Kerr black hole in de Sitter spacetime and observational redshift: Toward a new method to measure the Hubble constant

Momennia, Mehrab; Herrera–Aguilar, Alfredo; Nucamendi, Ulises

doi:10.1103/physrevd.107.104041

Cited by 6 publications

(1 citation statement)

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“…In [54], the authors investigate null geodesics of a class of charged, spherical, and asymptotically flat hairy black holes in an Einstein-Maxwell-scalar theory with nonminimal coupling for the scalar and electromagnetic fields. In [55], the Hubble law is extracted through frequency-shift considerations of test particles revolving around the Kerr black hole in asymptotically de Sitter spacetime. In [56], the authors delve into the correspondence between the shape of the shadow and Kerr parameters, extending it to a general rotating black hole generated by the Newman-Janis algorithm, as detailed in Refs.…”

Section: Introductionmentioning

confidence: 99%

Image of Kerr–de Sitter black holes illuminated by equatorial thin accretion disks

Wang,

Feng,

Wang

2024

Eur. Phys. J. C

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To explore the influence of the cosmological constant on black hole images, we have developed a comprehensive analytical method for simulating images of Kerr–de Sitter black holes illuminated by equatorial thin accretion disks. Through the application of explicit equations, we simulate images of Kerr–de Sitter black holes illuminated by both prograde and retrograde accretion disks, examining the impact of the cosmological constant on their characteristic curves, relative sizes, and observed intensities. Our findings reveal that, in comparison to Kerr black holes, the cosmological constant not only diminishes the relative size of a black hole but also amplifies its luminosity. Moreover, an observer’s relative position in the universe ($$r_0/r_C$$ r 0 / r C ) can influence both the relative size and luminosity of a black hole, where $$r_0$$ r 0 is the distance from the observer to the black hole, $$r_C$$ r C is the cosmological horizon determined by the value of the cosmological constant $$\Lambda $$ Λ .

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Section: Introductionmentioning

confidence: 99%

Image of Kerr–de Sitter black holes illuminated by equatorial thin accretion disks

Wang,

Feng,

Wang

2024

Eur. Phys. J. C

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Unveiling the evolution of rotating black holes in loop quantum cosmology

Swain,

Sahoo,

Nayak

2024

Sci Rep

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In this work, we aim to discuss about the evolution of rotating black holes (RBHs) within the context of loop quantum cosmology. Here, the main part of our research work focuses on the impacts of angular momentum based rotating parameter and accretion efficiency on the lifetime of RBHs. Our study reveals that accretion of dark energy would not significantly affect the evolution of RBHs, however higher value of rotating parameter could slightly delay the evaporation times of RBHs. Our analysis also depicts that the maximum value of rotating parameter for evolution of any RBH is , where is the formation mass of RBH. Moreover, from our calculation we found that the maximum mass of a presently existing supermassive black hole would be , if it undergoes rotation. Also from astrophysical constraint analysis, we found that there is a greater tendency for formation of black holes in loop quantum cosmology than standard model of cosmology.

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