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Low-luminosity gamma-ray bursts as the sources of ultrahigh-energy cosmic ray nuclei

Physical Review D

American Physical Society (APS)

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Most cited references44

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Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector

(2013)
We report on results of an all-sky search for high-energy neutrino events interacting within the IceCube neutrino detector conducted between May 2010 and May 2012. The search follows up on the previous detection of two PeV neutrino events, with improved sensitivity and extended energy coverage down to approximately 30 TeV. Twenty-six additional events were observed, substantially more than expected from atmospheric backgrounds. Combined, both searches reject a purely atmospheric origin for the twenty-eight events at the $$4\sigma$$ level. These twenty-eight events, which include the highest energy neutrinos ever observed, have flavors, directions, and energies inconsistent with those expected from the atmospheric muon and neutrino backgrounds. These properties are, however, consistent with generic predictions for an additional component of extraterrestrial origin.
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Observations and implications of the ultrahigh-energy cosmic rays

(2000)
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COSMOLOGICAL GAMMA RAY BURSTS AND THE HIGHEST ENERGY COSMIC RAYS

(1995)
We discuss a scenario in which the highest energy cosmic rays (CR's) and cosmological $$\gamma$$-ray bursts (GRB's) have a common origin. This scenario is consistent with the observed CR flux above $$10^{20}\text{eV}$$, provided that each burst produces similar energies in $$\gamma$$-rays and in CR's above $$10^{20}\text{eV}$$. Protons may be accelerated by Fermi's mechanism to energies $$\sim10^{20}\text{eV}$$ in a dissipative, ultra-relativistic wind, with luminosity and Lorentz factor high enough to produce a GRB. For a homogeneous GRB distribution, this scenario predicts an isotropic, time-independent CR flux.
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Author and article information

Journal
PRVDAQ
Physical Review D
Phys. Rev. D
American Physical Society (APS)
2470-0010
2470-0029
April 2018
April 23 2018
: 97
: 8
10.1103/PhysRevD.97.083010