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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| Format: | Text |
| Language: | unknown |
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arXiv
2005
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| Online Access: | https://dx.doi.org/10.48550/arxiv.astro-ph/0509069 https://arxiv.org/abs/astro-ph/0509069 |
| Summary: | 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 |
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