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Title: Cosmogenic Neutrinos and New Physics Signal at Neutrino Telescopes

Abstract

Cosmogenic neutrinos reach the Earth with energies around 109 GeV, and their interactions with matter will be measured in upcoming experiments (Auger, IceCube). Models with extra dimensions and the fundamental scale at the TeV could imply signals in these experiments. In particular, besides the production of microscopic black holes by cosmogenic neutrinos, gravity-mediated interactions at larger distances (that can be calculated in the eikonal approximation) can take place. In these processes a neutrino of energy Ev interacts elastically with a parton inside a nucleon, loses a small fraction y of its energy, and starts a hadronic shower of energy yEv << Ev. We show that for the expected fluxes of cosmogenic neutrinos these elastic processes give a stronger signal than black hole production in neutrino telescopes and that the energy distribution of contained hadronic showers can help to distinguish between eikonal and black hole or Standard Model events. On the other hand, the absence of any signal at IceCube would imply a bound of MD > or approx. 5 TeV.

Authors:
;  [1];  [2]
  1. CAFPE, Universidad de Granada, 18071 Granada (Spain)
  2. INFN, Universita degli Studi di Roma 'La Sapienza', 00185 Rome (Italy)
Publication Date:
OSTI Identifier:
20719480
Resource Type:
Journal Article
Journal Name:
AIP Conference Proceedings
Additional Journal Information:
Journal Volume: 794; Journal Issue: 1; Conference: IFAE 2005: 17. Italian meeting on high energy physics, Catania (Italy), 30 Mar - 2 Apr 2005; Other Information: DOI: 10.1063/1.2125664; (c) 2005 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0094-243X
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; BLACK HOLES; COSMIC NEUTRINOS; COSMIC SHOWERS; EIKONAL APPROXIMATION; ENERGY SPECTRA; GEV RANGE 100-1000; GLUONS; GRAVITATION; NEUTRINO DETECTION; QUARKS; SIGNALS; STANDARD MODEL; TELESCOPES; TEV RANGE 01-10

Citation Formats

Illana, J I, Masip, M, Depto. de Fisica Teorica y del Cosmos, Universidad de Granada, 18071 Granada, Meloni, D, and Dipto. di Fisica, Universita degli Studi di Roma 'La Sapienza', 00185 Rome. Cosmogenic Neutrinos and New Physics Signal at Neutrino Telescopes. United States: N. p., 2005. Web. doi:10.1063/1.2125664.
Illana, J I, Masip, M, Depto. de Fisica Teorica y del Cosmos, Universidad de Granada, 18071 Granada, Meloni, D, & Dipto. di Fisica, Universita degli Studi di Roma 'La Sapienza', 00185 Rome. Cosmogenic Neutrinos and New Physics Signal at Neutrino Telescopes. United States. https://doi.org/10.1063/1.2125664
Illana, J I, Masip, M, Depto. de Fisica Teorica y del Cosmos, Universidad de Granada, 18071 Granada, Meloni, D, and Dipto. di Fisica, Universita degli Studi di Roma 'La Sapienza', 00185 Rome. Wed . "Cosmogenic Neutrinos and New Physics Signal at Neutrino Telescopes". United States. https://doi.org/10.1063/1.2125664.
@article{osti_20719480,
title = {Cosmogenic Neutrinos and New Physics Signal at Neutrino Telescopes},
author = {Illana, J I and Masip, M and Depto. de Fisica Teorica y del Cosmos, Universidad de Granada, 18071 Granada and Meloni, D and Dipto. di Fisica, Universita degli Studi di Roma 'La Sapienza', 00185 Rome},
abstractNote = {Cosmogenic neutrinos reach the Earth with energies around 109 GeV, and their interactions with matter will be measured in upcoming experiments (Auger, IceCube). Models with extra dimensions and the fundamental scale at the TeV could imply signals in these experiments. In particular, besides the production of microscopic black holes by cosmogenic neutrinos, gravity-mediated interactions at larger distances (that can be calculated in the eikonal approximation) can take place. In these processes a neutrino of energy Ev interacts elastically with a parton inside a nucleon, loses a small fraction y of its energy, and starts a hadronic shower of energy yEv << Ev. We show that for the expected fluxes of cosmogenic neutrinos these elastic processes give a stronger signal than black hole production in neutrino telescopes and that the energy distribution of contained hadronic showers can help to distinguish between eikonal and black hole or Standard Model events. On the other hand, the absence of any signal at IceCube would imply a bound of MD > or approx. 5 TeV.},
doi = {10.1063/1.2125664},
url = {https://www.osti.gov/biblio/20719480}, journal = {AIP Conference Proceedings},
issn = {0094-243X},
number = 1,
volume = 794,
place = {United States},
year = {2005},
month = {10}
}