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Before beginning the study of the quantum theory of black
holes, one must first become thoroughly familiar with the geometry of
classical black holes in a variety of different coordinate systems. Each
coordinate system that we will study has its own particular utility, and no
one of them is in any sense the best or most correct description. For example,
the Kruskal–Szekeres coordinate system is valuable for obtaining a
global overview of the entire geometry. It can however be misleading when applied to
observations made by distant observers who remain outside the horizon
during the entire history of the black hole. For these purposes, Schwarzschild
coordinates, or the related tortoise coordinates, which cover only the exterior
of the horizon are in many ways more valuable. We begin with the simplest spherically symmetric static
uncharged black holes described by Schwarzschild geometry.
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