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This study investigates whether the "knee" feature observed in the cosmic ray energy spectrum around PeV energies can be explained by a transition from diffusion-dominated to drift-dominated particle transport in the Galaxy's magnetic field. Using test-particle simulations in various magnetic field configurations, the researchers find that drift effects can produce a knee only under specific conditions: either in purely azimuthal fields (though this fails to match observed grammage data) or when the parallel diffusion coefficient becomes energy-independent above 1 TeV in more realistic field configurations. The results suggest that magnetic field topology and the interplay between diffusion and drift mechanisms are critical for understanding high-energy cosmic ray propagation.
Why it matters
Understanding the origin of the knee in the cosmic ray spectrum is fundamental to particle astrophysics, as it constrains models of cosmic ray acceleration, propagation, and confinement in our Galaxy. This work provides testable predictions about Galactic magnetic field structure that could be verified with improved cosmic ray composition measurements at PeV energies.
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⚠️ Preprint – Noch nicht peer-reviewed
Dieser Artikel wurde noch nicht von unabhängigen Experten begutachtet. Die Ergebnisse sind vorläufig und sollten mit Vorsicht interpretiert werden.
Abstract: In a magnetic field with a complex topology, as can be the Galactic magnetic field, cosmic ray transport cannot simply be described by diffusion parallel and perpendicular to magnetic field lines, because the gradients and curvature of the large-scale magnetic field induce drift motions. These effects become especially important at high energies. Here we revisit the possibility that the competition between diffusion and drifts may lead to a knee in the cosmic ray spectrum. We carry out test-particle simulations of cosmic ray transport in a mock Galactic magnetic field made of a regular large scale component, with a non-trivial topology and a homogeneous and isotropic turbulent magnetic field, with a spectrum that is assumed to be Kolmogorov-like in the basic setup. These simulations are used to infer the escape time and the grammage accumulated by cosmic rays with energy in the TeV–10 PeV energy range. In the case of a large scale magnetic field with a purely azimuthal structure, the drift due to the curvature of magnetic field lines produces a knee in the PeV range, but the model fails to reproduce the grammage, due to the exceedingly low value of the perpendicular diffusion coefficient. If the large scale magnetic field acquires a component perpendicular to the Galactic disc, the parallel diffusion coefficient becomes quickly dominant in terms of particle escape, and drifts are unable to compete. A knee structure does not appear in such a scenario. However, if the parallel diffusion coefficient becomes energy independent at $Egtrsim 1$ TeV, a knee may arise around PeV energies due to drift dominance. We discuss two cases in which this situation may occur.
Source: Transition from Diffusion to Drift-Dominated Cosmic Ray Transport and the Origin of the Knee