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Closer to the black hole spacetime starts to deform. In some convenient coordinate systems, there are more paths going towards the black hole than paths moving away. [Note 1] Inside the event horizon all future time paths bring the particle closer to the center of the black hole.
The Kerr metric or Kerr geometry describes the geometry of empty spacetime around a rotating uncharged axially symmetric black hole with a quasispherical event horizon.The Kerr metric is an exact solution of the Einstein field equations of general relativity; these equations are highly non-linear, which makes exact solutions very difficult to find.
The inner event horizon of the Kerr geometry is probably not stable, due to the infinite blue-shifting of infalling radiation. [4] This observation was supported by the investigation of charged black holes which exhibited similar "infinite blueshifting" behavior. [5] While much work has been done, the realistic gravitational collapse of objects ...
(Supermassive black holes up to 21 billion (2.1 × 10 10) M ☉ have been detected, such as NGC 4889.) [16] Unlike stellar mass black holes, supermassive black holes have comparatively low average densities. (Note that a (non-rotating) black hole is a spherical region in space that surrounds the singularity at its center; it is not the ...
The blueshifted energy of the infalling radiation should, in principle, have a significant impact on the spacetime geometry near the inner horizon. The backreaction of the blueshifted radiation leads to a runaway effect where the effective mass parameter (or energy density) of the black hole as measured near the inner horizon grows without bound.
A black hole with the mass of a car would have a diameter of about 10 −24 m and take a nanosecond to evaporate, during which time it would briefly have a luminosity of more than 200 times that of the Sun. Lower-mass black holes are expected to evaporate even faster; for example, a black hole of mass 1 TeV/c 2 would take less than 10 −88 ...
The event horizons bounding the black hole and white hole interior regions are also a pair of straight lines at 45 degrees, reflecting the fact that a light ray emitted at the horizon in a radial direction (aimed outward in the case of the black hole, inward in the case of the white hole) would remain on the horizon forever. Thus the two black ...
Event horizons and ergospheres of a charged and spinning black hole in pseudospherical r,θ,φ and cartesian x,y,z coordinates. Setting / to 0 and solving for gives the inner and outer event horizon, which is located at the Boyer–Lindquist coordinate