Cosmic-ray diffusion and the turbulent galactic magnetic field

Details Cosmic-ray diffusion and the turbulent galactic magnetic field Cosmic-ray diffusion and the turbulent galactic magnetic field

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.187...23c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 187, Apr. 1979, p. 23-40.

Astronomy and Astrophysics

Astronomy

2

Cosmic Rays, Diffusion Coefficient, Dynamo Theory, Interstellar Magnetic Fields, Particle Diffusion, Galactic Structure, Gamma Ray Astronomy, H Ii Regions, Radiation Distribution, Supernova Remnants, Velocity Distribution

Scientific paper

Lerche's (1971) turbulent kinematic-dynamo equations are used to calculate the mean-square displacement of the fluctuating component of the galactic magnetic field and hence the cosmic-ray diffusion coefficient. It is found that the radial variation of the diffusion coefficient thus calculated agrees well with that deduced from gamma-ray observations, provided a mean velocity field is used which includes a compressional component, which, according to Burton (1976), is also responsible for the observed peaking of H II regions, CO, supernova remnants, and gamma-rays at about 6 kpc from the Galactic Center.

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