  This paper describes an application of the Mathisson-Papapetrou-Dixon (MPD)
equations in analytic perturbation form to the case of circular motion around a
radially accreting or radiating black hole described by the Vaidya metric.
Based on the formalism presented earlier, this paper explores the effects of
mass accretion or loss of the central body on the overall dynamics of the
orbiting spinning particle. This includes changes to its squared mass and spin
magnitude due to the classical analog of radiative corrections from
spin-curvature coupling. Various quantitative consequences are explored when
considering orbital motion near the black hole's event horizon. An analysis on
the orbital stability properties due to spin-curvature interactions is examined
briefly, with conclusions in general agreement with previous work performed for
the case of circular motion around a Kerr black hole.
