Relativistic Motion of Stars Near Rotating Black Hole
Abstract
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.
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