  We present results from four convectively-driven stellar dynamo simulations
in spherical wedge geometry. All of these simulations produce cyclic and
migrating mean magnetic fields. Through detailed comparisons we show that the
migration direction can be explained by an $\alpha\Omega$ dynamo wave following
the Parker--Yoshimura rule. We conclude that the equatorward migration in this
and previous work is due to a positive (negative) $\alpha$ effect in the
northern (southern) hemisphere and a negative radial gradient of $\Omega$
outside the inner tangent cylinder of these models. This idea is supported by a
strong correlation between negative radial shear and toroidal field strength in
the region of equatorward propagation.
