Delayed Energy Injection Model for Gamma-Ray Burst Afterglows

Geng, Jin-Jun; Wu, Xue-Feng; Huang, Yun‐Feng; Yu, Y. B.

doi:10.1088/0004-637x/779/1/28

Cited by 28 publications

(39 citation statements)

References 77 publications

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“…Basically, the above model can give a good description for the external shocks and GRB afterglows. For example, the dynamical model has been applied to many GRBs and can well explain the observations (Huang, Cheng & Gao 2006;Kong, Huang & Cheng 2009;Xu, Huang & Lu 2009;Kong, Wong, Huang & Cheng 2010;Xu, Nagataki & Huang 2011;Geng, Wu, Huang et al 2013). Here in Fig.…”

Section: Dynamical Model and Fast Sensitivitymentioning

confidence: 92%

Detecting radio afterglows of gamma-ray bursts with FAST

Zhang¹,

Kong²,

Huang³

et al. 2015

Res. Astron. Astrophys.

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Using the generic hydrodynamic model of Gamma-Ray Burst (GRB) afterglows, we calculate the radio afterglow light curves of low luminosity, high luminosity, failed and standard GRBs in different observational bands of FAST's energy window. The GRBs are assumed to be located at different distances from us. Our results rank the detectability of GRBs in descending order as high luminosity, standard, failed and low luminosity GRBs. We predict that almost all types of radio afterglows except that of low luminosity GRBs could be observed by the large radio telescope as long as the domains of time and frequency are appropriate. It is important to note that FAST can detect relatively weak radio afterglows at a higher frequency of 2.5 GHz for very high redshift up to z=15 or even more. Radio afterglows of low luminosity GRBs can be detected only after the completion of the 2nd phase of FAST. FAST is expected to significantly expand the sample of GRB radio afterglows in the near future.

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Section: Dynamical Model and Fast Sensitivitymentioning

confidence: 92%

Detecting radio afterglows of gamma-ray bursts with FAST

Zhang¹,

Kong²,

Huang³

et al. 2015

Res. Astron. Astrophys.

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“…In the scenario of a black hole accretion system, the energy flow from the fall-back accretion may be delayed for a fall-back time t fb and produce giant bumps in the optical bands (Geng et al 2013). In this scenario, one may place some constraint on the progenitor stars.…”

Section: Possible Sources Of the Delayed Energy Injectionmentioning

confidence: 99%

GRB 110530a: Peculiar Broad Bump and Delayed Plateau in Early Optical Afterglows

Zhong

Xin

Liang

et al. 2016

ApJ

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We report our very early optical observations of GRB 110530A and investigate its jet properties together with its X-ray afterglow data. A peculiar broad onset bump followed by a plateau is observed in its early R band afterglow lightcurve. The optical data in the other bands and the X-ray data are well consistent with the temporal feature of the R band lightcurve. Our joint spectral fits of the optical and X-ray data show that they are in the same regime, with a photon index of ∼ 1.70. The optical and X-ray afterglow lightcurves are well fitted with the standard external shock model by considering a delayed energy injection component. Based on our modeling results, we find that the radiative efficiency of the GRB jet is ∼ 1% and the magnetization parameter of the afterglow jet is < 0.04 with the derived extremely low ǫ B (the fraction of shock energy to magnetic field) of (1.64 ± 0.25) × 10 −6 . These results indicate that the jet may be matter dominated. Discussion on delayed energy injection from accretion of late fall-back material of its pre-supernova star is also presented.

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“…The observed γ-ray variability and late-time X-ray and optical flaring activity have encouraged a range of theoretical models predicting ejecta stratification, including fragmentation of the accretion disk due to viscous instabilities, two-stage collapse, fallback accretion, variability in the accretion rate, and shell collisions (King et al 2005;Perna et al 2006;Proga & Zhang 2006;Ghisellini et al 2009;Vlasis et al 2011;Geng et al 2013;Guidorzi et al 2015;Yu et al 2015;Dall'Osso et al 2017). The resulting structured ejecta profiles are expected to have a long-term impact on the afterglow, producing a long-lasting energy injection phase as slower shells catch up with the forward shock (FS; Sari & Mészáros 2000).…”

Section: Introductionmentioning

confidence: 99%

A VLA Study of High-redshift GRBs. II. The Complex Radio Afterglow of GRB 140304A: Shell Collisions and Two Reverse Shocks

Laskar

Berger

Margutti

et al. 2018

ApJ

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We present detailed multifrequency, multiepoch radio observations of GRB140304A at z=5.283 from 1 to 86 GHz and from 0.45 to 89 days. The radio and millimeter data exhibit unusual multiple spectral components, which cannot be simply explained by standard forward and reverse shock scenarios. Through detailed multiwavelength analysis spanning radio to X-rays, we constrain the forward shock parameters to E k,iso ≈4., p≈2.6, and q jet ≈1°.1, yielding a beaming-corrected γ-ray and kinetic energy, g E ≈2.3×10 49 erg and E K ≈9.5×10 50 erg, respectively. We model the excess radio emission as due to a combination of a late-time reverse shock (RS) launched by a shell collision, which also produces a rebrightening in the X-rays at ≈0.26 days, and either a standard RS or diffractive interstellar scintillation (ISS). Under the standard RS interpretation, we invoke consistency arguments between the forward and reverse shocks to derive a deceleration time, t dec ≈100 s, the ejecta Lorentz factor, Γ(t dec )≈300, and a low RS magnetization, R B ≈0.6. Our observations highlight both the power of radio observations in capturing RS emission and thus constraining the properties of GRB ejecta and central engines and the challenge presented by ISS in conclusively identifying RS emission in GRB radio afterglows.

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Delayed Energy Injection Model for Gamma-Ray Burst Afterglows

Cited by 28 publications

References 77 publications

Detecting radio afterglows of gamma-ray bursts with FAST

Detecting radio afterglows of gamma-ray bursts with FAST

GRB 110530a: Peculiar Broad Bump and Delayed Plateau in Early Optical Afterglows

A VLA Study of High-redshift GRBs. II. The Complex Radio Afterglow of GRB 140304A: Shell Collisions and Two Reverse Shocks

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