Messages from GRB 060218

Zhang, Bing; Liang, En‐Wei; Gupta, Nayantara; Virgili, Fabio; Dai, Z. G.

doi:10.1098/rsta.2006.1999

Cited by 4 publications

(4 citation statements)

References 17 publications

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“…We then take an constant medium density (n). The temporal evolution of both minimum and cooling frequencies (ν m and ν c ) in the reverse and forward shock regions are taken from Rossi et al (2003), Fan et al (2006), Zhang et al (2007) and Yi et al (2013).…”

Section: Theoretically Modeling the Afterglow Lightcurvesmentioning

confidence: 99%

Very Bright Prompt and Reverse Shock Emission of GRB 140512a

Huang

Xin

et al. 2016

ApJ

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We report our observations of very bright prompt optical and reverse shock (RS) optical emission of GRB 140512A and analyze its multi-wavelength data observed with the Swift and Fermi missions. It is found that the joint optical-X-ray-gamma-ray spectrum with our first optical detection (R=13.09 mag) at T 0 + 136 seconds during the second episode of the prompt gamma-rays can be fit by a single power-law with index −1.32 ± 0.01. Our empirical fit to the afterglow lightcurves indicates that the observed bright optical afterglow with R=13.00 mag at the peak time is consistent with predictions of the RS and forward shock (FS) emission of external shock models. Joint optical-X-ray afterglow spectrum is well fit with an absorbed single power-law, with an index evolving with time from −1.86 ± 0.01 at the peak time to −1.57 ± 0.01 at late epoch, which could be due to the evolution of the ratio of the RS to FS emission fluxes. We fit the lightcurves with standard external models, and derive the physical properties of the outflow. It is found that the ratio R B ≡ ǫ B,r /ǫ B,f is 8187, indicating a high magnetization degree in the RS region. Measuring the relative radiation efficiency with R e ≡ ǫ e,r /ǫ e,f , we have R e = 0.02, implying the radiation efficiency of the RS is much lower than that in FS. We also show that the R B of GRBs 990123, 090102, and 130427A are similar to that of GRB 140512A and their apparent difference may be mainly attributed to the difference of the jet kinetic energy, initial Lorentz factor, and medium density among them.

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Section: Theoretically Modeling the Afterglow Lightcurvesmentioning

confidence: 99%

Very Bright Prompt and Reverse Shock Emission of GRB 140512a

Huang

Xin

et al. 2016

ApJ

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“…Results indicate considerably more complexity in many bursts than would be expected from the standard fireball model and varying degrees of correspondence between the X-ray and the optical light curves. In this respect, GRB 050525A may be an exception as it exhibits an achromatic jet break at w10 4 s, although, even in this case, the decay indices are shallow compared with what might be expected from the standard model (Zhang et al 2007; and references therein). Afterglow behaviour from other bursts is not so easily interpreted and the absence of jet breaks in the X-ray afterglow, when present in the optical, remains to be understood.…”

Section: Afterglowsmentioning

confidence: 87%

“…Swift's multi-wavelength measurements (gamma ray to optical/UV) of the exceptional nearby burst GRB 060218 (zZ0.033) have provided a direct observation of the shock breakout in a supernova collapse (Campana et al 2006;Blustin 2007;Zhang et al 2007), this observation adding to the small sample of previously observed nearby long GRBs associated with supernova collapse. Conversely, Swift has found two bursts, GRB 060614 and GRB 060505, for which no supernova association has been found down to deep limits (Watson et al 2007;and references therein).…”

Section: Observational Contributions From Swiftmentioning

confidence: 98%

Introduction: recent developments in the study of gamma-ray bursts

Wells

Wijers

Rees

2007

Phil. Trans. R. Soc. A.

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Gamma-ray bursts (GRBs) are immensely powerful explosions, originating at cosmological distances, whose outbursts persist for durations ranging from milliseconds to tens of seconds or more. In these brief moments, the explosions radiate more energy than the Sun will release in its entire 10 Gyr lifetime. Current theories attribute these phenomena to the final collapse of a massive star, or the coalescence of a binary system induced by gravity wave emission.New results from Swift and related programmes offer fresh understanding of the physics of GRBs, and of the local environments and host galaxies of burst progenitors. Bursts found at very high red shifts are new tools for exploring the intergalactic medium, the first stars and the earliest stages of galaxy formation.This Royal Society Discussion Meeting has brought together leading figures in the field, together with young researchers and students, to discuss and review the latest results from NASA's Swift Gamma-ray Burst Observatory and elsewhere, and to examine their impact on current understanding of the observed phenomena.

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“…We then adopt a constant medium density (n). The temporal evolution of both the minimum and cooling frequencies (ν m and ν c ) in the RS and FS regions are taken from Yost et al (2003); Fan & Piran (2006); Zhang et al (2007a), and Yi et al (2013). The model does not incorporate emission produced by the inverse-Compton effect, which is expected to delay the transition between the fast and slow cooling phases, as well as to decrease the cooling frequency in the FS (Wu et al 2005).…”

Section: Model Fitmentioning

confidence: 99%

A Possibly Short GRB 180418A and Phenomenology of Reverse-Shock Emission in the Optical Afterglows of Gamma-Ray Bursts

Wang,

Zhou,

Zhou

et al. 2024

ApJ

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We present early-time ground-based optical follow-up observations of GRB 180418A, which was discovered by both Swift/BAT and Fermi/GBM. Its broadband afterglow was well monitored by Swift/XRT and ground-based optical telescopes. The optical light curve of GRB 180418A can be modeled by forward shock (FS) plus reverse shock (RS). We fit the light curves with standard external shock models and derive the physical properties of the outflow. It is found that the ratio R B ≡ ε B,r /ε B,f is 11.22, indicating a moderate degree of magnetization in the RS region. The reported duration of GRB 180418A, T 90, lies in the intermediate region between short and long gamma-ray bursts (GRBs). We further discuss the classification of GRB 180418A, and calculate ε = E γ,iso,52/E p,z,2 values of 0.026 and 0.018 (assuming the redshift z is 1.0 and 1.5, respectively), which is closer to short GRBs (SGRBs) in the ε-T 90,z plane. If GRB 180418A is an SGRB, it is the only reported SGRB thus far with RS emission in optical light curves. In order to compare the properties of GRB 180418A, we collected three SGRBs that may have RS emission (GRBs 060313, 090426, and 210207B) and also 22 long GRBs (LGRBs) with RS emission. We find that the parameters of LGRBs are in a wider range than those of SGRBs. Also, SGRBs appear to have very small R B values, but the results are generally similar to those of LGRBs. The fitting parameters of GRB 180418A are generally consistent with those of the other three SGRBs, implying that GRB 180418A may belong to the category of SGRBs.

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Messages from GRB 060218

Cited by 4 publications

References 17 publications

Very Bright Prompt and Reverse Shock Emission of GRB 140512a

Very Bright Prompt and Reverse Shock Emission of GRB 140512a

Introduction: recent developments in the study of gamma-ray bursts

A Possibly Short GRB 180418A and Phenomenology of Reverse-Shock Emission in the Optical Afterglows of Gamma-Ray Bursts

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