Spectrum and Composition of Ultra-high Energy Cosmic Rays from Semi-relativistic Hypernovae

Abstract

It has been suggested that hypernova remnants, with a substantial amount of energy in semi-relativistic ejecta, can accelerate intermediate mass or heavy nuclei to ultra-high energies and provide sufficient amount of energy in cosmic rays to account for the observed flux. We here calculate the expected energy spectrum and chemical composition of ultra-high energy cosmic rays from such semi-relativistic hypernovae. With a chemical composition equal to that of the hypernova ejecta and a flat or hard spectrum for cosmic rays at the sources, the spectrum and composition of the propagated cosmic rays observed at the Earth can be compatible with the measurements by the Pierre Auger Observatory.

7 pages, 4 figures, accepted for publication in ApJ

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• Star-forming galaxies as the origin of the IceCube PeV neutrinos
• Propagation of Ultra-High-Energy Cosmic Ray Nuclei in Cosmic Magnetic Fields and Implications for Anisotropy Measurements
• Model-dependent estimate on the connection between fast radio bursts and ultra-high energy cosmic rays
• Acceleration and propagation of ultrahigh energy cosmic rays
• Constraints on the source of ultra-high energy cosmic rays using anisotropy vs chemical composition
• On the synthesis of heavy nuclei in protomagnetar outflows and implications for ultra-high energy cosmic rays
• On the excess of ultra-high energy cosmic rays in the direction of Centaurus A
• Implications of the UHECRs penetration depth measurements
• Acceleration of ultra-high energy cosmic rays in the early afterglows of gamma-ray bursts: concurrence of jet's dynamics and wave-particle interactions
• Ultraheavy Ultrahigh-Energy Cosmic Rays
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