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- W2549754851 abstract "In the analysis of the interior region of both stationary and rotating black holes, it is customary to switch to a set of in-falling coordinates to avoid problems posed by the coordinate singularity at the event horizon. I take the view here that to understand the physics of black holes, we need to restrict ourselves to bookkeeper or Schwarzschild coordinates of a distant observer if we are to derive measurable properties. I show that one can derive interesting properties of black holes that might explain some of the observational evidence available without the necessity of introducing further ad hoc conjectures. 1 The Schwarzschild black hole Birkhoff’s theorem [1] assures us that for any non-rotating spherically symmetric distribution of matter, the gravitational effect on any test mass is solely due to whatever mass lies closer to the center of symmetry. This allows us to infer what happens inside the event horizon, by comparing a hypothetical distribution of matter that is identical but with all mass outside the point of interest removed, with that of (say) a collapsing star. Making no further assumptions, let the density" @default.
- W2549754851 created "2016-11-30" @default.
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- W2549754851 date "2014-07-01" @default.
- W2549754851 modified "2023-09-26" @default.
- W2549754851 title "Black Hole Structure in Schwarzschild Coordinates" @default.
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