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Q: Spacetime diagram of a collapse of a rotating star There is a well-known "standard" spacetime diagram (Kruskal and Penrose) for the collapse of a spherically symmetric star to a Schwarzschild black hole (for example here, or here in EF), which stands in nice contrast to the idealised "eternal" Schwarzschild black hole/white hole spacetime. I've been looking without success for an analogous spacetime diagram that shows a collapsing rotating star. In particular, I'm curious to see how the star decides which of the two Kerr singularities to fall into. Does anyone have such a diagram or reference to one, or could produce a sketch? A: It's not quite what you're looking for, but the article here from Physics World shows such a diagram for a charged Reissner-Nordström black hole. They note that Reissner-Nordström black holes were used to try to model the effects of incoming radiation being infinitely blueshifted at the inner (Cauchy) horizon, including the infinite blueshift of incoming gravitational waves which should cause a singularity at the Cauchy horizon. Apparently, physicists assumed that answer for a Reissner-Nordström black hole would serve as a reasonable approximation for what would happen in the case of a rotating Kerr black hole: This picture of an unstable Cauchy horizon, which becomes singular under exposure to radiative tails, was established through numerical integrations by Penrose and Michael Simpson at Birkbeck in 1973, and by several analytical studies in the following decade. However, this earlier work assumed a fixed (Reissner-Nordström) background, and did not attempt to estimate the effect of the blue-shifted radiation on the gravitational field. The first attempts to take this back-reaction into account were made by William Hiscock of the University of Montana in 1981. More representative models were examined by Eric Poisson and one of the authors (WI) at the University of Alberta in 1999, and by Amos Ori, then at CalTech, in 1991. To simplify the mathematics for a first reconnaissance, these early models made several approximations. It was assumed that rotating (non-spherical) black holes could be adequately modeled by spherical charged holes, since their horizon structures are similar. Gravitational (quadrupole) wave tails were modeled by spherical scalar waves. More general studies by Ori, by Patrick Brady, Chris Chambers and John Smith at the University of Newcastle-upon-Tyne in the UK, and by our group at the University of Alberta, confirm that these simplified models capture most of the essential features of the generic case. So with that in mind, here's the diagram: Here the red line is the outer event horizon, the blue line is the inner Cauchy horizon. Also note that it's possible for an infalling observer to cross a black line before crossing the Cauchy horizon--some recent work suggests there should actually be an additional singularity at this black line, created by the infinite blueshift of "backscattered" radiation, see this paper (the paper also seems to indicate a different Penrose diagram for the interior, see Fig. 1) along with this section of the book The Science of