Lorentz factor — Beaming corrected energy/luminosity correlations and GRB central engine models

Yi, Shuang-Xi; Lei, Wei‐Hua; Zhang, Bing; Dai, Z. G.; Wu, Xue-Feng; Liang, En‐Wei

doi:10.1016/j.jheap.2017.01.001

Cited by 36 publications

(34 citation statements)

References 91 publications

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“…Table1reveals that the on-axis observed isotropic kinetic energy E k,iso,on of these bursts (i.e., ∼ 5 × 10 54 erg, 6 × 10 53 erg, and 8 × 10 54 erg for GRBs 120326A, 120404A, and 100814A, respectively) are significantly high but consistent with those found in other bursts (see the figure10inRacusin et al 2011 and the table 1 inYi et al 2017). The total kinetic energy of the structured jet is also estimated and shown in the last row of Table1.…”

supporting

confidence: 79%

Late Afterglow Bump/Plateau around the Jet Break: Signature of a free-to-shocked wind Environment in Gamma-ray Burst

Li,

Lin,

Ren

et al. 2021

Preprint

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A number of gamma-ray bursts (GRBs) exhibit the late simultaneous bumps in their optical and Xray afterglows around the jet break. Its origin is unclear. Based on the following two facts, we suggest that this feature may sound a transition of circum-burst environment from a free-wind medium to a homogeneous medium. (I) The late bump followed by a steep decay is strongly reminiscent of the afterglows of GRB 170817A, which is attributed to an off-axis observed external-forward shock (eFS) propagating in an interstellar medium. (II) Observations seem to feature a long shallow decay before the late optical bump, which is different from the afterglow of GRB 170817A. In this paper, we study the emission of an eFS propagating in a free-to-shocked wind for on/off-axis observers, where the mass density in the shocked-wind is almost constant. The late simultaneous bumps/plateaux in the optical and X-ray afterglows are really found around the jet break for high-viewing-angle observers. Moreover, there is a long plateau or shallow decay before the late bump in the theoretical light-curves, which is formed during the eFS propagating in the free-wind. For low-viewing-angle observers, the above bumps appear only in the situation that the structured jet has a low characteristic angle and the deceleration radius of the on-axis jet flow is at around or beyond the free-wind boundary. As examples, the X-ray and optical afterglows of GRBs 120326A, 120404A, and 100814A are fitted. We find that an off-axis observed eFS in a free-to-shocked wind can well explain the afterglows in these bursts.

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supporting

confidence: 79%

Late Afterglow Bump/Plateau around the Jet Break: Signature of a free-to-shocked wind Environment in Gamma-ray Burst

Li,

Lin,

Ren

et al. 2021

Preprint

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“…Theoretically there are another two types of temporal breaks except the shallow decays. The first type is a transition from the normal decay phase (the slope ∼ −1) to a steeper phase (the slope ∼ −2), which is best interpreted as a jet break (Rhoads 1999;Frail et al 2001;Wu et al 2004;Liang et al 2008;Racusin et al 2009;Yi et al 2017b;Xi et al 2017). The second type connects the onset afterglow with a smooth bump in the early time.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

The Three-parameter Correlations About the Optical Plateaus of Gamma-Ray Bursts

Xue

et al. 2018

ApJ

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Well-sampled optical light curves of 50 gamma-ray bursts (GRBs) with plateau features are compiled from the literature. By empirical fitting, we obtained the parameters of the optical plateaus, such as the decay slopes (α 1 and α 2 ), the break times (T b ), and the corresponding optical fluxes (F b ) at the break times. The break time of optical plateaus ranges from tens of seconds to 10 6 seconds, with a typical value about 10 4 seconds. We have calculated the break luminosity, and it mainly ranges from 10 44 erg s −1 to 10 47 erg s −1 , which is generally two or three orders of magnitude less than the corresponding break luminosity of the X-ray afterglow plateaus. We reanalyzed the optical plateaus and also found that a significantly tighter correlation exists when we added the isotropic equivalent energy of GRBs E γ,iso into the L b,z − T b,z relation. The best fit correlation is obtained to be L b,z ∝ T −0.9 b,z E 0.4 γ,iso . We next explored the possible correlations among L b,z , T b,z and E p,i , and found there is also a tight correlation between them, which takes the form of L b,z ∝ T −0.9 b,z E 0.5 p,i . We argue that these two tight L b,z − T b,z − E γ,iso and L b,z − T b,z − E p,i correlations are more physical, and it may be directly related to radiation physics of GRBs. The tight correlations are possible to be used as standard candles.

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“…It starts from t bo and lasts for about T 90,rest (e.g., Bromberg et al 2012, the rest-frame duration can be expressed by T 90,rest = T 90 /(1 + z), where z is the redshift). Using the beaming corrected mean luminosity (defined as beaming-corrected prompt γ-ray energy and afterglow kinetic energy divided by T 90,rest (e.g., Yi et al 2017), one can derive the mean accretion rate at the inner boundary of the disk through the BZ power formula (Equation 7). Then the characteristics of the progenitor star can be inversely constrained by using Equations 1 and 2.…”

Section: Modelmentioning

confidence: 99%

“…In Figure 2, the majority of data are taken from Yi et al (2017), who have carefully analyzed the beaming corrected jet luminosity by properly treating the prompt emission data, afterglow data, and the jet break data. These dots are denoted in black filled circles.…”

Section: Modelmentioning

confidence: 99%

Black Hole Hyperaccretion Inflow–Outflow Model. I. Long and Ultra-long Gamma-Ray Bursts

Liu

Song

Zhang

et al. 2017

ApJ

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Long-duration gamma-ray bursts (LGRBs) and ultra-LGRBs (ULGRBs) originate from collapsars, in the center of which a newborn rotating stellar-mass black hole (BH) surrounded by a massive accretion disk may form. In the scenario of BH hyperaccretion inflow-outflow model and BlandfordZnajek (BZ) mechanism to trigger gamma-ray bursts (GRBs), the real accretion rate to power a BZ jet is far lower than the mass supply rate from the progenitor star. The characteristics of the progenitor stars can be constrained by GRB luminosity observations, and the results exceed usual expectations.LGRBs lasting from several seconds to tens of seconds in the rest frame may originate from solar-metallicity (Z ∼ 1 Z ⊙ , where Z and Z ⊙ are the metallicities of progenitor stars and the Sun), massive (M 34 M ⊙ , where M and M ⊙ are the masses of progenitor stars and the Sun) stars or some zero-metallicity (Z ∼ 0) stars. A fraction of low-metallicity (Z 10 −2 Z ⊙ ) stars, including Population III stars, can produce ULGRBs such as GRB 111209A. The fraction of LGRBs lasting less than tens of seconds in the rest frame is more than 40%, which cannot conform to the fraction of the demanded type of progenitor star. It possibly implies that the activity timescale of central engine may be much longer than the observed timescale of prompt emission phase, as indicated by X-ray late-time activities. Alternatively, LGRBs and ULGRBs may be powered by a millisecond magnetar central engine.

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Lorentz factor — Beaming corrected energy/luminosity correlations and GRB central engine models

Cited by 36 publications

References 91 publications

Late Afterglow Bump/Plateau around the Jet Break: Signature of a free-to-shocked wind Environment in Gamma-ray Burst

Late Afterglow Bump/Plateau around the Jet Break: Signature of a free-to-shocked wind Environment in Gamma-ray Burst

The Three-parameter Correlations About the Optical Plateaus of Gamma-Ray Bursts

Black Hole Hyperaccretion Inflow–Outflow Model. I. Long and Ultra-long Gamma-Ray Bursts

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