Kerr–Vaidya black holes

Dahal, Pravin Kumar; Terno, Daniel R.

doi:10.1103/physrevd.102.124032

Cited by 16 publications

(23 citation statements)

References 39 publications

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“…We have Ṙ < 0, and the velocity component Ẇ > 0 is obtained from the normalization condition u 2 A = −1. Similar to the Vaidya metrics, the result depends 157 on whether this is a retarded or an advanced metric and on the sign of M (w). In (u, r) coordinates…”

Section: Finite Blueshift and Finite Infall Timementioning

confidence: 89%

“…The metric of Eq. ( 71) with variable M (u) is obtained from the outgoing Vaidya metric, 156 and its counterpart with variable M (v) from the ingoing Vaidya metric, 157 while other models of regular axially symmetric black holes are obtained by transforming their spherically symmetric counterparts. 158…”

Section: Axial Symmetrymentioning

confidence: 99%

“…A detailed investigation reveals some interesting properties of this EMT. 157 We use a tetrad in which the null eigenvector k µ = k âe µ â has the components k â = (1, 1, 0, 0), the third vector e 2 ∝ ∂ θ , and the remaining vector e 3 is found by completing the basis. Then the EMT takes the form…”

Section: Properties Of Kerr-vaidya Metricsmentioning

confidence: 99%

“…It can be obtained numerically and shows some unusual properties, such as z = 0 at the poles. 157 The static limit -the boundary of the region where static observers cannot exist -is given in the Kerr spacetime by…”

Section: Properties Of Kerr-vaidya Metricsmentioning

confidence: 99%

“…Consider now Alice on the background of a Kerr-Vaidya metric. 157 For a generic trajectory her four-velocity is written as u µ A = U , Ṙ, Θ, Ψ . Here, we again use capital letters to distinguish the trajectories, W = w ± (τ ) and Ψ = ψ ± (τ ), and treat the two coordinate systems simultaneously as long as it is feasible.…”

Section: Finite Blueshift and Finite Infall Timementioning

confidence: 99%

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Black holes and their horizons in semiclassical and modified theories of gravity

Mann,

Murk,

Terno

2021

Preprint

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For distant observers black holes are trapped spacetime domains bounded by apparent horizons. We review properties of the near-horizon geometry emphasizing the consequences of two common implicit assumptions of semiclassical physics. The first is a consequence of the cosmic censorship conjecture, namely that curvature scalars are finite at apparent horizons. The second is that horizons form in finite asymptotic time (i.e. according to distant observers), a property implicitly assumed in conventional descriptions of black hole formation and evaporation. Taking these as the only requirements within the semiclassical framework, we find that in spherical symmetry only two classes of dynamic solutions are admissible, both describing evaporating black holes and expanding white holes. We review their properties and present the implications. The null energy condition is violated in the vicinity of the outer and satisfied in the vicinity of the inner apparent/anti-trapping horizon. Apparent and anti-trapping horizons are timelike surfaces of intermediately singular behavior, which is demonstrated in negative energy density firewalls. These and other properties are also present in axially symmetric solutions. Different generalizations of surface gravity to dynamic spacetimes are discordant and do not match the semiclassical results. We conclude by discussing signatures of these models and implications for the identification of observed ultra-compact objects.

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Section: Finite Blueshift and Finite Infall Timementioning

confidence: 89%

Section: Axial Symmetrymentioning

confidence: 99%

Section: Properties Of Kerr-vaidya Metricsmentioning

confidence: 99%

Section: Properties Of Kerr-vaidya Metricsmentioning

confidence: 99%

Section: Finite Blueshift and Finite Infall Timementioning

confidence: 99%

See 3 more Smart Citations

Black holes and their horizons in semiclassical and modified theories of gravity

Mann,

Murk,

Terno

2021

Preprint

Self Cite

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Shadows of Kerr–Vaidya-like black holes

Tan

2023

Class. Quantum Grav.

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In this work, we study the shadow boundary curves of rotating time-dependent black hole solutions which have well-deﬁned Kerr and Vaidya limits. These solutions are constructed by applying the Newman-Janis algorithm to a spherically symmetric seed metric conformal to the Vaidya solution with a mass function that is linear in Eddington-Finkelstein coordinates. Equipped with a conformal Killing vector ﬁeld, this class of solution exhibits separability of null geodesics, thus allowing one to develop an analytic formula for the boundary curve of its shadow. We ﬁnd a simple power law describing the dependence of the mean radius and asymmetry factor of the shadow on the accretion rate. Applicability of our model to recent Event Horizon Telescope observations of M87∗ and Sgr A∗ is also discussed.

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Kodama-like vector fields in axisymmetric spacetimes

Dorau,

Verch

2024

Class. Quantum Grav.

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We extend the concept of the Kodama symmetry, a quasi-local time translation symmetry for dynamical spherically symmetric spacetimes, to a specific class of dynamical axisymmetric spacetimes, namely the families of Kerr–Vaidya and Kerr–Vaidya–de Sitter spacetimes. We study some geometrical properties of the asymptotically flat Kerr–Vaidya metric, such as the Brown–York mass and the Einstein tensor. Furthermore, we propose a generalization of the Kerr–Vaidya metric to an asymptotic de Sitter background. We show that for these classes of dynamical axisymmetric black hole spacetimes, there exists a timelike vector field that exhibits similar properties to the Kodama vector field in spherical symmetry. This includes the construction of a covariantly conserved current and a corresponding locally conserved charge, which in the Kerr–Vaidya case converges to the Brown–York mass in the asymptotically flat region.

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Kerr–Vaidya black holes

Cited by 16 publications

References 39 publications

Black holes and their horizons in semiclassical and modified theories of gravity

Black holes and their horizons in semiclassical and modified theories of gravity

Shadows of Kerr–Vaidya-like black holes

Kodama-like vector fields in axisymmetric spacetimes

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