Even perturbations of the self-similar Vaidya space-time

Nolan, Brien C.; Waters, Thomas J.

doi:10.1103/physrevd.71.104030

Cited by 11 publications

(12 citation statements)

References 25 publications

(32 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…to the full PDE as well as in the individual modes obtained after separation. Although our analysis has a different focus to that of [36,37] our results for the stability of the wave-equations on out-going Vaidya are in agreement with their results for the wave-equations on ingoing linear mass Vaidya.…”

supporting

confidence: 86%

Wave equations on the linear mass Vaidya metric

Nafooshe

O’Loughlin

2016

Phys. Rev. D

View full text Add to dashboard Cite

We discuss the near singularity region of the linear mass Vaidya metric. In particular we investigate the structure in the numerical solutions for the scattering of scalar and electromagnetic metric perturbations from the singularity. In addition to directly integrating the full wave-equation, we use the symmetry of the metric to reduce the problem to that of an ODE. We observe that, around the total evaporation point, quasi-normal like oscillations appear, indicating that this may be an interesting model for the description of the end-point of black hole evaporation.

show abstract

supporting

confidence: 86%

Wave equations on the linear mass Vaidya metric

Nafooshe

O’Loughlin

2016

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…In addition, the assumption of spherical symmetry is very restricted. Very recently, the naked singularity formation in the self-similar Vaidya solution was found to be stable against non-spherical linear perturbations with even parity [17]. Analyses in Gauss-Bonnet gravity beyond spherical symmetry must be addressed.…”

Section: Discussionmentioning

confidence: 99%

“…(4.15) is 17) where E and F are integration constants. We set E = 1 and F = 0 by redefinition of the affine parameter.…”

Section: Curvature Strength Of a Naked Singularitymentioning

confidence: 99%

“…In a genuine counterexample of CCH, the solution must be stable against non-spherical perturbations. Stability analyses against non-spherical linear perturbations have been done for the marginally bound LTB solution [16] and the self-similar Vaidya solution [17]. It has been shown numerically that the naked singularity formation in the LTB solution is marginally stable against odd-parity perturbations but is unstable against even-parity perturbations [16].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Effects of Gauss–Bonnet term on the final fate of gravitational collapse

Maeda

2006

Class. Quantum Grav.

View full text Add to dashboard Cite

We obtain a general spherically symmetric solution of a null dust fluid in n(≥ 4)-dimensions in Gauss-Bonnet gravity. This solution is a generalization of the n-dimensional Vaidya-(anti)de Sitter solution in general relativity. For n = 4, the Gauss-Bonnet term in the action does not contribute to the field equations, so that the solution coincides with the Vaidya-(anti)de Sitter solution. Using the solution for n ≥ 5 with a specific form of the mass function, we present a model for a gravitational collapse in which a null dust fluid radially injects into an initially flat and empty region. It is found that a naked singularity is inevitably formed and its properties are quite different between n = 5 and n ≥ 6. In the n ≥ 6 case, a massless ingoing null naked singularity is formed, while in the n = 5 case, a massive timelike naked singularity is formed, which does not appear in the general relativistic case. The strength of the naked singularities is weaker than that in the general relativistic case. These naked singularities can be globally naked when the null dust fluid is turned off after a finite time and the field settles into the empty asymptotically flat spacetime.

show abstract

“…Since a massless scalar field supports waves moving at ingoing and outgoing streams. Thus the Cauchy horizon considered by [69,70,71], which lies outside the event horizon, is not expected to be subject to the mass inflation instability. Curiously, [71] go on to find that the flux diverges on the event horizon that eventually covers the naked singularity.…”

Section: Introductionmentioning

confidence: 99%

Perturbation theory of spherically symmetric self-similar black holes

Hamilton

2007

Preprint

View full text Add to dashboard Cite

The theory of perturbations of spherically symmetric self-similar black holes is presented, in the Newman-Penrose formalism. It is shown that the wave equations for gravitational, electromagnetic, and scalar waves are separable, though not decoupled. A generalization of the Teukolsky equation is given. Monopole and dipole modes are treated. The Newman-Penrose wave equations governing polar and axial spin-0 perturbations are explored.

show abstract

Even perturbations of the self-similar Vaidya space-time

Cited by 11 publications

References 25 publications

Wave equations on the linear mass Vaidya metric

Wave equations on the linear mass Vaidya metric

Effects of Gauss–Bonnet term on the final fate of gravitational collapse

Perturbation theory of spherically symmetric self-similar black holes

Contact Info

Product

Resources

About