Eunice Omwoyo | Searcharxiv

arXiv2023

Black hole lensing in Kerr-de Sitter spacetimes

We have derived analytical solutions using Jacobi elliptic functions for bound and nearly bound photon orbits in Kerr-de Sitter (KdS) and Kerr-de Sitter Revisited (RKdS) spacetimes. Leveraging our obtained solutions, we have conducted an analytic ray-tracing in both spacetimes. We have obtained direct images, lensing rings and photon rings for equatorial disks considering inclined locally static observers. Images corresponding to n=(2,3) exhibit a significantly closer resemblance to the critical curve as compared to the n=1 image. This highlights the remarkable potential of these higher-order images as robust testing grounds for General Relativity (GR). Furthermore in both spacetimes, we have obtained analytical solutions for the critical parameters governing the structure of the photon ring and analyzed these parameters in details.

gr-qc↗

arXiv2022

Remarks on the black hole shadows in Kerr-de Sitter space times

This work is geared towards analysis of shadows cast by Kerr-de Sitter (KdS) and Kerr-de Sitter Revisited (RKdS) black holes. Considering observers in the vicinity of the static radius, we derive the impact parameters defining the apparent positions of the shadows. Such observers are of interest to our work because embedding diagrams have shown that de Sitter space-time is analogous to an asymptotically flat one in the vicinity of the static radius. We also perform a comparative analysis between our result with that in Ref.[1]. Furthermore, we numerically obtain the radii of curvature, vertical diameters and horizontal diameters of the shadows. We find that for $Λ=1.11\times 10^{-52} m^{-2}$, M87* observations cannot distinguish a RKdS black hole shadow from that of a Kerr black hole. Additionally, for the same value of $Λ$, KdS and RKdS black hole shadows are identical. Previously, it has also been shown that when $Λ=1.11\times 10^{-52} m^{-2}$, KdS and Kerr black hole shadows are indistinguishable. Utilizing the 2017 EHT observations of M87* on the allowed range of the characteristic radius of the shadow, we obtain constraints on both black holes. When, a/M>0.812311, we observe that large angles of inclination ($θ>30.5107^{\circ}$) do not pass the constraints for both KdS and RKdS black holes.

gr-qc↗