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Abstract <p>The problem of diffusive propagation of cosmic rays (CRs) with a general tensor in a model homogeneous magnetic field of the Galaxy has been solved, and its stability has been investigated. An algorithm for generating stencils of second-order accuracy finite-difference schemes for a three-dimensional differential equation with tensor components is implemented. The components of the diffusion tensor are calculated with a specified spatial step and are determined based on the magnitudes of the large-scale magnetic field vector and the magnitude of the random field component, which is assumed to be 6 <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11972_2025_8787_Article_IEq1.gif" Format="GIF" Height="12" Rendition="HTML" Resolution="72" Type="Linedraw" Width="15" /> </InlineMediaObject> <EquationSource Format="TEX">\(\mu\)</EquationSource> <!--BPhysMGU2570040Borisov-m1--> </InlineEquation>G. The study demonstrates the fundamental possibility of determining the energy spectra of CRs in various regions of the Galaxy, where the free parameters are the distribution of CR sources and the structure of the magnetic field.</p>

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Numerical Model of Cosmic Ray Propagation in the Anisotropic Magnetic Field of the Galaxy

  • 期刊论文

  • 发表日期：

    2025年4月1日

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  • V. D. Borisov,
  • V. O. Yurovsky,
  • I. A. Kudryashov

摘要

Abstract

The problem of diffusive propagation of cosmic rays (CRs) with a general tensor in a model homogeneous magnetic field of the Galaxy has been solved, and its stability has been investigated. An algorithm for generating stencils of second-order accuracy finite-difference schemes for a three-dimensional differential equation with tensor components is implemented. The components of the diffusion tensor are calculated with a specified spatial step and are determined based on the magnitudes of the large-scale magnetic field vector and the magnitude of the random field component, which is assumed to be 6 \(\mu\) G. The study demonstrates the fundamental possibility of determining the energy spectra of CRs in various regions of the Galaxy, where the free parameters are the distribution of CR sources and the structure of the magnetic field.