  We analyse and determine the effects of modest progenitor rotation in the
context of core-collapse supernovae by comparing two separate long-duration
three-dimensional simulations of 9 M$_{\odot}$ progenitors, one rotating with
an initial spin period of $\sim$60 seconds and the other non-rotating. We
determine that both models explode early, though the rotating model explodes a
bit earlier. Despite this difference, the asymptotic explosion energies
($\sim$10$^{50}$ ergs) and residual neutron star baryon masses ($\sim$1.3
M$_{\odot}$) are similar. We find that the proto-neutron star (PNS) core can
deleptonize and cool significantly more quickly. Soon into the evolution of the
rotating model, we witness more vigorous and extended PNS core convection that
early in its evolution envelopes the entire inner sphere, not just a shell.
Moreover, we see a corresponding excursion in both the $\nu_e$ luminosity and
gravitational-wave strain that may be diagnostic of this observed dramatic
phenomenon. In addition, after bounce the innermost region of the rotating
model seems to execute meridional circulation. The rotationally-induced growth
of the convective PNS region may facilitate the growth of core B-fields by the
dynamo mechanism by facilitating the achievement of the critical Rossby number
condition for substantial growth of a dipole field, obviating the need for
rapid rotation rates to create dipole fields of significance. The next step is
to explore the progenitor-mass and spin dependencies across the progenitor
continuum of the supernova explosion, dynamics, and evolution of PNS convection
and its potential role in the generation of magnetar and pulsar magnetic
fields.
