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This Full PDF is an intuitive introduction to the Kerr solution of Einstein’s Field Equations, explaining how spacetime behaves around a rotating, uncharged black hole. Starting from historical context and the key physical quantities (mass, Schwarzschild radius, and specific angular momentum), we carefully build up the full Kerr metric in Boyer–Lindquist coordinates and explores its main features: the inner and outer horizons, the ergosphere, and frame dragging (Lense–Thirring effect). We apply the knowledge to real astrophysical examples such as Sagittarius A* and M87*. 

We also present exercises with detailed solutions, so that you can practice everything you learned.

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