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The classification of black holes

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If you have a question about this talk, please contact Valentin Hübner.

I will provide a gentle introduction to the problem of classifying black hole solutions of the Einstein equation (the equation of motion of General Relativity). Uniqueness theorems proved in the 1970s indicate that, in three spatial dimensions, a time-independent black hole is described by the Kerr solution, which depends on just 2 parameters: the mass and angular momentum of the hole. However, in four spatial dimensions, there exist black holes with non-spherical topology as well as generalizations of the Kerr solution. Thus the classification problem is much more complicated in higher dimensions. I will describe the results that have been proved so far and the open problems that remain.

This talk is part of the The Archimedeans (CU Mathematical Society) series.

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