The Kerr metric describes the time-independent, axis-symmetric gravitational field of a collapsed object that has retained its angular momentum. All matter having collapsed, the Kerr metric satisfies the vacuum Einstein equation given by Rμν = 0.
The Kerr solution di ers from the Schwarzschild in that there are two horizons. As we cross the outer horizon at r = r+; the roles of t and r change and we can only go forward in r and not backward.
Within 4-dimensional general relativity, a stationary black hole in an otherwise empty universe is necessarily a Kerr-Newman black hole, which is an electro-vacuum solution of Einstein equation described by only 3 parameters: the total mass M the total specific angular momentum a = J=M the total electric charge Q
Basics of black hole physics 3. The Kerr black hole - obspm.fr
Kerr metric is a special 2-parameter subfamily in this class, which makes these considerations directly relevant to Kerr as well. This results in a derivation of the Kerr metric that is self-contained and elementary, in the sense of being mostly an exercise in linear algebra.
In this paper, we will explore the geometry of the Kerr spacetime, a solution to the Einstein Equation in general relativity.
All results on the linear stability of Kerr in the physics literature during the 10-15 years after Roy Kerr’s 1963 discovery, often called the “Golden Age of Black Hole Physics”, are based on mode decompositions.
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