Surfaces of infinite red-shift around a uniformly accelerating and rotating particle

Farhoosh, Hamid; Zimmerman, Robert L.

doi:10.1103/physrevd.21.2064

Cited by 28 publications

(31 citation statements)

References 5 publications

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“…However, Hong and Teo [12] have recently shown that, at least for some special cases, the available freedom is much better used to simplify the roots of these functions. In the rotating case, they obtained a new solution [13] for an accelerating and rotating black hole which differs from what is usually called the "spinning C-metric" [14]- [16] in which the linear terms are set to zero. Surprisingly, it is the new solution of Hong and Teo which represents the NUT-free case, while the "spinning C-metric" retains NUT-like properties (i.e.…”

Section: Introductionmentioning

confidence: 99%

Accelerating Kerr–Newman black holes in (anti-)de Sitter space-time

Podolský

Griffiths

2006

Phys. Rev. D

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Section: Introductionmentioning

confidence: 99%

Accelerating Kerr–Newman black holes in (anti-)de Sitter space-time

Podolský

Griffiths

2006

Phys. Rev. D

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“…One can show that, after writing the directional derivatives eâ in terms of the weighted derivatives Dâ, these basic equations (a)-(c) form a consistent, closed system of PDEs in the variables (A2)-(A10) and with formal derivative operators Dâ. Compared to the NP formalism, the 6 complex Ricci identities which concern directional derivatives of the non-well-weighted NP spin coefficients α, β, γ and ǫ (corresponding to [âb] = [12], [34]) have been absorbed in the commutator relations (1). Explicitly, for a (w p , w q )-weighted scalar one gets…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Expanding perfect fluid generalizations of theCmetric

Wylleman

Beke

2010

Phys. Rev. D

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Petrov type D gravitational fields, generated by a perfect fluid with spatially homogeneous energy density and with flow lines which form a non-shearing and non-rotating timelike congruence, are re-examined. It turns out that the anisotropic such spacetimes, which comprise the vacuum Cmetric as a limit case, can have non-zero expansion, contrary to the conclusion in the original investigation by Barnes [1]. Apart from the static members, this class consists of cosmological models with precisely one symmetry. The general line element is constructed and some important properties are discussed. It is also shown that purely electric Petrov type D vacuum spacetimes admit shearfree normal timelike congruences everywhere, even in the non-static regions. This result incited to deduce intrinsic, easily testable criteria regarding shearfree normality and staticity of Petrov type D spacetimes in general, which are added in an appendix.

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“…For the nonrotating case the E cm given by (25) becomes This CM energy given by (28) diverges at the acceleration horizons r = ±(1/α). It also diverges at the event horizon if the black hole is extremal.…”

Section: Collision Energy In the Center-of-mass Frame For Rotating Anmentioning

confidence: 99%

Collision Energy in the Center-of-Mass Frame for Rotating and Accelerating Black Holes

Hussain

2012

Mod. Phys. Lett. A

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The center-of-mass (CM) energy of collision for two uncharged particles falling freely from rest at infinity is investigated in the background of charged, rotating and accelerating black hole. It is found that the CM energy of collision is unlimited at the acceleration horizon and at the event horizon (in the extremal case) if one of the colliding particles has critical angular momentum and the other one has a proper angular momentum such that the particle can reach the horizon.

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Surfaces of infinite red-shift around a uniformly accelerating and rotating particle

Cited by 28 publications

References 5 publications

Accelerating Kerr–Newman black holes in (anti-)de Sitter space-time

Accelerating Kerr–Newman black holes in (anti-)de Sitter space-time

Expanding perfect fluid generalizations of theCmetric

Collision Energy in the Center-of-Mass Frame for Rotating and Accelerating Black Holes

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