Interstellar turbulence and the kinetics of cosmic rays

Details Interstellar turbulence and the kinetics of cosmic rays Interstellar turbulence and the kinetics of cosmic rays

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982izssr..46.1659b&link_type=abstract

(Vsesoiuznaia Konferentsiia po Kosmicheskim Lucham, Samarkand, Uzbek SSR, Oct. 27-29, 1981.) Akademiia Nauk SSSR, Izvestiia, Ser

Physics

1

Cosmic Rays, Interstellar Gas, Particle Motion, Gas Dynamics, Heavy Nuclei, Molecular Clouds, Power Spectra, Supernova Remnants, Turbulent Flow

Scientific paper

A model of cosmic-ray acceleration is proposed. According to this model, the acceleration of cosmic-ray nuclei and the formation of the power spectrum occurs in hot coronal gas under the effect of large-scale turbulence and shock waves. The injection of primary nuclei with energies of approximately 1 GeV occurs at the shock fronts due to the destruction of dust particles, insofar as enrichment with heavy nuclei is necessary. The secondary nuclei are generated in molecular clouds, and are then injected into interstellar 'tunnels' (formed as a result of the intersection of supernova remnants), where they are accelerated by large-scale turbulence.

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