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Formation of the cosmic-ray halo: The role of nonlinear Landau damping

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arxiv 2209.12302 v1 pith:O7MTVHEY submitted 2022-09-25 astro-ph.GA

Formation of the cosmic-ray halo: The role of nonlinear Landau damping

D. O. Chernyshov , V. A. Dogiel , A. V. Ivlev , A. D. Erlykin , A. M. Kiselev This is my paper
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keywords halodampingnonlinearexcitationlandaupropagationregionssize
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We present a nonlinear model of self-consistent Galactic halo, where the processes of cosmic ray (CR) propagation and excitation/damping of MHD waves are included. The MHD-turbulence, which prevents CR escape from the Galaxy, is entirely generated by the resonant streaming instability. The key mechanism controlling the halo size is the nonlinear Landau (NL) damping, which suppresses the amplitude of MHD fluctuations and, thus, makes the halo larger. The equilibrium turbulence spectrum is determined by a balance of CR excitation and NL damping, which sets the regions of diffusive and advective propagation of CRs. The boundary $z_{cr}(E)$ between the two regions is the halo size, which slowly increases with the energy. For the vertical magnetic field of $\sim 1~\mu G$, we estimate $z_{cr} \sim 1$ kpc for GeV protons. The derived proton spectrum is in a good agreement with observational data.

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Cited by 2 Pith papers

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  1. Charge-dependent spectral softenings of primary cosmic-rays below the knee

    astro-ph.HE 2025-11 conditional novelty 7.0

    Direct measurements reveal charge-dependent spectral softenings in primary cosmic rays at a common rigidity of ~15 TV, rejecting mass-dependent softening at >99.999% confidence.

  2. Implication of multiple source populations of Galactic cosmic rays from proton and helium spectra

    astro-ph.HE 2025-11 conditional novelty 5.0

    The proton and helium spectra from 1 GeV to 10 PeV can be reproduced only by adding two local sources or a second background population on top of the standard cosmic-ray background.