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Numerical testing of mirror diffusion of cosmic rays
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abstract
The tension between recent observations and theories on cosmic ray (CR) diffusion necessitates exploration of new CR diffusion mechanisms. We perform the first numerical study on the mirror diffusion of CRs that is recently proposed by Lazarian & Xu (2021). We demonstrate that the perpendicular superdiffusion of turbulent magnetic fields and magnetic mirroring that naturally arise in magnetohydrodynamic (MHD) turbulence are the two essential physical ingredients for the mirror diffusion to happen. In supersonic, subsonic, and incompressible MHD turbulence, with the pitch angles of CRs repeatedly crossing $90^\circ$ due to the mirror reflection, we find that the mirror diffusion strongly enhances the confinement of CRs, and their pitch-angle-dependent parallel mean free path can be much smaller than the injection scale of turbulence. With the stochastic change of pitch angles due to gyroresonant scattering, CRs stochastically undergo slow mirror diffusion at relatively large pitch angles and fast scattering diffusion at smaller pitch angles, resulting in a L\'{e}vy-flight-like propagation.
Forward citations
Cited by 2 Pith papers
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Sub-sonic compressible magnetohydrodynamic turbulence I. Alfv\'enic and fast-magnetosonic injection, amplitude dependence, and compressibility effects
In decaying sub-sonic MHD turbulence simulations, the amplitude and plasma beta, not the injection wave type, set the turbulent density fluctuation level, while curvature and mirror statistics change dramatically with...
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Superdiffusion of cosmic rays in the vicinity of their accelerators and the resulting $\gamma$-ray emission
Superdiffusion produces constant or r^{α-3} CR radial profiles near sources; the associated γ-ray morphology can distinguish it from normal diffusion with IACTs.
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