Line-of-sight magnetograms for 217 active regions ( ARs ) of different flare rate observed at the solar disk center from January 1997 until December 2006 are utilized to study the turbulence regime and its relationship to the flare productivity .
Data from SOHO /MDI instrument recorded in the high resolution mode and data from the BBSO magnetograph were used .
The turbulence regime was probed via magnetic energy spectra and magnetic dissipation spectra .
We found steeper energy spectra for ARs of higher flare productivity .
We also report that both the power index , \alpha , of the energy spectrum , E ( k ) \sim k ^ { - \alpha } , and the total spectral energy W = \int E ( k ) dk are comparably correlated with the flare index , A , of an active region .
The correlations are found to be stronger than that found between the flare index and total unsigned flux .
The flare index for an AR can be estimated based on measurements of \alpha and W as A = 10 ^ { b } ( \alpha W ) ^ { c } , with b = -7.92 \pm 0.58 and c = 1.85 \pm 0.13 .
We found that the regime of the fully-developed turbulence occurs in decaying ARs and in emerging ARs ( at the very early stage of emergence ) .
Well-developed ARs display under-developed turbulence with strong magnetic dissipation at all scales .