Abstract
The Kerr solution describes, in Einstein's theory, the gravitational field of a rotating black hole. The axial symmetry and stationarity of the solution are shown here to arise in a simple way from properties of the curvature tensor.
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A portion of this work was completed, in part, during the summer of 1972 at the University of Texas at Dallas, Division of Mathematics and Mathematical Physics, and at the Black Hole session of the Ecole d'été de Physique Théorique in Les Houches; supported, in part, by the National Science Foundation, Grants GP-8868, GP-3463 9X, GP-20023, and GU-1598; the Air Force Office of Scientific Research, Grant 903-67; the National Aeronautics and Space Administration, Grant 44-004-001; the Westinghouse Corparation; the Clark Foundation; and the Rhodes Trust at Oxford.
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Hughston, L.P., Sommers, P. The symmetries of Kerr black holes. Commun.Math. Phys. 33, 129–133 (1973). https://doi.org/10.1007/BF01645624
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DOI: https://doi.org/10.1007/BF01645624