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Line-of-sight magnetograms for 217 active regions (ARs) of different flarerate observed at the solar disk center from January 1997 until December 2006are utilized to study the turbulence regime and its relationship to the flareproductivity. Data from {\it SOHO}/MDI instrument recorded in the highresolution mode and data from the BBSO magnetograph were used. The turbulenceregime was probed via magnetic energy spectra and magnetic dissipation spectra.We found steeper energy spectra for ARs of higher flare productivity. We alsoreport that both the power index, $\alpha$, of the energy spectrum, $E(k) \simk^{-\alpha}$, and the total spectral energy $W=\int E(k)dk$ are comparablycorrelated with the flare index, $A$, of an active region. The correlations arefound to be stronger than that found between the flare index and total unsignedflux. 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 indecaying ARs and in emerging ARs (at the very early stage of emergence).Well-developed ARs display under-developed turbulence with strong magneticdissipation at all scales.

Magnetic Energy Spectra in Active Regions