Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays
The dip is a feature in the diffuse spectrum of UHE protons in energy range $1\times 10^{18} - 4\times 10^{19}$ eV, which is caused by electron-positron pair production on CMB photons. Calculated for power-law generation spectrum with index $γ_g=2.7$, the shape of the dip is confirmed with high accu...
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ftdatacite:10.48550/arxiv.astro-ph/0509069 2023-05-15T18:45:29+02:00 Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays Berezinsky, Veniamin 2005 https://dx.doi.org/10.48550/arxiv.astro-ph/0509069 https://arxiv.org/abs/astro-ph/0509069 unknown arXiv https://dx.doi.org/10.1088/1742-6596/47/1/018 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 2005 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/0509069 https://doi.org/10.1088/1742-6596/47/1/018 2022-04-01T16:21:00Z The dip is a feature in the diffuse spectrum of UHE protons in energy range $1\times 10^{18} - 4\times 10^{19}$ eV, which is caused by electron-positron pair production on CMB photons. Calculated for power-law generation spectrum with index $γ_g=2.7$, the shape of the dip is confirmed with high accuracy by data of Akeno - AGASA, HiRes, Yakutsk and Fly's Eye detectors. The predicted shape of the dip is robust: it is valid for the rectilinear and diffusive propagation, for different discretenesses in the source distribution, for local source overdensity and deficit, for source inhomogeneities on scale $\ell \lsim 100$ Mpc etc. Below the characteristic energy $E_c \approx 1\times 10^{18}$ eV the spectrum of the dip flattens for both diffusive and rectilinear propagation, and more steep galactic spectrum becomes dominant at $E < E_c$. The energy of transition $E_{\rm tr} < E_c$ approximately coincides with the position of the second knee $E_{2kn}$ observed in the cosmic ray spectrum. The critical energy $E_c$ is determined by the energy $E_{\rm eq} = 2.3\times 10^{18}$ eV, where adiabatic and pair-production energy losses are equal. Thus, position of the second knee is explained by proton energy losses on CMB photons. : 12 pages, 9 figures, new section is added, a technical problem is fixed Text Yakutsk DataCite Metadata Store (German National Library of Science and Technology) Yakutsk |
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Astrophysics astro-ph FOS Physical sciences |
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Astrophysics astro-ph FOS Physical sciences Berezinsky, Veniamin Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays |
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Astrophysics astro-ph FOS Physical sciences |
description |
The dip is a feature in the diffuse spectrum of UHE protons in energy range $1\times 10^{18} - 4\times 10^{19}$ eV, which is caused by electron-positron pair production on CMB photons. Calculated for power-law generation spectrum with index $γ_g=2.7$, the shape of the dip is confirmed with high accuracy by data of Akeno - AGASA, HiRes, Yakutsk and Fly's Eye detectors. The predicted shape of the dip is robust: it is valid for the rectilinear and diffusive propagation, for different discretenesses in the source distribution, for local source overdensity and deficit, for source inhomogeneities on scale $\ell \lsim 100$ Mpc etc. Below the characteristic energy $E_c \approx 1\times 10^{18}$ eV the spectrum of the dip flattens for both diffusive and rectilinear propagation, and more steep galactic spectrum becomes dominant at $E < E_c$. The energy of transition $E_{\rm tr} < E_c$ approximately coincides with the position of the second knee $E_{2kn}$ observed in the cosmic ray spectrum. The critical energy $E_c$ is determined by the energy $E_{\rm eq} = 2.3\times 10^{18}$ eV, where adiabatic and pair-production energy losses are equal. Thus, position of the second knee is explained by proton energy losses on CMB photons. : 12 pages, 9 figures, new section is added, a technical problem is fixed |
format |
Text |
author |
Berezinsky, Veniamin |
author_facet |
Berezinsky, Veniamin |
author_sort |
Berezinsky, Veniamin |
title |
Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays |
title_short |
Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays |
title_full |
Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays |
title_fullStr |
Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays |
title_full_unstemmed |
Dip in UHECR and Transition from Galactic to Extragalactic Cosmic Rays |
title_sort |
dip in uhecr and transition from galactic to extragalactic cosmic rays |
publisher |
arXiv |
publishDate |
2005 |
url |
https://dx.doi.org/10.48550/arxiv.astro-ph/0509069 https://arxiv.org/abs/astro-ph/0509069 |
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Yakutsk |
geographic_facet |
Yakutsk |
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Yakutsk |
genre_facet |
Yakutsk |
op_relation |
https://dx.doi.org/10.1088/1742-6596/47/1/018 |
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/0509069 https://doi.org/10.1088/1742-6596/47/1/018 |
_version_ |
1766236548110483456 |