Abstract
Assuming that a single-flavor diffuse neutrino flux dNv/dEv is equal to kE-2v in the energy range 1017 eV - 2:5 × 1019 eV, an upper bound on k is calculated in the ADD model as a function of the number of extra dimensions n and gravity scale MD. An expected number of neutrino induced events at the Surface Detector array of the Pierre Auger Observatory is estimated.
Highlights
High energy cosmic neutrinos may help us– to discover cosmic rays (CRs) point sources;– to define their position, in particular, to constrain a position of the gravity wave (GW) sources;– to understand a mechanisms of CR acceleration;– to define an energy boundary between galactic and extragalactic parts of CR spectrum;– to give information on a nature of CR composition;– to measure a cosmic neutrino flux, flavor ratio and high energy neutrino-nucleon cross section.The first observation of high-energy astrophysical neutrinos was done by the IceCube neutrino detector [1]
As one can see in fig. 1, in the ADD model the cross sections rise more rapidly with the neutrino energy than the SM cross sections
Using the exposure of the Pierre Auger Observatory (PAO) for the period equivalent of 6.4 years of the complete PAO Surface Detector (SD) array working continuously, we have estimated the PAO exposures for the neutrino induced events expected in the ADD model with n extra dimensions and gravity scale MD
Summary
– to define their position, in particular, to constrain a position of the gravity wave (GW). – to measure a cosmic neutrino flux, flavor ratio and high energy neutrino-nucleon cross section. Ultra-high energy (UHE) neutrinos (with energies above 1017 eV) are of particular interest They may probe a new physics if the latter gives us a significant enhancement of neutrino-nucleon cross sections. In the energy range 1.0 × 1017 eV – 2.5 × 1019 eV, the single-flavor upper limit to the diffuse flux of UHE neutrinos was obtained by the PAO Collaboration [6]. The goal of the present paper is to calculate the single-flavor upper bound on the diffuse flux of UHE cosmic neutrinos in the ADD model [13] as a function of the number of extra dimensions n and D-dimensional Planck scale MD (D = 4 + n)
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