flat space-time

flat space-time

[′flat ¦spās ¦tīm]
(relativity)
Space-time in which the Riemann-Christoffel tensor vanishes; geometry is then equivalent to that of the Minkowski universe used in special relativity.
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In the Euclidean flat space-time, the coordinates are represented by [z.sup.A] = ([x.sup.a], [[theta].sup.I]).
(6) The diagram shown is for flat space-time (from Wikipedia).
Moreover, an EH always exists in black hole asymptotically flat space-time under a weak cosmic censorship condition and is represented by a Killing horizon such that the space-time is analytic and the stress tensor obeys the weak energy condition.
In [11], they considered a conformal transformation [bar.g] = [[OMEGA].sup.2]g to a stationary, asymptotically flat space-time (M, g) admitting a Killing horizon H.
According to this theory, dynamical phenomena occurring in a curved space-time like black holes can be described by a theory on a flat space-time, just as a hologram can record the information of 3D objects on a plane.
The teleparallel equivalent of general relativity allows the curvature of a metric to be rephrased as contorsion in a flat space-time due to a tetrad field [2].
This results in a flat space-time with an index of refraction.
and we identify the mass M of the sphere under study as constant, in flat space-time (M = 4/3[pi][rho][r.sup.3]).
In the second case, it reduces to flat space-time of special relativity.
This solution has the same thermodynamic characteristics as the black hole solution in asymptotically flat space-time; that is, the black hole entropy is equal to a quarter of the event horizon area, while the corresponding thermodynamics quantity satisfies the law of thermodynamics of black hole.