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The Kruskal–Szekeres coordinates also apply to space-time around a spherical object, but in that case do not give a description of space-time inside the radius of the object. Space-time in a region where a star is collapsing into a black hole is approximated by the Kruskal–Szekeres coordinates (or by the Schwarzschild coordinates).
An example is the apparent (longitudinal) singularity at the 90 degree latitude in spherical coordinates. An object moving due north (for example, along the line 0 degrees longitude ) on the surface of a sphere will suddenly experience an instantaneous change in longitude at the pole (i.e., jumping from longitude 0 to longitude 180 degrees).
From Wikipedia, the free encyclopedia. Redirect page. Redirect to: Kruskal–Szekeres coordinates
The metric in Kruskal–Szekeres coordinates covers all of the extended Schwarzschild spacetime in a single coordinate system. Its chief disadvantage is that in those coordinates the metric depends on both the time and space coordinates.
As the article correctly says the "curvature singularity is given by the equation UV = 1". Thus one of U or V may be varied freely (with the other determined thereby) while remaining at the singularity. Thus three dimensions have either been constrained or rendered null while one dimension remains. In other words, the singularity is one ...
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