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On the Stability of Slowly Rotating Kerr Black Holes

 By Amal Pushp, Affiliate Physicist at the Resonance Science Foundation

A black hole is a solution to Einstein’s general relativistic field equations. Based on the property of angular momentum, black holes can be categorized into two types: non-rotating and rotating. The former is described by the Schwarzschild solution and the latter by the Kerr solution, originally named after its discoverers.

Perhaps all physical systems tend to move towards equilibrium irrespective of their initial conditions and similar is the case with black holes. A long-standing problem in black hole physics concerns the stability of these great astrophysical voids. The idea is to regain the original state of the black hole after the effect of an externally applied perturbation has faded away. This proves that the black hole is indeed stable. The case otherwise is an instability and would be quite a task in that it would compel us to modify Einstein’s theory.

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