Black holes: A physical route to the Kerr metric

Abstract

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.

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

References in corpus (2)

• General relativistic gravitational field of a rigidly rotating disk of dust: Solution in terms of ultraelliptic functions
• Highly accurate calculation of rotating neutron stars

Cited by in corpus (4)

• Progress in relativistic gravitational theory using the inverse scattering method
• On the black hole limit of rotating discs and rings
• The Post-Newtonian Maclaurin Spheroids to Arbitrary Order
• Geometry of charged rotating discs of dust in Einstein-Maxwell theory