In ice radio detection of GZK neutrinos
Abstract. 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 ra...
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| Format: | Text |
| Language: | English |
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| Online Access: | http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.254.5590 http://arxiv.org/pdf/astro-ph/0103300v1.pdf |
| Summary: | Abstract. 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. |
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