Detection of a γ-ray burst of very long duration and very high energy

Hurley, K.; Dingus, B. L.; Mukherjee, R.; Sreekumar, P.; Kouveliotou, C.; Meegan, C.; Fishman, G. J.; Band, D. L.; Ford, L.; Bertsch, D. L.; Cline, T.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Thompson, D. J.; Kanbach, G.; Mayer‐Hasselwander, H. A.; Montigny, C. von; Sommer, M.; Lin, Y. C.; Nolan, P. L.; Michelson, P. F.; Kniffen, D. A.; Mattox, J. R.; Schneid, E. J.; Boër, M.; Niel, M.

doi:10.1038/372652a0

Cited by 456 publications

(317 citation statements)

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“…One detection of a GeV photon from GRB 940217 was reported 17 years ago (Hurley et al 1994). Compared with the previous research, recently, with the Large Area Telescope (LAT) on board the Fermi satellite, we have more observational cases for the study of GRB high-energy emission above 100 MeV.…”

Section: Introductionmentioning

confidence: 99%

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

Mao

Wang

2012

ApJ

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Jitter radiation, the emission of relativistic electrons in a random and small-scale magnetic field, has been applied to explain the gamma-ray burst (GRB) prompt emission. The seed photons produced from jitter radiation can be scattered by thermal/nonthermal electrons to the high-energy bands. This mechanism is called jitter self-Compton (JSC) radiation. GRB 100728A, which was simultaneously observed by Swift and Fermi, is a great example to constrain the physical processes of jitter and JSC. In our work, we utilize jitter/JSC radiation to reproduce the multiwavelength spectrum of GRB 100728A. In particular, due to JSC radiation, the powerful emission above the GeV band is the result of those jitter photons in the X-ray band scattered by the relativistic electrons with a mixed thermal-nonthermal energy distribution. We also combine the geometric effect of microemitters to the radiation mechanism, such that the "jet-in-jet" scenario is considered. The observed GRB duration is the result of summing up all of the contributions from those microemitters in the bulk jet.

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Section: Introductionmentioning

confidence: 99%

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

Mao

Wang

2012

ApJ

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“…(4) we can evaluate the extra-dimensional and /or quantum gravity energy scale, which follows from the time delay of the 18 GeV photon in GRB 940217 (Hurley et al, 1994). GRB 940217 is a very strong burst, with a total fluence above 20 keV of (6.6 ± 2.7) × 10 −4 erg cm −2 and a duration of ∼180 s in the BATSE range.…”

Section: Discussion and Final Remarksmentioning

confidence: 99%

Constraints on Extra-Dimensions and Variable Constants from Cosmological Gamma-Ray Bursts

Harkó

Cheng

2005

Astrophys Space Sci

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Abstract. The observation of the time delay between the soft emission and the high-energy radiation from cosmological gamma ray bursts can be used as an important observational test of multi-dimensional physical theories. The main source of the time delay is the variation of the electromagnetic coupling, due to dimensional reduction, which induces an energy dependence of the speed of light. For photons with energies around 1 TeV, the time delay could range from a few seconds in the case of Kaluza-Klein models to a few days for models with large extra-dimensions. Based on these results we suggest that the detection of the 18-GeV photon ∼4500 s after the keV/MeV burst in GRB 940217 provides a strong evidence for the existence of extra-dimensions. The time delay of photons, if observed by the next generation of high energy detectors, like, for example, the SWIFT and GLAST satellite based detectors, or the VERITAS ground-based TeV gamma-ray instrument, could differentiate between the different models with extra-dimensions.

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“…GRB940217 was a very famous burst for its long-lasting high energy afterglow emission (Hurley et al 1994). The high energy photons (E > 30 MeV) were recorded for about 5400 seconds, including an 18 GeV photon ∼ 4500s after the low energy emission had ended.…”

Section: The Case Of Grb940217mentioning

confidence: 99%

“…The sub-GeV emission lasted more than 5000 seconds and it included also a 18 GeV photon (Hurley et al 1994). The spectrum in the energy range 1 MeV to 18 GeV, cannot be fitted with a simple power law (see Fig.…”

Section: Introductionmentioning

confidence: 99%

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The Synchrotron-self-Compton Radiation Accompanying Shallow Decaying X-Ray Afterglow: the Case of GRB 940217

Wei¹,

Fan²

2007

Chin. J. Astron. Astrophys.

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High energy emission (> tens MeV) of Gamma-Ray Bursts (GRBs) provides an important clue to understand the physical processes involved in GRBs, which may be correlated with the GRB early afterglow. A shallow decline phase has been well detected in about half Swift Gamma-ray Burst X-ray afterglows. The widely considered interpretation involves a significant energy injection and possibly time-evolving shock parameter(s). This work we calculate the synchrotronself-Compton (SSC) radiation of such an external forward shock and show that it could explain the well-known long term high energy (i.e., tens MeV to GeV) afterglow of GRB 940217. We propose that the cooperation of Swift and GLAST will help to reveal the nature of GRBs.

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Detection of a γ-ray burst of very long duration and very high energy

Cited by 456 publications

References 10 publications

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

JITTER SELF-COMPTON PROCESS: GeV EMISSION OF GRB 100728A

Constraints on Extra-Dimensions and Variable Constants from Cosmological Gamma-Ray Bursts

The Synchrotron-self-Compton Radiation Accompanying Shallow Decaying X-Ray Afterglow: the Case of GRB 940217

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