Tail Emission from a Ring-like Jet: Its Application to Shallow Decays of Early Afterglows and GRB 050709

Zou, Yuan‐Chuan; Dai, Zhuojun

doi:10.1088/1009-9271/6/5/06

Cited by 5 publications

(3 citation statements)

References 15 publications

(16 reference statements)

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“…A ring-shaped jet can be produced by the central engine during the prompt GRB phase. The most natural mechanism may be via precessing (Fargion & Grossi 2006;Zou & Dai 2006). In almost all GRB progenitor models, the central engine is a rapidly rotating compact objects, such as a black hole or a neutron star.…”

Section: Ring-shaped Jetmentioning

confidence: 99%

Early rebrightenings of X-ray afterglows from ring-shaped GRB jets

Huang

2010

A&A

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Aims. Early rebrightenings at a post-burst time of 10 2 -10 4 s have been observed in the afterglows of some gamma-ray bursts (GRBs). Unlike X-ray flares, these rebrightenings usually last for a comparatively long period. The continuous energy injection mechanism can usually only produce a plateau in the afterglow light curve, but not a rebrightening. Also, a sudden energy injection can induce a rebrightening, but the rebrightening is slightly too rapid. Methods. We argue that the early rebrightenings can be produced by a ring-shaped jet, for which we here present a model. In this scenario, the GRB outflow is not a full cone, but a centrally hollowed ring. Assuming that the line of sight is on the central symmetry axis of the hollow cone, we calculate the dynamical evolution of the outflows and the multiband afterglow light curves. Results. We find that the early rebrightenings observed in the afterglows of some GRBs (i.e. approximately 1% of Swift events), such as GRB 051016B, 060109, 070103, and 070208, can be reproduced with this model. Conclusions. We suggest that these long-lasting early rebrightenings in GRB afterglows are the result of ring-shaped jets.

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Section: Ring-shaped Jetmentioning

confidence: 99%

Early rebrightenings of X-ray afterglows from ring-shaped GRB jets

Huang

2010

A&A

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“…However, it fails to describe the jet structure for the situation with θpre = 10 • . The energy distribution in the situation of θopen < θpre is a ring-shaped jet, but not a uniform ring-shaped jet(Granot 2005;Zou & Dai 2006;0 Xu, Huang, & Kong 2008;Xu & Huang 2010).…”

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confidence: 99%

Jet structure in the afterglow phase for gamma-ray bursts with a precessing jet

Huang

Lin

Liu

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The structured jet is involved to explain the afterglows and even the prompt emission of GRB 170817A. In this paper, we stress that for a precessing jet, the jet structure in the prompt emission phase and that in the afterglow phase may be different. The jet structure in the afterglow phase can be non-uniform even if a narrow-uniform jet is presented in the prompt emission phase. We estimate the jet structure in the afterglow phase under the situation that a narrow-uniform-precessing jet is launched from the central engine of gamma-ray burst. With different precession angles, it is found that the structured jet can be roughly described as follows: a narrow uniform core with power-law wings and sharp cut-off edges, a Gaussian profile, a ring shape, or other complex profile in energy per solid angle. Correspondingly, the afterglows for our obtained structured jets are also estimated. We find that the estimates of the intrinsic kinetic energy, the electron index, and the jet opening angle based on the afterglows formed in a precessing system may be incorrect. Our obtained structured jet is likely to be revealed by future observations for a fraction of gravitational wave detected merging compact binary systems (e.g., black hole-neutron star mergers).

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“…[3][4][5][6][7][8]). For the shallow decay phase, Nousek et al [1] and Zhang et al [3] supposed that they come from late energy re-injection; Toma et al [4] proposed a special jet profile; Zou and Dai [7] and Xu and Huang [9] thought that they may be tail emissions from a slow ring-like jet; Fan and Piran [10] and Kong et al [11] considered the possibility of tuning the microphysical parameters; Toma et al [4] suggested that summation of many different directed mini-jets may produce shallow decay radiation; Ghisellini et al [12] suggested a late internal shock emission model; Yamazaki 2009 [13] and Liang et al [14] suggested that by shifting the starting time to ∼10 3 s ahead, the shallow decay becomes normal decay automatically. In this Letter we propose an alternative explanation, that the external shock (in a wind environment) [15−18] before the deceleration time produces the shallow decay phase of early x-ray emission.…”

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confidence: 99%

Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment

Hai-dong

Wang

Lü

et al. 2011

Chinese Phys. Lett.

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The shallow decay phase of the early X-ray afterglow in gamma-ray bursts discovered by Swift is a widely discussed topic. As the spectral index does not change at the transferring of the shallow decay phase to a normal phase, it implies this transferring should be a dynamical change rather than a spectral evolution. We suggest both the shallow decay phase and the normal phase are from the external shock in a wind environment, while the transferring time is the deceleration time. We apply this model to GRBs 050319 and 081008, and find them can be well explained by choosing a proper set of parameters.PACS numbers: 98.70. Rz, 94.05.Dd, 98.58.Fd

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Tail Emission from a Ring-like Jet: Its Application to Shallow Decays of Early Afterglows and GRB 050709

Cited by 5 publications

References 15 publications

Early rebrightenings of X-ray afterglows from ring-shaped GRB jets

Early rebrightenings of X-ray afterglows from ring-shaped GRB jets

Jet structure in the afterglow phase for gamma-ray bursts with a precessing jet

Shallow Decay Phase of the Early X-Ray Afterglow from External Shock in a Wind Environment

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