Long-Time Behaviour of MHD Shell Models

Details Long-Time Behaviour of MHD Shell Models Long-Time Behaviour of MHD Shell Models

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ptep.proc..190f&link_type=abstract

Plasma Turbulence and Energetic Particles in Astrophysics, Proceedings of the International Conference, Cracow (Poland), 5-10 Se

Astronomy and Astrophysics

Astrophysics

Scientific paper

We demonstrate in the framework of a MHD-shell model that the final stage of turbulent dynamo depends on turbulence nature. For free-decaying turbulence the final stage is achieved after several tens of turnover times and characterized by a statistical equipartition of kinetic and magnetic energy under low cross-correlation. The evolution of forced turbulence is much more complicated. After a long metastable stage (a few hundreds of turnover times) characterized by the Kolmogorov spectral index ``-5/3'' and low cross-correlation, a change to a state with high correlation between magnetic and velocity fields takes place. This state is described by the steep spectra and weak spectral energy flux which causes an increase in total energy of the MHD system.

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