By Andreas Shalchi
This booklet offers with the physics of cosmic ray diffusion thought, concentrating on the physics of nonlinear delivery of cosmic rays via turbulent interplanetary or interstellar plasma.
The writer discusses primary approaches equivalent to cosmic ray propagation and acceleration within the sun procedure or in interstellar area, the houses of such plasmas, the normal quasilinear method of describing plasma-particle interactions in addition to a number of extra actual nonlinear theories. inside a nonlinear therapy he revisits the mechanism of diffusive surprise acceleration, that is chargeable for the excessive cosmic ray energies. in response to new effects provided during this ebook the writer proposes destiny numerical, theoretical and observational learn which may develop the sector of cosmic ray diffusion theory.
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In Fig. 4, the results are compared with the analytical approximations. 30)) Z 2 lc;slab ıBslab D 1 0 slab dz R? 2 0 lc,slab 1 2 3 4 5 z /lslab 2 Fig. 4 The slab-correlation function R? =ıBslab for D 5=6 as a function of the parallel position z= lslab . Shown are numerical results (solid line) and the analytical approximation for z lslab 2 (dotted line). For z D 0 we have R? D ıBslab . 33), we finally find Z 2 lc;slab ıBslab 1 D 0 slab 2 dz R? z/ D 2 C. 47) Obviously, the correlation length for the used spectrum is related to the slab bendover scale through lc;slab D 2 C.
In this chapter, it is demonstrated that the turbulence geometry, the wave spectrum, and the temporal behavior of these fields have to be specified. For the geometry, we employ the so-called slab/2D composite model, which is often used to approximate solar wind turbulence. Correlation functions for slab, pure 2D, and composite turbulence models are calculated, as well as field line diffusion coefficients. Although for slab geometry, the field line random walk can be described linearly, for more realistic models, a nonlinear formulation has to be applied.
7, the different observations for perpendicular mean free paths are shown and can easily be compared with each other. One of the goals of cosmic ray transport theories is to reproduce the observed mean free paths visualized in Figs. 7. It will be demonstrated in Chap. 8 that advanced models for the turbulence and nonlinear transport theories are necessary to explain these measurements. 2 Transport in the Interstellar Medium The properties of cosmic rays, their composition, and their interaction with the interstellar medium are discussed in Schlickeiser (2002).