Solar MHD Turbulence in Regions with Various Levels of Flare Activity

Details Solar MHD Turbulence in Regions with Various Levels of Flare Activity Solar MHD Turbulence in Regions with Various Levels of Flare Activity

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002arep...46..161a&link_type=abstract

Astronomy Reports, Volume 46, Issue 2, February 2002, pp.161-171

Astronomy and Astrophysics

Astronomy

4

Scientific paper

The paper continues investigations of MHD turbulence in active solar regions. The statistical distributions of the increments (structure functions) of the turbulent field are studied analytically in the context of a refined Kolmogorov theory of turbulence. Since photospheric transport of the B z component of the magnetic field is quite similar to that of a scalar field in a turbulent flow, the theory of transport of a passive scalar can be applied. This approach enables us to show that the structure functions are determined by the competition between the dissipation of the magnetic and kinetic energies and to obtain a number of relations between the structure-function parameters and energy characteristics of the MHD turbulence. Taking into account general conclusions that can be drawn on the basis of the refined Kolmogorov turbulence theory, the structure functions of the B z field are calculated for eight active regions (from measurements of SOHO/MDI and the Huairou Solar Observing Station, China). These calculations show that the behavior of the structure functions is different for the B z field of each active region. The energy-dissipation index of the fluctuation spectrum (which is uniquely determined by the structure functions) is closely related to the level of flare activity: the more activity, the less steep the dissipation spectrum for a given active region. This provides a means to test and, consequently, forecast the flare activity of active regions.

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