Black holes and black hole thermodynamics without event horizons

Nielsen, A. B.

doi:10.1007/s10714-008-0739-9

Cited by 63 publications

(67 citation statements)

References 118 publications

(213 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The location of the event horizon is independent of the choice of foliation. This approach however causes trouble in certain quantum inspired spacetimes [3,18] where no event horizon exists. In numerical settings, the teleological definition of the event horizon means that it is only known after a simulation is finished, preventing it from being used to analyse the simulation's state as it proceeds.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

et al. 2011

Self Cite

View full text Add to dashboard Cite

It is well known that quasi-local black hole horizons depend on the choice of a time coordinate in a spacetime. This has implications for notions such as the surface of the black hole and also on quasi-local physical quantities such as horizon measures of mass and angular momentum. In this paper, we compare different horizons on non-spherically symmetric slicings of Vaidya spacetimes. The spacetimes we investigate include both accreting and evaporating black holes. For some simple choices of the Vaidya mass function function corresponding to collapse of a hollow shell, we compare the area for the numerically found axisymmetric trapping horizons with the area of the spherically symmetric trapping horizon and event horizon. We find that as expected, both the location and area are dependent on the choice of foliation. However, the area variation is not large, of order 0.017% for a slowly evolving horizon withṁ = 0.02. We also calculate analytically the difference in area between the spherically symmetric quasi-local horizon and event horizon for a slowly accreting black hole. We find that the difference can be many orders of magnitude larger than the Planck area for sufficiently large black holes.

show abstract

Section: Conclusion and Discussionmentioning

confidence: 99%

“…A number of useful analytic relations for the Vaidya spacetime are given in the appendix. Background detail on the properties of trapping horizons and their thermodynamics can be found in [1] and [3].…”

mentioning

confidence: 99%

Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

et al. 2011

Self Cite

View full text Add to dashboard Cite

show abstract

“…The GP coordinates are commonly presented as a set of coordinates obtained by transformation of the Schwarzschild, or Reissner-Nordström (RN) ones, in which the static time is replaced by a GP time t →t(t, r ), preserving the spherical symmetry of the problem [24,25]. We shall use a slightly different method by using the GP cartesian metric and using the vielbein related to an orthonormal basis.…”

Section: D Gullstränd-painlevé (Gp) Metricmentioning

confidence: 99%

“…With a constant foliation we must obtain η αβ = ±1, for the basis { − → E α }. In this context the Weitzenböck torsion is specially easy to obtain according to (25), and we can transform it to other representations using the corresponding vielbein.…”

Section: Appendix A: Connecting Onb Gp and Rnmentioning

confidence: 99%

WIMT in Gullstränd–Painlevé and Reissner–Nordström metrics: induced stable gravito-magnetic monopoles

Romero

Bellini

2015

Eur. Phys. J. C

View full text Add to dashboard Cite

The aim of this work is to apply Weitzeböck Induced Matter Theory (WIMT) to Gullstränd-Painlevé and Reissner-Nordström metrics in the framework of WIMT. This is a newly developed method that extends Induced Matter Theory from a curved 5D manifold using the Weitzeböck's geometry, using the fact that the Riemann-Weitzenböck curvature tensor is always null. We obtain the presence of currents whose interpretation can lead to the presence of stable gravito-magnetic monopoles.

show abstract

“…The Hawking radiation is usually associated with the existence of an event horizon, but crucial in the tunneling calculation is a pole in the path integral that does not always occur at the location of the causal event horizon. This has led several authors to claim that Hawking radiation should be associated with quasi-local trapping horizons, both for black holes [7] [8] [9] and for cosmological horizons [10].…”

Section: Introductionmentioning

confidence: 99%

Conformally rescaled spacetimes and Hawking radiation

Nielsen

Firouzjaee

2013

Gen Relativ Gravit

Self Cite

View full text Add to dashboard Cite

Abstract. We study various derivations of Hawking radiation in conformally rescaled metrics. We focus on two important properties, the location of the horizon under a conformal transformation and its associated temperature. We find that the production of Hawking radiation cannot be associated in all cases to the trapping horizon because its location is not invariant under a conformal transformation. We also find evidence that the temperature of the Hawking radiation should transform simply under a conformal transformation, being invariant for asymptotic observers in the limit that the conformal transformation factor is unity at their location.

show abstract

Black holes and black hole thermodynamics without event horizons

Cited by 63 publications

References 118 publications

Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

Slicing dependence of nonspherically symmetric quasilocal horizons in Vaidya spacetimes

WIMT in Gullstränd–Painlevé and Reissner–Nordström metrics: induced stable gravito-magnetic monopoles

Conformally rescaled spacetimes and Hawking radiation

Contact Info

Product

Resources

About