Black holes: A physical route to the Kerr metric

Details Black holes: A physical route to the Kerr metric Black holes: A physical route to the Kerr metric

2002-05-30

arxiv.org/abs/gr-qc/0205127v2

Annalen Phys.11:509-521,2002

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

14 pages, 1 table, 4 figures, accepted for publication in Annalen der Physik (Leipzig)

Scientific paper

10.1002/1521-3889(200208)11:7<50

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 black holes.

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