Effective potential and geodesic motion in Kerr-de Sitter space-time
  In the present work, geodesic trajectories in Kerr-de Sitter geometry is
analyzed. From the mathematical solution of Lagrangian formalism appropriate to
motions in the equatorial plane (for which 'theta' = 0 and 'theta' =
(constant)= pi/2) can give potential energy of massive and massless particles
for rotating axisymetric black hole. From this, for a particular value of
cosmological constant, Kerr parameter, mass, angular momentum and impact
parameter; variation of potential with distance can be found. Similarly, for a
particular value of cosmological constant, mass and Kerr parameter; variation
of velocity with distance can be found.
