Enhancement and Suppression of Heat Transfer by MHD Turbulence

By A. Lazarian. 2006

146 citations recorded by the source corpus.

We study the effect of turbulence on heat transfer within magnetized plasmas for energy injection velocities both larger and smaller than the Alfvén speed. We find that in the latter regime the heat transfer is partially suppressed, while in the former regime the effects of turbulence depend on the intensity of driving. In fact, the scale lA at which the turbulent velocity is equal to the Alfvén velocity is an important new parameter. When the electron mean free path λ is larger than lA, the stronger the turbulence, the lower the thermal conductivity by electrons. The turbulent motions, however, induce their own advective heat transport, which, for the parameters of intracluster medium, provides effective heat diffusivity that exceeds the classical Spitzer value.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/25756cc72cdf5fa1233c12ae5b8868aaa6b64714

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In Nuclear and High Energy Physics

Citations in the corpus

PICO: Probe of Inflation and Cosmic Origins (2019, background): “Key processes in the diffuse ISM, including heat transport, streaming of cosmic rays, and magnetic reconnection depend strongly on the level of the environment’s magnetization [172–174].”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, background): “…the theoretical viewpoint, turbulence may have a deep impact on the physics of the ICM (e.g. Narayan & Medvedev 2001; Shekochihin et al 2005, 2010; Lazarian 2006; Ruszkowsky & Peng 2010) and on the properties of non-thermal components in galaxy clusters (e.g. Subramanian et al. 2006; Brunetti &…”
Feedback heating by cosmic rays in clusters of galaxies (2007, background): “In reality, both electron conduction and turbulent mixing may contribute to heat transport in clusters (for a comprehensive discussion, see Lazarian 2006).”
Cosmic-Ray Propagation: Nonlinear Diffusion Parallel and Perpendicular to Mean Magnetic Field (2007, methodology): “We found, that similar to the case of thermal diffusion discussed in Lazarian (2006), the diffusion of CRs depends on the Alfvénic Mach number MA.”
Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “…and the Transit-Time Damping (TTD) (Chandran 2000; Yan & Lazarian 2002, 2004; Farmer & Goldreich 2004; Cassano & Brunetti 2005) as well as the non-resonance acceleration of cosmic rays by large scale compressible motions (see Ptuskin 1988, Chandran 2003, Cho & Lazarian 2006) has been altered.”
Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, methodology): “MHD turbulence theory seriously advanced in the last decades also affecting our view of particle acceleration in astrophysical plasmas (e.g. Chandran 2000; Yan & Lazarian 2002; Lazarian 2006a and ref therein).”