  Accurately modeling astrophysical extreme-mass-ratio-insprials requires
calculating the gravitational self-force for orbits in Kerr spacetime. The
necessary calculation techniques are typically very complex and, consequently,
toy scalar-field models are often developed in order to establish a particular
calculational approach. To that end, I present a calculation of the
scalar-field self-force for a particle moving on a (fixed) inclined circular
geodesic of a background Kerr black hole. I make the calculation in the
frequency-domain and demonstrate how to apply the mode-sum regularization
procedure to all four components of the self-force. I present results for a
number of strong-field orbits which can be used as benchmarks for emerging
self-force calculation techniques in Kerr spacetime.
