Signatures of Protons in UHECR
We demonstrate that the energy spectra of Ultra High Energy Cosmic Rays (UHECR) as observed by AGASA, Fly's Eye, HiRes and Yakutsk detectors, have the imprints of UHE proton interaction with the CMB radiation as the dip centered at $E\sim 1\times 10^{19}$ eV, beginning of the GZK cutoff, and ve...
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| Online Access: | https://dx.doi.org/10.48550/arxiv.astro-ph/0302483 https://arxiv.org/abs/astro-ph/0302483 |
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ftdatacite:10.48550/arxiv.astro-ph/0302483 2023-05-15T18:45:29+02:00 Signatures of Protons in UHECR Berezinsky, V. Gazizov, A. Grigorieva, S. 2003 https://dx.doi.org/10.48550/arxiv.astro-ph/0302483 https://arxiv.org/abs/astro-ph/0302483 unknown arXiv 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 High Energy Physics - Phenomenology hep-ph FOS Physical sciences Preprint Article article CreativeWork 2003 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/0302483 2022-04-01T16:33:42Z We demonstrate that the energy spectra of Ultra High Energy Cosmic Rays (UHECR) as observed by AGASA, Fly's Eye, HiRes and Yakutsk detectors, have the imprints of UHE proton interaction with the CMB radiation as the dip centered at $E\sim 1\times 10^{19}$ eV, beginning of the GZK cutoff, and very good agreement with calculated spectrum shape. This conclusion about proton composition agrees with recent HiRes data on elongation rate that support the proton composition at $E\geq 1\times 10^{18}$ eV. The visible bump in the spectrum at $E \sim 4\times 10^{19}$ eV is not caused by pile-up protons, but is an artifact of multiplying the spectrum by $E^3$. We argue that these data, combined with small-angle clustering and correlation with AGN (BL Lacs), point to the AGN model of UHECR origin at energies $E \leq 1\times 10^{20}$ eV. The events at higher energies and the excess of the events at $E \geq 1\times 10^{20}$ eV, which is observed by AGASA (but absent in the HiRes data) must be explained by another component of UHECR, e.g. by UHECR from superheavy dark matter. : Extended version of the paper to be published in Proc. of Int. Workshop "Extremely High Energy Cosmic Rays" (Tokyo, November 2002). Small changes Report 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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ftdatacite |
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unknown |
| topic |
Astrophysics astro-ph High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
| spellingShingle |
Astrophysics astro-ph High Energy Physics - Phenomenology hep-ph FOS Physical sciences Berezinsky, V. Gazizov, A. Grigorieva, S. Signatures of Protons in UHECR |
| topic_facet |
Astrophysics astro-ph High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
| description |
We demonstrate that the energy spectra of Ultra High Energy Cosmic Rays (UHECR) as observed by AGASA, Fly's Eye, HiRes and Yakutsk detectors, have the imprints of UHE proton interaction with the CMB radiation as the dip centered at $E\sim 1\times 10^{19}$ eV, beginning of the GZK cutoff, and very good agreement with calculated spectrum shape. This conclusion about proton composition agrees with recent HiRes data on elongation rate that support the proton composition at $E\geq 1\times 10^{18}$ eV. The visible bump in the spectrum at $E \sim 4\times 10^{19}$ eV is not caused by pile-up protons, but is an artifact of multiplying the spectrum by $E^3$. We argue that these data, combined with small-angle clustering and correlation with AGN (BL Lacs), point to the AGN model of UHECR origin at energies $E \leq 1\times 10^{20}$ eV. The events at higher energies and the excess of the events at $E \geq 1\times 10^{20}$ eV, which is observed by AGASA (but absent in the HiRes data) must be explained by another component of UHECR, e.g. by UHECR from superheavy dark matter. : Extended version of the paper to be published in Proc. of Int. Workshop "Extremely High Energy Cosmic Rays" (Tokyo, November 2002). Small changes |
| format |
Report |
| author |
Berezinsky, V. Gazizov, A. Grigorieva, S. |
| author_facet |
Berezinsky, V. Gazizov, A. Grigorieva, S. |
| author_sort |
Berezinsky, V. |
| title |
Signatures of Protons in UHECR |
| title_short |
Signatures of Protons in UHECR |
| title_full |
Signatures of Protons in UHECR |
| title_fullStr |
Signatures of Protons in UHECR |
| title_full_unstemmed |
Signatures of Protons in UHECR |
| title_sort |
signatures of protons in uhecr |
| publisher |
arXiv |
| publishDate |
2003 |
| url |
https://dx.doi.org/10.48550/arxiv.astro-ph/0302483 https://arxiv.org/abs/astro-ph/0302483 |
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Yakutsk |
| geographic_facet |
Yakutsk |
| genre |
Yakutsk |
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Yakutsk |
| 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/0302483 |
| _version_ |
1766236548686151680 |