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2002•arXiv (Cornell University)Open access

The Properties of Compressible MHD and Cosmic Ray Transport

A. Lazarian, Jungyeon Cho, Huirong Yan

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Abstract

Turbulence is the most common state of astrophysical flows. In typical astrophysical fluids, turbulence is accompanied by strong magnetic fields, which has a large impact on the dynamics of the turbulent cascade. Recently, there has been a significant breakthrough on the theory of magnetohydrodynamic (MHD) turbulence. For the first time we have a scaling model that is supported by both observations and numerical simulations. We review recent progress in studies of both incompressible and compressible turbulence. We compare Iroshnikov-Kraichnan and Goldreich-Sridhar models, and discuss scalings of Alfven, slow, and fast waves. We discuss the implications of this new insight into MHD turbulence for cosmic ray transport.

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Turbulence is the most common state of astrophysical flows. In typical astrophysical fluids, turbulence is accompanied by strong magnetic fields, which has a large impact on the dynamics of the turbulent cascade. Recently, there has been a significant breakthrough on the theory of magnetohydrodynamic (MHD) turbulence. For the first time we have a scaling model that is supported by both observations and numerical simulations. We review recent progress in studies of both incompressible and compressible turbulence. We compare Iroshnikov-Kraichnan and Goldreich-Sridhar models, and discuss scalings of Alfven, slow, and fast waves. We discuss the implications of this new insight into MHD turbulence for cosmic ray transport.

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Available abstract

Turbulence is the most common state of astrophysical flows. In typical astrophysical fluids, turbulence is accompanied by strong magnetic fields, which has a large impact on the dynamics of the turbulent cascade. Recently, there has been a significant breakthrough on the theory of magnetohydrodynamic (MHD) turbulence. For the first time we have a scaling model that is supported by both observations and numerical simulations. We review recent progress in studies of both incompressible and compressible turbulence. We compare Iroshnikov-Kraichnan and Goldreich-Sridhar models, and discuss scalings of Alfven, slow, and fast waves. We discuss the implications of this new insight into MHD turbulence for cosmic ray transport.

Key concepts: Magnetohydrodynamic turbulence, Magnetohydrodynamics, Turbulence, Physics, Magnetohydrodynamic drive, Compressibility, Energy cascade, K-omega turbulence model

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