Neutrino signatures of the supernova: Gamma ray burst relationship

Razzaque, S.; Mészáros, P.; Waxman, Eli

doi:10.1103/physrevd.69.023001

Cited by 58 publications

(63 citation statements)

References 34 publications

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“…For extended or slowly rotating stars, the jet may be unable to break through the envelope. Both penetrating (GRB producing) and 'choked' jets can produce a burst of approximately 5 TeV neutrinos by the interaction of accelerated protons with jet photons, while the jet propagates in the envelope (Mészáros & Waxman 2001;Razzaque et al 2004). The estimated event rates may exceed approximately 10 2 events per year in a kilometre-scale detector, depending on the ratio of non-visible to visible fireballs.…”

Section: (B ) Teraelectron Volt Neutrinosmentioning

confidence: 99%

Neutrino astronomy and gamma-ray bursts

Waxman

2007

Phil. Trans. R. Soc. A.

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The construction of large-volume detectors of high energy, greater than 1 TeV, neutrinos is mainly driven by the search for extragalactic neutrino sources. The existence of such sources is implied by the observations of ultra-high-energy, greater than or equal to 10 19 eV, cosmic rays, the origin of which is a mystery. In this lecture, I briefly discuss the expected extragalactic neutrino signal and the current state of the experimental efforts. Neutrino emission from gamma-ray bursts (GRBs), which are probably sources of both high-energy protons and neutrinos, is discussed in some detail. The detection of the predicted GRB neutrino signal, which may become possible in the coming few years, will allow one to identify the sources of ultra-high-energy cosmic rays and to resolve open questions related to the underlying physics of GRB models. Moreover, detection of GRB neutrinos will allow one to test for neutrino properties (e.g. flavour oscillations and coupling to gravity) with an accuracy many orders of magnitude better than is currently possible.

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Section: (B ) Teraelectron Volt Neutrinosmentioning

confidence: 99%

Neutrino astronomy and gamma-ray bursts

Waxman

2007

Phil. Trans. R. Soc. A.

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“…GRB composition is greatly tied to two interesting topics: whether GRBs are the dominant sources of ultrahigh energy cosmic rays (UHECRs) [189,190] and high energy neutrinos [191,192,193]. These models all invoked a baryon-dominated outflow.…”

Section: Ejecta Compositionmentioning

confidence: 99%

Open questions in GRB physics

Zhang

2011

Comptes Rendus. Physique

127

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Open questions in GRB physics are summarized as of 2011, including classification, progenitor, central engine, ejecta composition, energy dissipation and particle acceleration mechanism, radiation mechanism, long term engine activity, external shock afterglow physics, origin of high energy emission, and cosmological setting. Prospects of addressing some of these problems with the upcoming Chinese-French GRB mission, SVOM, are outlined.

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“…When calculating the diffuse neutrino background from GRBs we assume that GRBs follow the star formation rate 3 . The diffuse neutrino flux on earth from GRBs distributed up to a redshift of z max can be expressed as,…”

Section: Diffuse Neutrino Spectra From Hl and Ll Grbsmentioning

confidence: 99%

“…The possibility of high energy neutrino emission from GRBs in the burst and the afterglow phases has been studied earlier by different groups [1,2,3,4]. It has been found that only the nearby high luminosity (HL) GRBs (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Neutrino spectra from low and high luminosity populations of gamma ray bursts

Gupta

Zhang

2007

Astroparticle Physics

106

115

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The detection of GRB 060218 at z=0.033 by Swift within 1.5 years of operation, together with the detection of GRB 980425 at z = 0.0085 by BeppoSAX, suggest that these low-luminosity (LL) GRBs have a much higher event rate than the canonical high-luminosity (HL) GRBs, and they form a distinct new component in the GRB luminosity function. We explore the contribution of this previously neglected GRB population to the diffuse neutrino background within the internal shock model and compare it with that of the canonical HL population. By considering a wide range of distributions of various parameters (e.g. luminosity, spectral break energy, duration, variability time, Lorentz factor, redshift) for both populations, we find that although it is difficult to detect neutrinos from the individual LL GRBs, the contribution of the LL population to the diffuse neutrino background is more than the HL population above about 10 8 GeV.

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Neutrino signatures of the supernova: Gamma ray burst relationship

Cited by 58 publications

References 34 publications

Neutrino astronomy and gamma-ray bursts

Neutrino astronomy and gamma-ray bursts

Open questions in GRB physics

Neutrino spectra from low and high luminosity populations of gamma ray bursts

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