  We investigate the three-dimensional, general relativistic Poynting-Robertson
effect in the case of rigidly rotating spherical source which emits radiation
radially in the local comoving frame. Such radiation field is meant to
approximate the field produced by the surface of a rotating neutron star, or by
the central radiating hot corona of accreting black holes; it extends the
purely radial radiation field that we considered in a previous study. Its
angular momentum is expressed in terms of the rotation frequency and radius of
the emitting source. For the background we adopt a Kerr spacetime geometry. We
derive the equations of motion for test particles influenced by such radiation
field, recovering the classical and weak-field approximation for slow rotation.
We concentrate on solutions consisting of particles orbiting along circular
orbits off and parallel to the equatorial plane, which are stabilized by the
balance between gravitational attraction, radiation force and PR drag. Such
solutions are found to lie on a critical hypersurface, whose shape may morph
from prolate to oblate depending on the Kerr spin parameter and the luminosity,
rotation and radius of the radiating sphere. For selected parameter ranges, the
critical hypersurface intersects the radiating sphere giving rise to a bulging
equatorial region or, alternatively, two lobes above the poles. We calculate
the trajectories of test particles in the close vicinity of the critical
hypersurface for a selected set of initial parameters and analyze the spatial
and angular velocity of test particles captured on the critical hypersurface.
