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Galaxies 2018, 6(2), 61; https://doi.org/10.3390/galaxies6020061

Relativistic Motion of Stars near Rotating Black Holes

1
Scientific Advisory Group, Pasadena, CA 91125, USA
2
Faculté des Sciences et Technologies, Université de Lillé, F-59000 Lille, France
*
Author to whom correspondence should be addressed.
Received: 20 April 2018 / Revised: 31 May 2018 / Accepted: 1 June 2018 / Published: 5 June 2018
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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 a strong gravitational field. View Full-Text
Keywords: fast-spinning black hole; Kerr space–time; structure of Lagrangian; motion regimes fast-spinning black hole; Kerr space–time; structure of Lagrangian; motion regimes
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This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).
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Tito, E.P.; Pavlov, V.I. Relativistic Motion of Stars near Rotating Black Holes. Galaxies 2018, 6, 61.

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