  Obtaining observational evidence of the turbulent component of solar dynamo
operating in the convective zone is a challenging problem because the dynamo
action is hidden below the photosphere. Here we present results of a
statistical study of flaring active regions (ARs) that produced strong solar
flares of an X-ray class X1.0 and higher during a time period that covered
solar cycles 23 and 24. We introduced a magneto-morphological classification
(MMC) of ARs, which allowed us to estimate possible contribution of the
turbulent component of the dynamo into the structure of an AR. We found that in
72\% of cases, flaring ARs do not comply with the empirical laws of the global
dynamo (frequently they are not bipolar ARs, or, if they are, they violate
either Hale polarity law, or the Joy's law, or the leading sunspot prevalence
rule), which may be attributed to the influence of the turbulent dynamo action
inside the convective zone on spatial scales of typical ARs. Thus it appears
that the flaring is governed by the turbulent component of solar dynamo. A
contribution into the flaring from these ARs-``violators'' is enhanced during
the second maximum and the descending phase of a solar cycle, when the toroidal
field weakens and the influence of the turbulent component becomes more
pronounced. These observational findings are in consensus with a concept of the
essential role of non-linearities and turbulent intermittency in the magnetic
fields generation inside the convective zone, which follows from simulations of
dynamo.
