From any location outside the event horizon of a black hole there are an infinite number of trajectories for light to an observer. Each of these paths differ in the number of orbits revolved around the black hole and in their proximity to the last photon orbit. With simple numerical and a...
On the other hand, we consider the non-radial motion of a free-falling test particle, in the equatorial plane, from spatial infinity to the black hole. In the ultrarelativistic limit, we show that the photon sphere acts as an effective Rindler horizon for the geodesic motion of the test ...
when traced backward from the perspective of the observer, asymptotically approach bound photon orbits. The aggregate of all such bound photon orbits constitutes what is known as the photon region, or the photon sphere in the case of spherically symmetric spacetimes. It’...
A large class of spherically symmetric static extremal black hole spacetimes possesses a stable null photon sphere on their horizons. For the extremal Kerr-Newman family, the photon sphere only really coincides with the horizon in the sense clarified by Doran. The condition under which photon orbit...
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Bipolar qubit as a key for BQLG extends 2-state (01) unipolar Bloch Sphere to a 4-state bipolar qubit register for equilibrium-based bipolar interaction, computing, and communication [3], [44], [79] (Note: In theory, a holographic extension is possible [3]). Even though QI is quantum...
In the current experiment, we demonstrate an average teleported state fidelity of 0.78±0.03 (0.80±0.03) with (and without) spin-echo sequences, for four states that lie on a plane on the Bloch sphere; for such states, the optimal state estimation yields a fidelity of 3/4 and our ...
[10]S. Setiawan, T. G Mackay and A. Lakhtakia, “A Comparison of Super Radiance and Negative Phase Velocity Phenomena in Ergo Sphere of Rotating Black Hole” Physics Letters A, Vol. 341, No. 1-4, 2005, pp. 15-21. doi:10.1016/j.physleta.2005.04.064 ...
We study the general motion of photons in the Kerr–de Sitter black-hole and naked singularity spacetimes. The motion is governed by the impact parametersX, related to the axial symmetry of the spacetime, andq, related to its hidden symmetry. Appropriate ‘effective potentials’ governing the ...