In ice radio detection of GZK neutrinos
Models for the source and propagation of cosmic rays are stressed by observations of cosmic rays with energies $E>10^{20}$ eV. A key discriminant between different models may be complementary observations of neutrinos with energies $E>10^{18}$ eV. Independent of the source of the cosmic rays,...
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ftcern:oai:cds.cern.ch:491861 2023-05-15T13:45:09+02:00 In ice radio detection of GZK neutrinos Seckel, D 2001-03-19 http://cds.cern.ch/record/491861 eng eng http://cds.cern.ch/record/491861 astro-ph/0103300 BA-2001-13 oai:cds.cern.ch:491861 Astrophysics and Astronomy 2001 ftcern 2018-07-28T04:56:35Z Models for the source and propagation of cosmic rays are stressed by observations of cosmic rays with energies $E>10^{20}$ eV. A key discriminant between different models may be complementary observations of neutrinos with energies $E>10^{18}$ eV. Independent of the source of the cosmic rays, neutrinos are produced during propagation via the GZK mechanism. Event rates for GZK neutrinos are expected to be in the range of $0.01-0.1$ per km$^3$ yr, suggesting a detector mass in excess of 1 Eg. Detection of radio cherenkov emission from showers produced in Antarctic ice may be an economical way to instrument such a large mass. It is suggested that a 100 km$^2$ array of antennas centered on Icecube may allow confirmation of the radio technique and also increase the science achievable with Icecube by providing vertex information for events with throughgoing muons. Other/Unknown Material Antarc* Antarctic CERN Document Server (CDS) Antarctic |
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CERN Document Server (CDS) |
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English |
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Astrophysics and Astronomy |
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Astrophysics and Astronomy Seckel, D In ice radio detection of GZK neutrinos |
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Astrophysics and Astronomy |
description |
Models for the source and propagation of cosmic rays are stressed by observations of cosmic rays with energies $E>10^{20}$ eV. A key discriminant between different models may be complementary observations of neutrinos with energies $E>10^{18}$ eV. Independent of the source of the cosmic rays, neutrinos are produced during propagation via the GZK mechanism. Event rates for GZK neutrinos are expected to be in the range of $0.01-0.1$ per km$^3$ yr, suggesting a detector mass in excess of 1 Eg. Detection of radio cherenkov emission from showers produced in Antarctic ice may be an economical way to instrument such a large mass. It is suggested that a 100 km$^2$ array of antennas centered on Icecube may allow confirmation of the radio technique and also increase the science achievable with Icecube by providing vertex information for events with throughgoing muons. |
author |
Seckel, D |
author_facet |
Seckel, D |
author_sort |
Seckel, D |
title |
In ice radio detection of GZK neutrinos |
title_short |
In ice radio detection of GZK neutrinos |
title_full |
In ice radio detection of GZK neutrinos |
title_fullStr |
In ice radio detection of GZK neutrinos |
title_full_unstemmed |
In ice radio detection of GZK neutrinos |
title_sort |
in ice radio detection of gzk neutrinos |
publishDate |
2001 |
url |
http://cds.cern.ch/record/491861 |
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Antarctic |
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Antarctic |
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Antarc* Antarctic |
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Antarc* Antarctic |
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http://cds.cern.ch/record/491861 astro-ph/0103300 BA-2001-13 oai:cds.cern.ch:491861 |
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1766213891387293696 |