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- W1666822040 endingPage "98" @default.
- W1666822040 startingPage "56" @default.
- W1666822040 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 Alfvén, slow, and fast waves. We also discuss the completely new regime of MHD turbulence that happens below the scale at which hydrodynamic turbulent motions are damped by viscosity. In the case of the partially ionized diffuse interstellar gas the viscosity is due to neutrals and truncates the turbulent cascade at ~parsec scales. We show that below this scale magnetic fluctuations with a shallow spectrum persist and discuss the possibility of a resumption of the MHD cascade after ions and neutrals decouple. We discuss the implications of this new insight into MHD turbulence for cosmic ray transport, grain dynamics, etc., and how to test theoretical predictions against observations." @default.
- W1666822040 created "2016-06-24" @default.
- W1666822040 creator A5018242289 @default.
- W1666822040 creator A5026085924 @default.
- W1666822040 creator A5028300061 @default.
- W1666822040 date "2003-01-01" @default.
- W1666822040 modified "2023-09-24" @default.
- W1666822040 title "MHD Turbulence: Scaling Laws and Astrophysical Implications" @default.
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