  Stellar dynamos are driven by complex couplings between rotation and
turbulent convection, which drive global-scale flows and build and rebuild
stellar magnetic fields. When stars like our sun are young, they rotate much
more rapidly than the current solar rate. Observations generally indicate that
more rapid rotation is correlated with stronger magnetic activity and perhaps
more effective dynamo action. Here we examine the effects of more rapid
rotation on dynamo action in a star like our sun. We find that vigorous dynamo
action is realized, with magnetic field generated throughout the bulk of the
convection zone. These simulations do not possess a penetrative tachocline of
shear where global-scale fields are thought to be organized in our sun, but
despite this we find strikingly ordered fields, much like sea-snakes of
toroidal field, which are organized on global scales. We believe this to be a
novel finding.
