Cosmic-ray diffusion and the turbulent galactic magnetic field.
Abstract
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.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- April 1979
- DOI:
- 10.1093/mnras/187.1.23
- Bibcode:
- 1979MNRAS.187...23C
- Keywords:
-
- 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;
- Space Radiation;
- Cosmic Rays:Diffusion;
- Cosmic Rays:Galactic Magnetic Field;
- Galactic Magnetic Field:Turbulence