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,...
| Main Author: | |
|---|---|
| Format: | Text |
| Language: | unknown |
| Published: |
arXiv
2001
|
| Subjects: | |
| Online Access: | https://dx.doi.org/10.48550/arxiv.astro-ph/0103300 https://arxiv.org/abs/astro-ph/0103300 |
| Summary: | 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 |
|---|