Studying the relative position of magnetic lines of a two-component random magnetic field

Galactic cosmic rays play an important role in cosmic physics. Despite numerous studies in the field of the magnetic fields of the Galaxy, the understanding of the structure of magnetic lines remains insufficient for predicting the trajectories of high-energy cosmic particles in various configurations of galactic magnetic fields. In this work, the magnetic field is studied numerically by constructing its two-component model and its further qualitative and statistical analysis. At a qualitative level, the results of modeling a random isotropic field, where the magnetic lines are located close to each other, are presented. In this case, a regular structure is observed (see Section 2.2). It is shown that when simulating an isotropic random field, a diffusion mode of motion is observed. When a regular component of a certain intensity is added, the longitudinal mode of transport becomes ballistic.