Black holes: A Physical route to the Kerr metric
May, 2002Citations per year
Abstract: (arXiv)
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.Note:
- 14 pages, 1 table, 4 figures, accepted for publication in Annalen der Physik (Leipzig)
References(22)
Figures(4)