Evolution of the ultra high energy cosmic ray spectron by transport equation

Details Evolution of the ultra high energy cosmic ray spectron by transport equation Evolution of the ultra high energy cosmic ray spectron by transport equation

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icrc....2..393h&link_type=abstract

Presented at the 18th Intern. Cosmic Ray Conf., Bangalore, India, 22 Aug. 1983

Physics

Differential Equations, Electromagnetic Spectra, Energy Spectra, Primary Cosmic Rays, Transport Theory, Background Radiation, Particle Interactions, Photons, Protons

Scientific paper

Ultra-high energy proton primaries interacting with the 3 K photon background are treated as a transport phenomenon. Baryon number is explicity conserved and the evolved spectrum develops a bump at a scale of order 5x10 to the 19 power eV, below the cutoff, due to the pile up of energy degraded protons. This may correspond in part to the observed ankle structure in the CR spectrum.

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