Theoretical Explanation of the Cosmic Ray Perpendicular Diffusion Coefficient in the Nearby Starburst Galaxy NGC 253

Abstract

Diffusion coefficients are usually used to describe the propagation of Cosmic Rays through the Universe. Whereas such transport parameters can be obtained from experiments in the Solar System, it is difficult to determine diffusion coefficients in the Milky Way or in external galaxies. Recently a value for the perpendicular diffusion coefficient in the nearby starburst halaxy NGC 253 has been proposed. In the present paper we reproduce this value theoretically by using an advanced analytical theory for perpendicular diffusion.

5 pages, 2 figures

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• CHANG-ES XVI: An in-depth view of the cosmic-ray transport in the edge-on spiral galaxies NGC 891 and NGC 4565
• Investigation of the cosmic ray population and magnetic field strength in the halo of NGC 891
• The radio continuum perspective on cosmic-ray transport in external galaxies
• Modelling the cosmic ray electron propagation in M 51
• The magnetic field structure of the central region in M31
• Perpendicular diffusion of energetic particles in noisy reduced magnetohydrodynamic turbulence
• Anisotropic cosmic-ray diffusion in isotropic Kolmogorov turbulence
• The impact of a young radio galaxy: clues from the cosmic-ray electron population
• The implicit contribution of slab modes to the perpendicular diffusion coefficient of particles interacting with two-component turbulence