Transport of relativistic nucleons in a galactic wind driven by cosmic rays.

Details Transport of relativistic nucleons in a galactic wind driven by cosmic rays. Transport of relativistic nucleons in a galactic wind driven by cosmic rays.

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...321..434p&link_type=abstract

Astronomy and Astrophysics, v.321, p.434-443

Astronomy and Astrophysics

Astrophysics

85

Cosmic Rays, Galaxy: Halo, Galaxies: Halos, Turbulence, Diffusion

Scientific paper

For the first time an attempt is made at a self-consistent analytical description of the halo structure and the propagation of energetic particles in late type galaxies like our own. Galactic CR are produced together with hot gas by sources deep in the disk. This leads to a galactic wind and magnetohydrodynamic fluctuations (excited by the cosmic-ray streaming instability) which in turn together determine the transport of these energetic particles into intergalactic space. Wave excitation is balanced locally by nonlinear Landau damping. The cosmic-ray transport equations for the dominant nucleons are solved in an approximate form analytically. Although fully nonlinear, the resulting picture is simple and corresponds to an overall spatial structure that extends to distances considerably greater than the radius of the galactic disk. The inferred source spectrum for cosmic-ray nucleons is a rather hard power law in energy, of index ~2.1. The observed abundances of secondary nuclei are also consistent with this model. The observed disk-halo transition at distances ~1kpc is an important part of the detailed picture in wich ion neutral friction damps short-scale magnetic fluctuations below that level.

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