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.
A new paper released by Professor Skenderis and Dr Marco Caldarelli from the University of Southampton, Dr Joan Camps from the University of Cambridge and Dr Blaise Gouteraux from the Nordic Institute for Theoretical Physics, Sweden published in the Rapid Communication section of Physical Review D, makes connections between negatively curved space-time and flat space-time.
Flat space-time and negative space-time describe an environment in which the Universe is non-compact, with space extending infinitely, forever in time, in any direction.
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.