Overall Evolution of Jetted Gamma‐Ray Burst Ejecta

Huang, Yun‐Feng; Gou, Lingshan; Dai, Z. G.; Liu, Tan

doi:10.1086/317076

Cited by 247 publications

(317 citation statements)

References 64 publications

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“…The code used here has been developed in Fan & Piran (2006) and Zhang et al (2006). The dynamical evolution of the outflow is calculated using the formulae in Huang et al (2000), which can be used to describe the dynamical evolution of the outflow for both the relativistic and non-relativistic phases. The energy distribution of the shock-accelerated electrons is calculated by solving the continuity equation with the power-law source function Q = Kγ −p w e , normalized by a local injection rate (Moderski et al 2000).…”

Section: The Second-component Jet Model For the Infrared Bump Of Grb mentioning

confidence: 99%

Is the Late Near-Infrared Bump in Short-Hard GRB 130603b Due to the Li-Paczynski Kilonova?

Jin

Fan

et al. 2013

ApJ

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Short-hard gamma-ray bursts (GRBs) are widely believed to be produced by the merger of two binary compact objects, specifically by two neutron stars or by a neutron star orbiting a black hole. According to the Li-Paczynski kilonova model, the merger would launch sub-relativistic ejecta and a near-infrared/optical transient would then occur, lasting up to days, which is powered by the radioactive decay of heavy elements synthesized in the ejecta. The detection of a late bump using the Hubble Space Telescope (HST) in the near-infrared afterglow light curve of the short-hard GRB 130603B is indeed consistent with such a model. However, as shown in this Letter, the limited HST near-infrared light curve behavior can also be interpreted as the synchrotron radiation of the external shock driven by a wide mildly relativistic outflow. In such a scenario, the radio emission is expected to peak with a flux of ∼100 μJy, which is detectable for current radio arrays. Hence, the radio afterglow data can provide complementary evidence on the nature of the bump in GRB 130603B. It is worth noting that good spectroscopy during the bump phase in short-hard bursts can test the validity of either model above, analogous to spectroscopy of broad-lined Type Ic supernova in long-soft GRBs.

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Section: The Second-component Jet Model For the Infrared Bump Of Grb mentioning

confidence: 99%

Is the Late Near-Infrared Bump in Short-Hard GRB 130603b Due to the Li-Paczynski Kilonova?

Jin

Fan

et al. 2013

ApJ

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“…Considering the equal-arrival-time effect for a fixed observer's time t, different angles θ should correspond to different radii R, satisfying (Huang et al 2000)…”

Section: The Radiation From the Shocksmentioning

confidence: 99%

The termination shock of a magnetar wind: a possible origin of gamma-ray burst X-ray afterglow emission

Mao

Dai

et al. 2010

A&A

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Context. Swift observations suggest that the X-ray afterglow emission of some gamma-ray bursts (GRB) may have internal origins, and the conventional external shock (ES) cannot be the exclusive source of the afterglow emission. Aims. If the central compact objects of some GRBs are millisecond magentars, the magnetar winds could play an important role in the (internal) X-ray afterglow emission, which is our focus here. Methods. The dynamics and the synchrotron radiation of the termination shock (TS) of the magmnetar winds, as well as the simultaneous GRB ES, are investigated by considering the magnetization of the winds. Results. As a result of the competition between the emission of the wind TS and the GRB ES, two basic types of X-ray afterglows are predicted, i.e., the TS-dominated and the ES-dominated types. Moreover, our results also show that both of the two types of afterglows have a shallow-decay phase and a normal-decay one, as observed by the Swift satellite. This indicates that some observed X-ray afterglows could be (internally) produced by the magnetar winds, but not necessarily GRB ESs.

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“…One may decompose the light curves using two different approaches: one through theoretical modeling and the other through empirical fitting. Theoretical modeling prevailing in the pre-Swift era (e.g., Panaitescu et al 1998;Panaitescu & Kumar 2001;Huang et al 2000;Wu et al 2005) is found increasingly difficult in the Swift era because of the large amount of data, and more importantly, the chromatic behavior that defeats the simplest external shock model. We therefore take the more empirical approach to perform the analysis (e.g., Liang & Zhang 2006;Nardini et al 2006;Panaitescu & Vestrand 2008Kann et al 2010Kann et al , 2011.…”

Section: Introductionmentioning

confidence: 99%

A Comprehensive Study of Gamma-Ray Burst Optical Emission. Ii. Afterglow Onset and Late Re-Brightening Components

Liang

Gao

et al. 2013

ApJ

109

116

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We continue our systematic statistical study of various components of gamma-ray burst (GRB) optical light curves. We decompose the early onset bump and the late re-brightening bump with empirical fits and analyze their statistical properties. Among the 146 GRBs that have well-sampled optical light curves, the onset and re-brightening bumps are observed in 38 and 26 GRBs, respectively. It is found that the typical rising and decaying slopes for both the onset and re-brightening bumps are ∼1.5 and ∼−1.15, respectively. No early onset bumps in the X-ray band are detected to be associated with the optical onset bumps, while an X-ray re-brightening bump is detected for half of the re-brightening optical bumps. The peak luminosity is anti-correlated with the peak time L p ∝ t −1.81±0.32 p for the onset bumps and L p ∝ t −0.83±0.17 p for the re-brightening bumps. Both L p and the isotropic energy release of the onset bumps are correlated with E γ,iso , whereas no similar correlation is found for the re-brightening bumps. These results suggest that the afterglow onset bumps are likely due to the deceleration of the GRB fireballs. Taking the onset bumps as probes for the properties of the fireballs and their ambient medium, we find that the typical power-law index of the relativistic electrons is 2.5 and the medium density profile behaves as n ∝ r −1 within the framework of the synchrotron external shock models. With the medium density profile obtained from our analysis, we also confirm the correlation between the initial Lorentz factor (Γ 0 ) and E iso,γ in our previous work. The jet component that produces the re-brightening bump seems to be on-axis and independent of the prompt emission jet component. Its typical kinetic energy budget would be about one order of magnitude larger than the prompt emission component, but with a lower Γ 0 , typically several tens.

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Overall Evolution of Jetted Gamma‐Ray Burst Ejecta

Cited by 247 publications

References 64 publications

Is the Late Near-Infrared Bump in Short-Hard GRB 130603b Due to the Li-Paczynski Kilonova?

Is the Late Near-Infrared Bump in Short-Hard GRB 130603b Due to the Li-Paczynski Kilonova?

The termination shock of a magnetar wind: a possible origin of gamma-ray burst X-ray afterglow emission

A Comprehensive Study of Gamma-Ray Burst Optical Emission. Ii. Afterglow Onset and Late Re-Brightening Components

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