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The Kerr metric or Kerr geometry describes the geometry of empty spacetime around a rotating uncharged axially symmetric black hole with a quasispherical event horizon.The Kerr metric is an exact solution of the Einstein field equations of general relativity; these equations are highly non-linear, which makes exact solutions very difficult to find.
The Kerr–Newman metric describes the spacetime geometry around a mass which is electrically charged and rotating. It is a vacuum solution which generalizes the Kerr metric (which describes an uncharged, rotating mass) by additionally taking into account the energy of an electromagnetic field, making it the most general asymptotically flat and stationary solution of the Einstein–Maxwell ...
The two types of charged black holes are Reissner–Nordström black holes (without spin), [1] and Kerr–Newman black holes (with spin). A black hole can be completely characterized by three (and only three) quantities: [1] M – mass; J – angular momentum; Q – electric charge; Charged black holes are two of four possible types of black ...
Two of those rotate: the Kerr and Kerr–Newman black holes. It is generally believed that every black hole decays rapidly to a stable black hole; and, by the no-hair theorem, that (except for quantum fluctuations) stable black holes can be completely described at any moment in time by these 11 numbers: mass–energy M,
This line element describes the Kerr–Newman metric. Here, is to be interpreted as the mass of the black hole, as seen by an observer at infinity, is interpreted as the angular momentum, and the electric charge. These are all meant to be constant parameters, held fixed.
The Kerr–Newman–de–Sitter metric (KNdS) [1] [2] is the one of the most general stationary solutions of the Einstein–Maxwell equations in general relativity that describes the spacetime geometry in the region surrounding an electrically charged, rotating mass embedded in an expanding universe.
In physics, black hole thermodynamics [1] is the area of study that seeks to reconcile the laws of thermodynamics with the existence of black hole event horizons.As the study of the statistical mechanics of black-body radiation led to the development of the theory of quantum mechanics, the effort to understand the statistical mechanics of black holes has had a deep impact upon the ...
In 1976, Subrahmanyan Chandrasekhar showed that a separable solution can be obtained from the Dirac equation in Kerr metric. [1] Later, Don Page extended this work to Kerr–Newman metric, that is applicable to charged black holes. [2] In his paper, Page notices that N. Toop also derived his results independently, as informed to him by ...