Cosmic rays, supernova and the origin of ultrahigh energy particles

Details Cosmic rays, supernova and the origin of ultrahigh energy particles Cosmic rays, supernova and the origin of ultrahigh energy particles

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985stin...8621497c&link_type=abstract

Presented at the Symposium on Cosmogonical Processes, Boulder, Colo., 25 Mar. 1985

Astronomy and Astrophysics

Astrophysics

Astrophysics, Cosmic Rays, Particle Acceleration, Shock Waves, Supernovae, Compton Effect, Energy Spectra, Magnetic Flux, Stochastic Processes

Scientific paper

The acceleration of ultrahigh energy cosmic rays, greater than or equal to 10(15 to 20) eV, is still an unsolved problem in high-energy astrophysics. The now classical mechanism of stochastic acceleration of cosmic rays in a strong shock in the interstellar or intergalactic medium is limited in time and dimension for all likely acceleration sites, particularly for the highest energies. Acceleration of cosmic rays across a plasma shock of velocity, (BETA)/sub s/ ((BETA)/sub s/ = v/sub shock//c), requires 1/(BETA)/sub s/ number of crossings and therefore (1/(BETA)/sub s/) (2) number of scatterings for doubling the energy of a particle. This requires space of the order of 1/9BETA)/sub s/ x the scattering length, or a multiple of the Larmor radius and hence, the space requirements to cosmic ray acceleration are very many Larmor orbits in dimension, as well as times that are larger by (1/(BETA)/sub s/) (2) x t/sub Larmor/. The acceleration of cosmic rays by the shock in the envelope of a Type 1 supernova is reviewed, and the interaction of the accelerated matter with the nearby ISM is considered.

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