Extragalactic cosmic rays and their signatures
The signatures of UHE proton propagation through CMB are pair-production dip and GZK cutoff. The visible manifestations of these spectral features are ankle, beginning of GZK cutoff in the differential spectrum and E_{1/2} in integral spectrum. Observed in all experiments, the ankle is usually inter...
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ftdatacite:10.48550/arxiv.1301.0914 2023-05-15T18:45:30+02:00 Extragalactic cosmic rays and their signatures Berezinsky, V. 2013 https://dx.doi.org/10.48550/arxiv.1301.0914 https://arxiv.org/abs/1301.0914 unknown arXiv https://dx.doi.org/10.1016/j.astropartphys.2013.04.001 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ High Energy Astrophysical Phenomena astro-ph.HE High Energy Physics - Phenomenology hep-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2013 ftdatacite https://doi.org/10.48550/arxiv.1301.0914 https://doi.org/10.1016/j.astropartphys.2013.04.001 2022-04-01T13:39:17Z The signatures of UHE proton propagation through CMB are pair-production dip and GZK cutoff. The visible manifestations of these spectral features are ankle, beginning of GZK cutoff in the differential spectrum and E_{1/2} in integral spectrum. Observed in all experiments, the ankle is usually interpreted as transition from galactic to extragalactic cosmic rays. Using the mass composition measured by HiRes, Telescope Array (TA) and Auger detectors at energy (1-3) EeV, calculated anisotropy of galactic cosmic rays at these energies, and the elongation curves we strongly argue against the interpretation of the ankle given above. The transition must occur at lower energy, most probably at the second knee as the dip model predicts. The other prediction of this model, the shape of the dip, is well confirmed by HiRes, TA, AGASA and Yakutsk detectors, and, after recalibration of energies, by Auger detector. Predicted beginning of GZK cutoff and E_{1/2} agree well with HiRes and TA data. However, directly measured mass composition remains a puzzle. While HiRes and TA detectors observe the proton-dominated mass composition, as required by the dip model, the data of Auger detector strongly evidence for nuclei mass composition becoming steadily heavier at energy higher than 4 EeV and reaching Iron at energy about 35 EeV. The Auger-based scenario is consistent with another interpretation of the ankle at energy E_a=4 EeV as transition from extragalactic protons to extragalactic nuclei. The heavy- nuclei dominance at higher energies may be provided by low-energy of acceleration for protons E_{max} \sim 4 EeV and rigidity-dependent E_{max}^A =Z E_{max}$ for nuclei. The highest energy suppression may be explained as nuclei-destroying cutoff. : Some changes according to the Referee report. The paper is accepted for publication in Astroparticle Physics Text Yakutsk DataCite Metadata Store (German National Library of Science and Technology) Yakutsk |
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DataCite Metadata Store (German National Library of Science and Technology) |
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High Energy Astrophysical Phenomena astro-ph.HE High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
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High Energy Astrophysical Phenomena astro-ph.HE High Energy Physics - Phenomenology hep-ph FOS Physical sciences Berezinsky, V. Extragalactic cosmic rays and their signatures |
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High Energy Astrophysical Phenomena astro-ph.HE High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
description |
The signatures of UHE proton propagation through CMB are pair-production dip and GZK cutoff. The visible manifestations of these spectral features are ankle, beginning of GZK cutoff in the differential spectrum and E_{1/2} in integral spectrum. Observed in all experiments, the ankle is usually interpreted as transition from galactic to extragalactic cosmic rays. Using the mass composition measured by HiRes, Telescope Array (TA) and Auger detectors at energy (1-3) EeV, calculated anisotropy of galactic cosmic rays at these energies, and the elongation curves we strongly argue against the interpretation of the ankle given above. The transition must occur at lower energy, most probably at the second knee as the dip model predicts. The other prediction of this model, the shape of the dip, is well confirmed by HiRes, TA, AGASA and Yakutsk detectors, and, after recalibration of energies, by Auger detector. Predicted beginning of GZK cutoff and E_{1/2} agree well with HiRes and TA data. However, directly measured mass composition remains a puzzle. While HiRes and TA detectors observe the proton-dominated mass composition, as required by the dip model, the data of Auger detector strongly evidence for nuclei mass composition becoming steadily heavier at energy higher than 4 EeV and reaching Iron at energy about 35 EeV. The Auger-based scenario is consistent with another interpretation of the ankle at energy E_a=4 EeV as transition from extragalactic protons to extragalactic nuclei. The heavy- nuclei dominance at higher energies may be provided by low-energy of acceleration for protons E_{max} \sim 4 EeV and rigidity-dependent E_{max}^A =Z E_{max}$ for nuclei. The highest energy suppression may be explained as nuclei-destroying cutoff. : Some changes according to the Referee report. The paper is accepted for publication in Astroparticle Physics |
format |
Text |
author |
Berezinsky, V. |
author_facet |
Berezinsky, V. |
author_sort |
Berezinsky, V. |
title |
Extragalactic cosmic rays and their signatures |
title_short |
Extragalactic cosmic rays and their signatures |
title_full |
Extragalactic cosmic rays and their signatures |
title_fullStr |
Extragalactic cosmic rays and their signatures |
title_full_unstemmed |
Extragalactic cosmic rays and their signatures |
title_sort |
extragalactic cosmic rays and their signatures |
publisher |
arXiv |
publishDate |
2013 |
url |
https://dx.doi.org/10.48550/arxiv.1301.0914 https://arxiv.org/abs/1301.0914 |
geographic |
Yakutsk |
geographic_facet |
Yakutsk |
genre |
Yakutsk |
genre_facet |
Yakutsk |
op_relation |
https://dx.doi.org/10.1016/j.astropartphys.2013.04.001 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1301.0914 https://doi.org/10.1016/j.astropartphys.2013.04.001 |
_version_ |
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