asymptotically flat

asymptotically flat

[‚ā·sim¦tät·ə·klē ′flat]
(relativity)
A space-time is asymptotically flat if it approaches Minkowski space-time at a prescribed rate at large spatial distances.
References in periodicals archive ?
The solution under study describes an asymptotically flat black hole and the motions of both massless and massive particles are analyzed.
Let (M, g, k) be an initial data set for the Einstein equations with a single asymptotically flat end.
This first of two volumes of proceedings contains 19 technical papers on such topics as instabilities in kinetic theory and their relationship to the ergodic theorem, the uniqueness of photon spheres in static vacuum asymptotically flat spacetimes, an initial-boundary value problem in a strip for two-dimensional equations of Zacharov-Kunzhetsov type, an extension of harmonicity and holomorphy, and over-determined transforms in integral geometry.
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.
This has led many researchers to conclude that the universe is home to a multitude of black holes conforming to one of the stationary, asymptotically flat, black hole metrics --in accordance with the claim of a leading relativist that the "black holes of nature are the most perfect macroscopic objects that are in the universe" [3].
The first work solves the Cauchy problem for the Einstein vacuum equations with more general, asymptotically flat initial data and then describes the asymptotic behavior.
Ahmed, "Cylindrically symmetric, asymptotically flat, petrov type d spacetime with a naked curvature singularity and matter collapse," Advances in High Energy Physics, vol.
And using the Kerr-Schild formalism, one can obtain exact asymptotically flat multiparticle solutions of the Einstein-Maxwell field equations.
A Cosmic Time Machine is a space-time which is asymptotically flat and admits closed nonspacelike curves which extend to future infinity.
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.
In Section 2, we briefly review the regular phantom BH solutions and discuss their properties in three different spacetimes, namely, asymptotically flat, de Sitter (dS), and anti-de Sitter (AdS).