V. Berezinsky

On astrophysical solution to ultrahigh-energy cosmic rays

We argue that an astrophysical solution to UHECR problem is viable. The pectral features of extragalactic protons interacting with CMB are calculated in model-independent way. Using the power-law generation spectrum

Clusters of Galaxies as Storage Room for Cosmic Rays

\propto E^{-\gamma_g}

Cosmic neutrinos of ultra-high energies and detection possibility

as the only assumption, we analyze four features of the proton spectrum: the GZK cutoff, dip, bump and the second dip. We found the dip, induced by electron-positron production on CMB, as the most robust feature, existing in energy range

Dip in UHECR spectrum as signature of proton interaction with CMB

1\times 10^{18} - 4\times 10^{19}

Small-scale clumps in the galactic halo and dark matter annihilation

eV. Its shape is stable relative to various phenomena included in calculations. The dip is well confirmed by observations of AGASA, HiRes, Flys Eye and Yakutsk detectors. The best fit is reached at

Cosmic Necklaces and Ultrahigh Energy Cosmic Rays

\gamma_g =2.7

Restricting UHECRs and cosmogenic neutrinos with Fermi-LAT

, with the allowed range 2.55 - 2.75. The dip is used for energy calibration of the detectors. After the energy calibration the fluxes and spectra of all three detectors agree perfectly, with discrepancy between AGASA and HiRes at

Gamma-ray bursts from superconducting cosmic strings

E>1\times 10^{20}

Ultra high energy cosmic rays: implications of Auger data for source spectra and chemical composition

eV being not statistically significant. The agreement of the dip with observations should be considered as confirmation of UHE proton interaction with CMB. The dip has two flattenings. The high energy flattening at

Diffusive Propagation of Ultra-High-Energy Cosmic Rays and the Propagation Theorem

E \approx 1\times 10^{19}