  Ellipticals in very low density environments are extremely rare but hold
important clues about galaxy formation and evolution. In this paper we continue
our study of isolated elliptical galaxies, presenting results on the radial
stellar kinematics for 13 isolated early-type galaxies. We derive radial
rotation velocity, velocity dispersion and hermite terms to ~1 effective
radius. We observe a dichotomy in kinematic properties similar to that in the
elliptical population as a whole, where low luminosity ellipticals tend to be
rotationally supported. For all galaxies the V/sigma ratio increases with
radius. We find kinematically distinct cores (KDCs), or velocity substructure,
in ~40% of the galaxies for which we have major axis spectra. Such a fraction
is similar to that observed for ellipticals in higher density environments.
Most galaxies in the sample reveal kinematic evidence for a nuclear disk. The
non-relaxed kinematics in several galaxies suggests that they have undergone a
merger or accretion event. Isolated ellipticals generally follow the
fundamental plane defined by cluster ellipticals -- exceptions being those
galaxies with evidence for young stellar populations. Overall, we find isolated
ellipticals have similar kinematic properties to their counterparts in higher
density environments.
