Kinetic theory of propagation and runaway galactic cosmic rays. 2: Self-consistent model

Details Kinetic theory of propagation and runaway galactic cosmic rays. 2: Self-consistent model Kinetic theory of propagation and runaway galactic cosmic rays. 2: Self-consistent model

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...281..937d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 281, no. 3, p. 937-944

Astronomy and Astrophysics

Astrophysics

11

Galactic Cosmic Rays, Galactic Halos, Kinetic Theory, Magnetohydrodynamics, Milky Way Galaxy, Turbulence, Astronomical Models, Cyclotron Resonance, Flux (Rate), Nonlinear Equations, Spatial Dependencies

Scientific paper

Nonlinear kinetic equations describing cosmic ray propagation in a scattering medium are analyzed. The scattering is determined by cosmic ray interaction with MHD-fluctuations. We consider a self-consistent model in the framework of MHD-wave excitation by the cosmic rays. Our investigations show that in the model the region in which cosmic rays are confined occurs naturally around the disk of cosmic ray sources if the particle energy is sufficiently small (less than 108 GeV for some model parameters). At the boundary the scattering is not effective giving rise to the runaway flux of cosmic rays. We define this region as the cosmic ray halo of the Galaxy. For higher particle energies the cosmic ray flux is not able to produce the MHD-turbulence needed for particle scattering and these particles freely leak out from the Galaxy. In the region of low energies the convective transport of particles in the halo may be important. However the runaway flux also arises at the boundary of the halo in this case.

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