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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| Online Access: | https://dx.doi.org/10.48550/arxiv.astro-ph/0103300 https://arxiv.org/abs/astro-ph/0103300 |
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ftdatacite:10.48550/arxiv.astro-ph/0103300 2023-05-15T13:37:59+02:00 In ice radio detection of GZK neutrinos Seckel, D. 2001 https://dx.doi.org/10.48550/arxiv.astro-ph/0103300 https://arxiv.org/abs/astro-ph/0103300 unknown arXiv https://dx.doi.org/10.1063/1.1398173 Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ Astrophysics astro-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2001 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/0103300 https://doi.org/10.1063/1.1398173 2022-04-01T16:50:05Z 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. : 8 pages, 3 figures, to be published in proceedings of RADHEP-2000 Text Antarc* Antarctic DataCite Metadata Store (German National Library of Science and Technology) Antarctic |
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DataCite Metadata Store (German National Library of Science and Technology) |
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ftdatacite |
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unknown |
| topic |
Astrophysics astro-ph FOS Physical sciences |
| spellingShingle |
Astrophysics astro-ph FOS Physical sciences Seckel, D. In ice radio detection of GZK neutrinos |
| topic_facet |
Astrophysics astro-ph FOS Physical sciences |
| 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. : 8 pages, 3 figures, to be published in proceedings of RADHEP-2000 |
| format |
Text |
| 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 |
| publisher |
arXiv |
| publishDate |
2001 |
| url |
https://dx.doi.org/10.48550/arxiv.astro-ph/0103300 https://arxiv.org/abs/astro-ph/0103300 |
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Antarctic |
| geographic_facet |
Antarctic |
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Antarc* Antarctic |
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Antarc* Antarctic |
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https://dx.doi.org/10.1063/1.1398173 |
| op_rights |
Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ |
| op_doi |
https://doi.org/10.48550/arxiv.astro-ph/0103300 https://doi.org/10.1063/1.1398173 |
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1766100250817200128 |