Asymptotically FRW black holes

Firouzjaee, Javad T.; Mansouri, Reza

doi:10.1007/s10714-010-0991-7

Cited by 43 publications

(67 citation statements)

References 48 publications

(103 reference statements)

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“…Taking the linear case f (T ) = T , the second and third equations of (42) yield again the constraint (29) well known in the metric of LTB. In order to compare with the example taken in the diagonal case, we put p r = p t = 0 in (14) and rewrite the first equation of (42) as…”

Section: Dust-dominated Universementioning

confidence: 99%

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Inhomogeneous universe in f(T) theory

et al. 2014

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We obtain the equations of motions of the f (T ) theory considering the Lemaître-TolmanBondi's metric for a set of diagonal and non-diagonal tetrads. In the case of diagonal tetrads the equations of motion of the f (T ) theory impose a constant torsion or the same equations of the General Relativity, while in the case of non-diagonal set the equations are quite different from that obtained in GR. We show a simple example of an universe dominated by the matter for the two cases. The comparison of the mass in the non-diagonal case shows a sort of increased with respect to the diagonal one. We also perform two examples for the nondiagonal case. The first concerns a black hole solution of type Sshwarzschild which presents a temperature higher than that of Schwarzschild, and a black hole in a dust-dominated universe.

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Section: Dust-dominated Universementioning

confidence: 99%

“…A particular case of these solutions is that of LT [8]. The models have been used in redshift drift [10], CMB [11], interpretation of supernova observations [12], averaging [13], formation of black holes [14], of galaxy clusters [15], superclusters [16], cosmic voids [18] and collapse from the perspective of loop quantum gravity [17].…”

Section: Introductionmentioning

confidence: 99%

Inhomogeneous universe in f(T) theory

et al. 2014

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“…And second many unknowns remains regarding collapsing structures and the process of formation of a black hole. Constructing such cosmological collapsing structures is not only useful to explore non-linear effect of GR but also to explore quasi-local features of that structure such as masses and horizons [5], black hole thermodynamics and Hawking radiation [6][7][8][9] or the validity of the weak field approximation [10].…”

Section: Introductionmentioning

confidence: 99%

“…It is furthermore possible to (asymptotically) recover the FLRW metric from the LTB one for a suitable choice of the free functions of the LTB metric. The LTB metric has been applied to various physical systems ranging from modeling radial inhomogeneities [38] or fractal pattern [39] on cosmological scales, to investigate singularity theorems or nucleus in nuclear physics [40], it is shown in [5,41] that the LTB metric admits a cosmological black hole solution.…”

Section: Introductionmentioning

confidence: 99%

Charged cosmological black hole

et al. 2017

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The cosmological black holes are black holes living not in an asymptotically flat universe but in an expanding spacetime. They have a rich dynamics in particular for their mass and horizon. In this article we perform a natural step in investigating this new type of black hole: we consider the possibility of a charged cosmological black hole. We derive the general equations of motion governing its dynamics and report a new analytic solution for the special case of the charged Lematre-TolmanBondi equations of motion that describe a charged cosmological black hole. We then study various relevant quantities for the characterization of the black hole such as the C-function, the effect of the charge on the black hole flux and the nature of the singularity. We also perform numerical investigations to strengthen our results. Finally we challenge a model of gamma ray burst within our framework. * Rahim.Moradi@icranet.org † clement.stahl@pucv.cl ‡ j.taghizadeh.f@ipm.ir § xue@icra.it 2

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“…There is however another area in the cosmology and astrophysics where general relativistic effects may come in without being in a strong gravity regime. This happens when one is dealing with non-local or large scale phenomena [7][8][9][10]12]. The expansion of the universe, as an example, is a general relativistic effect at large scale in a very weak gravity regime: assuming any non-zero density, however small it may be, Einstein equations lead to a non-static expanding universe, in contrast to the Newtonian gravity.…”

Section: Introductionmentioning

confidence: 99%

Relativistic virial relation for cosmological structures

2016

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Starting with the relativistic Boltzmann equation for a system of particles defined by a distribution function, we have derived the virial relation for a spherical structure within an expanding background in the context of general relativity. This generalized form of the virial relation is then applied to the static case of a spherically symmetric structure to see the difference in the simplest case to the Newtonian relation. A relativistic Mass-Temperature relation for this simple case is also derived which can be applied to compact objects in astrophysics. Our general virial relation is then applied to the non-static case of a structure within an expanding universe where an extra term, usually missed in studies of structures in the presence of the dark energy, appears. *

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Asymptotically FRW black holes

Cited by 43 publications

References 48 publications

Inhomogeneous universe in f(T) theory

Inhomogeneous universe in f(T) theory

Charged cosmological black hole

Relativistic virial relation for cosmological structures

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