Abstract
In this review I discuss the ultra-high energy neutrinos (UHEN) originated from Cosmic-Rays propogation (GZK neutrinos) and from Gamma Ray Bursts (GRBs), and discuss their detectability in kilometers scale detectors like ARA and IceCube.While GZK neutrinos are expected from cosmic ray interactions on the CMB, the GRB neutrinos depend on the physics inside the sources. GRBs are predicted to emit UHEN in the prompt and in the later “after-glow” phase.I discuss the constraints on the hadronic component of GRBs derived from the search of four years of IceCube data for a prompt neutrino fux from gamma-ray bursts (GRBs) and more in general I present the results of the search for high-energy neutrinos interacting within the IceCube detector between 2010 and 2013.
Highlights
The detection of MeV neutrinos emitted from the sun and from the supernovae allowed the understanding of the physics of these astrophysical objects [1, 2]
IceCube analyses include a model-independent search for Gamma Ray Bursts (GRBs) neutrinos [27], and for other diffuse and point sources
The most natural explanation of this coincidence is that both the neutrino excess and the ultra-high energy, > 1019 eV, cosmic-ray (UHECR) flux are produced by the same population of cosmologically distributed sources [31]
Summary
The detection of MeV neutrinos emitted from the sun and from the supernovae allowed the understanding of the physics of these astrophysical objects [1, 2]. The most common phenomenological interpretation of these cosmological sources is through the so called fireball model [19,20,21] In this model, part of the energy is carried out (e.g., from a collapsed star) by hadrons at highly-relativistic energies, some of which is dissipated internally and eventually reconverted into internal energy, which is radiated as rays by synchrotron and inverse-Compton emission by shock-accelerated electrons. If the GRB jet comprises PeV protons, it should produce energetic neutrinos through photon-hadron interactions The photons for this process can be supplied by the GRB gamma rays during its prompt phase, or during the afterglow phase [22, 23]. These lead to the production of charged pions, which subsequently decay to produce neutrinos. All these detectors look for the Cherenkov radiation initiated by the neutrino interactions in the ice using either optical detection (IceCube, KM3Net) or Radio Frequency (RF) detection (ARA)
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