Abstract
Cosmic ray (CR) transport and acceleration are determined by the properties of magnetic turbulence. Recent advances in MHD turbulence call for revisions in the paradigm of cosmic ray transport. We use the models of magnetohydrodynamic turbulence that were tested in numerical simulation, in which turbulence is injected at large scale and cascades to small scales. We shall address the issue of the transport of CRs, both parallel and perpendicular to the magnetic field. Both normal diffusion on large scales and superdiffusion on small scales shall be addressed. We shall demonstrate compressible fast modes are the dominant cosmic ray scatterer from both quasilinear and nonlinear theories. We shall also show that the self-generated wave growth by CRs is constrained by preexisting turbulence and discuss the process in detail in the context of shock acceleration at supernova remnants and their implications. In addition, we shall dwell on the nonlinear growth of kinetic gyroresonance instability of cosmic rays induced by large scale compressible turbulence. The feedback of the instability on large scale turbulence should be included in future simulations.
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Notes
- 1.
The comparison was done with the resonant term in Chandran (2000) as the nonresonant term is spurious.
- 2.
On the basis of weak turbulence theory, Chandran (2005) has argued that high-frequency fast waves, which move mostly parallel to magnetic field, generate Alfvén waves also moving mostly parallel to magnetic field. We expect that the scattering by thus generated Alfvén modes to be similar to the scattering by the fast modes created by them. Therefore we expect that the simplified approach adopted in Yan and Lazarian (2004) and the papers that followed to hold.
- 3.
The parameters of idealized interstellar phases are a subject of debate. Recently, even the entire concept of the phase being stable entities has been challenged (see Gazol et al. 2007; and ref. therein). Indeed different parts of interstellar medium can exhibit variations of these parameters (see Wolfire et al. 2003; and ref. therein).
- 4.
- 5.
We neglect the nonlinear Landau damping, which is suppressed in turbulence due to decrease of mean free path.
- 6.
The effective B 0 is therefore renormalized and can be much larger than the typical field in ISM (see, e.g., Diamond and Malkov 2007).
- 7.
The factor 1/4 arises from the following reason. As pointed out by Ostrowski and Schlickeiser (1996), the spectrum is steepened for small l, i.e., \(lU/D(p) \sim < 4\).
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Yan, H. (2015). Cosmic Ray Transport in Turbulent Magnetic Field. In: Lazarian, A., de Gouveia Dal Pino, E., Melioli, C. (eds) Magnetic Fields in Diffuse Media. Astrophysics and Space Science Library, vol 407. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-44625-6_10
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