Relativistic Motion of Stars Near Rotating Black Hole
  Formulation of the Lagrangian approach is presented for studying features of
motions of stellar bodies with non-zero rest mass in the vicinity of
fast-spinning black holes. The structure of Lagrangian is discussed. The
general method is applied to description of body motion in the Kerr model of
space-time to transition to the problem of tidal disruption of elastic bodies
by strong gravitational field.
