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Black holes: a physical route to the Kerr metric
Author(s) -
Meinel R.
Publication year - 2002
Publication title -
annalen der physik
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.009
H-Index - 68
eISSN - 1521-3889
pISSN - 0003-3804
DOI - 10.1002/1521-3889(200208)11:7<509::aid-andp509>3.0.co;2-o
Subject(s) - physics , kerr metric , schwarzschild metric , rotating black hole , black hole (networking) , schwarzschild radius , gravitational field , classical mechanics , metric (unit) , rotational symmetry , gravitation , charged black hole , field (mathematics) , general relativity , mechanics , angular momentum , mathematics , computer network , routing protocol , operations management , routing (electronic design automation) , computer science , economics , link state routing protocol , pure mathematics
As a consequence of Birkhoff's theorem, the exterior gravitational field of a spherically symmetric star or black hole is always given by the Schwarzschild metric. In contrast, the exterior gravitational field of a rotating (axisymmetric) star differs, in general, from the Kerr metric, which describes a stationary, rotating black hole. In this paper I discuss the possibility of a quasi–stationary transition from rotating equilibrium configurations of normal matter to rotating bla ck holes.