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

TL;DR

This paper provides a theoretical derivation of the perpendicular cosmic ray diffusion coefficient in the starburst galaxy NGC 253, aligning with recent observational estimates and advancing understanding of cosmic ray propagation in external galaxies.

Contribution

It introduces an advanced analytical theory to reproduce the perpendicular diffusion coefficient in NGC 253, bridging the gap between observational data and theoretical modeling.

Findings

Theoretical value matches recent observational estimates.

Demonstrates the applicability of advanced analytical models to external galaxies.

Enhances understanding of cosmic ray transport in starburst environments.

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.