Ultrahigh-energy Cosmic Rays from Fanaroff Riley class II radio galaxies

Details Ultrahigh-energy Cosmic Rays from Fanaroff Riley class II radio galaxies Ultrahigh-energy Cosmic Rays from Fanaroff Riley class II radio galaxies

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aipc..264..393r&link_type=abstract

In: Particle acceleration in cosmic plasmas; Proceedings of the Workshop, Bartol Research Inst., Newark, DE, Dec. 4-6, 1991 (A93

Mathematics

Logic

6

Energetic Particles, Energy Spectra, Galactic Cosmic Rays, Galactic Evolution, Radio Galaxies, Fermi Surfaces, Particle Theory

Scientific paper

The hot spots of very powerful radio galaxies (Fanaroff Riley class II) are argued to be the sources of the ultrahigh energy component in Cosmic Rays. We present calculations of Cosmic Ray transport in an evolving universe, taking the losses against the microwave background properly into account. As input we use the models for the cosmological radio source evolution derived by radioastronomers (mainly Peacock 1985). The model we adopt for the acceleration in the radio hot spots has been introduced by Biermann and Strittmatter (1987), and Meisenheimer et al. (1989) and is based on first order Fermi theory of particle acceleration at shocks (see, e.g., Drury 1983). As an unknown the actual proportion of energy density in protons enters, which together with structural uncertainties in the hot spots should introduce no more than one order of magnitude in uncertainty: We easily reproduce the observed spectra of high energy cosmic rays. It follows that scattering of charged energetic particles in intergalactic space must be sufficiently small in order to obtain contributions from sources as far away as even the nearest Fanaroff Riley class II radio galaxies. This implies a strong constraint on the turbulent magnetic field in intergalactic space.

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