Shadow and weak deflection angle of extended uncertainty principle black hole surrounded with dark matter

2021/04/30 by Reggie C. Pantig, Paul K. Yu, Emmanuel T. Rodulfo +1
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Black Holes and Theoretical Physics #Black hole (networking) #Charged black hole #Circular orbit #Classical mechanics #Dark matter #Deflection (physics) #Deflection angle #General relativity #Gravitation #Optics #Photon sphere #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #RADIUS #Schwarzschild metric #Schwarzschild radius #gr-qc

paper · pdf · doi:10.1016/j.aop.2021.168722

published as Annals of Physics 436, 168722 (2022) · 27 pages, 9 figures, edits/improvements on abstract and discussion, fixed some typos, added more references

openalex publication_date 2021/12/09 · arxiv created 2021/12/13 · arxiv updated 2021/12/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

In this paper, we discuss the possible effects of dark matter on a Schwarzschild black hole with the correction of extended uncertainty principle (EUP), such as the parameter α and the large fundamental length scale L_*. In particular, we surround the EUP black hole of mass m with a static spherical shell of dark matter described by the parameters mass M, inner radius r_s, and thickness Δr_s. In this study, we find that there is no deviation in the event horizon, which readily implies that the black hole temperature due to the Hawking radiation is independent of any dark matter concentration. In addition, we show some effects of the EUP parameter on the innermost stable circular orbit (ISCO) radius of time-like particles, photon sphere, shadow radius, and weak deflection angle. It is found that time-like orbits are affected by deviation of low values of mass M. A greater dark matter density is needed to have remarkable effects on the null orbits. Using the analytic expression for the shadow radius and the approximation Δr_s>>r_s, it is revealed that L_* should not be lower than 2m. To broaden the scope of this study, we also calculate the analytic expression for the weak deflection angle using the Ishihara et al. method \citeIshihara₂016. As a result, we show that Δr_s is improved by a factor of (1+4αm²/L_*²) due to the EUP correction parameters. The calculated shadow radius and weak deflection angle are then compared using the estimated values of the galactic mass from Sgr A*, M87, and UGC 7232, as well as the mass of the supermassive black hole at their center.

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