.g., LX,p∝tp,z−1.45 for the LGRB flares, and LX,p∝tp,z−1.27 for the SGRB flares, respectively. Furthermore, the peak luminosity is highly dependent on the isotropic energy (EX,iso) for the early LGRB flares, the best fit is LX,p∝EX,iso1.06(r=0.89). We also find a tight three-parameter correlation, LX,p∝tp,z−1.03EX,iso0.92(r=0.96). All the late flares fall into the 3σ confidence region defined by the early flares. In terms of the point of kinematic arguments, both the SGRB and LGRB flares support a common scheme of internal origin. The SGRB flares have similar properties to the LGRB flares, suggesting that both of them share a similar physical mechanism from the late-time activity of central engine.

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Gamma ray bursts flares detected and observed by the Swift satellite

Chincarini

Moretti

Romano

et al. 2007

Advances in Space Research

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The detection of flares with the Swift satellite triggered a lot of observational and theoretical interest in these phenomena. As a consequence a large analysis effort started within the community to characterize the phenomenon and at the same time a variety of theoretical speculations have been proposed to explain it. In this presentation we discuss part of the results we obtained analyzing a first statistical sample of GRBs observed with Swift. The first goal of this research is very simple: derive those observational properties that could distinguish between internal and external shock and between an ever active central engine and delayed shocks (refreshing) related to a very small initial Lorentz bulk factor. We discuss first the method of analysis and the morphology evidencing the similarities such flares have with the prompt emission pulses. We conclude that GRB flares are due to internal shocks and leave still open the question of whether or not the central engine is active for a time of the order of 10 5 seconds after the prompt emission.

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X-ray flare in XRF 050406: evidence for prolonged engine activity

Cited by 6 publications

References 32 publications

Gamma-ray burst afterglows

Gamma-ray burst afterglows

Statistical Properties of X-ray Flares in Gamma-ray Bursts

Gamma ray bursts flares detected and observed by the Swift satellite

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