Rotating regular black holes

By Cosimo Bambi, L. Modesto. 2013

454 citations recorded by the source corpus.

Abstract The formation of spacetime singularities is a quite common phenomenon in General Relativity and it is regulated by specific theorems. It is widely believed that spacetime singularities do not exist in Nature, but that they represent a limitation of the classical theory. While we do not yet have any solid theory of quantum gravity, toy models of black hole solutions without singularities have been proposed. So far, there are only non-rotating regular black holes in the literature. These metrics can be hardly tested by astrophysical observations, as the black hole spin plays a fundamental role in any astrophysical process. In this Letter, we apply the Newman–Janis algorithm to the Hayward and to the Bardeen black hole metrics. In both cases, we obtain a family of rotating solutions. Every solution corresponds to a different matter configuration. Each family has one solution with special properties, which can be written in Kerr-like form in Boyer–Lindquist coordinates. These special solutions are of Petrov type D, they are singularity free, but they violate the weak energy condition for a non-vanishing spin and their curvature invariants have different values at r = 0 depending on the way one approaches the origin. We propose a natural prescription to have rotating solutions with a minimal violation of the weak energy condition and without the questionable property of the curvature invariants at the origin.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/20fc8e76c8f52e876e25c5c528e7c0041211c48e

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Citations in the corpus

Magnetically charged black holes from non-linear electrodynamics and the Event Horizon Telescope (2019, unknown): “[78–112].”
Constraining the spin and the deformation parameters from the black hole shadow (2014, background): “2), with the mass M replaced by m [51, 52]:”
Construction of Regular Black Holes in General Relativity (2016, background): “Other regular black hole models are also proposed later [5, 6, 7, 8, 9, 10, 11, 12, 13, 14].”
Constraints on black-hole charges with the 2017 EHT observations of M87* (2021, methodology): “2 the shadow areal radius rsh,A for a number of stationary black holes, such as Kerr [39], Kerr-Newman (KN) [40], Sen [41], and the rotating versions of the Bardeen and Hayward black holes [42].”
A novel family of rotating black hole mimickers (2021, methodology): “Not surprisingly, rotating regular black holes have been considered before, see e.g. [26–31]; similarly, rotating traversable wormholes have been proposed in [32] and used for phenomenological modelling e.g. in [33– 37].”
Black Hole Parameter Estimation from Its Shadow (2018, methodology): “The metric of a general rotating, stationary, and axially symmetric black hole, in Boyer–Lindquist coordinates, reads (Bambi & Modesto 2013) q f q q q f =- -”
Regular Black Holes: A Short Topic Review (2023, methodology): “Inordertoestablishawell-deﬁnedﬁrstthermodynamiclawthatmeetstheaboveconditions for RBHs with two parameters, such as Bardeen BHs, we have applied [97, 185, 187] the following form in terms of the Gliner vacuum, d U = T d S − P + d V , (115) where the total internal energy reads P + and V are the ther”
Measuring the Kerr spin parameter of regular black holes from their shadow (2013, methodology): “The rotating solutions have the same form of the Kerr metric, with the mass M replaced by m as follows [64, 65]:”
Gravitational Lensing in Presence of Plasma: Strong Lens Systems, Black Hole Lensing and Shadow (2017, background): “Numerous analytical investigations and numerical simulations of the shadow are presented in literature (for example, see [90, 101, 95, 85, 86, 103, 104, 105, 94, 98, 99, 91, 106, 102, 97, 87, 88, 89, 93, 92, 96, 100, 110, 107, 108, 109, 111]).”
A coordinate-independent characterization of a black hole shadow (2015, methodology): “…in known space-times, either within general relativity (Young 1976; Perlick 2004; Abdujabbarov et al. 2013), or within alternative theories of gravity (Bambi & Modesto 2013; Tsukamoto et al. 2014; Amarilla et al. 2010; Amarilla & Eiroa 2012, 2013; Atamurotov et al. 2013a,b; Schee & Stuchlı́k 2009).”