  Recent data from the Kepler mission has revealed the occurrence of
superflares in sun-like stars which exceed by far any observed solar flares in
release of energy. A natural idea is that the dynamo mechanism in superflaring
stars differs in some respect from that in the Sun. We search for a difference
in the dynamo-related parameters between superflaring stars and the Sun to
suggest a dynamo-mechanism as close as possible to the conventional
solar/stellar dynamo but capable of providing much higher magnetic energy.
Dynamo based on joint action of differential rotation and mirror asymmetric
motions can in principle result in excitation of two types of magnetic fields.
First of all, it is well-known in solar physics dynamo waves. The point is that
another magnetic configuration with initial growth and further stabilisation is
also possible for excitation. For comparable conditions, magnetic field
strength of second configuration is much larger rather of the first one just
because dynamo do not spend its efforts for periodic magnetic field inversions
but use its for magnetic field growth. We analysed available data from the
Kepler mission concerning the superflaring stars in order to find tracers of
anomalous magnetic activity. Starting from the recent paper, we find that
anti-solar differential rotation or anti-solar sign of the mirror-asymmetry of
stellar convection can provide the desired strong magnetic field in dynamo
models. We confirm this concept by numerical models of stellar dynamos with
corresponding governing parameters. We conclude that the proposed mechanism can
plausibly explain the superflaring events at least for some cool stars,
including binaries, subgiants and, possibly, low-mass stars and young rapid
rotators.
