  We investigate the properties of Type IIP supernovae that are dominantly
powered by the rotational kinetic energy of the newly born neutron star. While
the spin-down of a magnetar has previously been proposed as a viable energy
source in the context of super-luminous supernovae, we show that a similar
mechanism could produce both normal and peculiar Type IIP supernova light
curves from red supergiant progenitors for a range of initial spin periods and
equivalent dipole magnetic field strengths. Although the formation channel for
such magnetars in a typical red supergiant progenitor is unknown, it is
tantalizing that this proof of concept model is capable of producing ordinary
Type IIP lightcurve properties, perhaps implying that rotation rate and
magnetic field strength may play important roles in some ordinary looking Type
IIP supernova explosions.
