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Diffusion of Particles, Heat and Magnetic Fields in Compressible Turbulent Media

Published online by Cambridge University Press:  12 April 2016

A.Z. Dolginov  and
N.A. Silant’ev
A.Z. Dolginov
Affiliation:
A.I.Ioffe Phys.-Tech. Institute, Academy of Sciences of USSR, 194021 Leningrad, USSR
N.A. Silant’ev
Affiliation:
A.I.Ioffe Phys.-Tech. Institute, Academy of Sciences of USSR, 194021 Leningrad, USSR

Abstract

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A new method for the calculation of kinetic coefficients is presented. This method allows us to obtain the distribution of scalar and vector fields (such as the temperature, the admixture particle number density and the magnetic field) in turbulent cosmic media with any value of S = u0т0/R0. The explicit expression for the “turbulent” diffusivity DT is obtained. In some cases DT becomes negative, implying the clustering of the admixture particles in patches (a local increase of the temperature and magnetic fields). The magnetic α-effect is considered for the case S ~ 1.

Type
Part I Convection and turbulence as the basis of magnetic activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 71 - 74
Copyright
Copyright © Springer-Verlag 1991

References

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Dolginov, A.Z., Silant’ev, N.A.: 1990, Astron. Astrophys. Google Scholar
Dolginov, A.Z., Silant’ev, N.A.: 1991, Geoph. Astroph. Fluid Dynamics (submitted)Google Scholar
Silant’ev, N.A., Korolkov, M.D.: 1990, Astron. Nachr. 311, 107 Google Scholar
Silant’ev, N.A.: 1988, Proc. Int. Meet, on “Physics and Evolution of Stars”, Leningrad, Nauka Google Scholar