Brane cosmological evolution with a general bulk matter configuration

Apostolopoulos, Pantelis S.; Tetradis, N.

doi:10.1103/physrevd.71.043506

Cited by 44 publications

(60 citation statements)

References 29 publications

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“…Cosmological evolution has been extensively studied in this scenario (for symmetric embeddings see [7], [8] and references therein; for asymmetric embeddings [3], [9] and references therein). The matter in the bulk affects the cosmological evolution on the brane through a "comoving mass" and a bulk pressure [10], [11].…”

Section: Introductionmentioning

confidence: 99%

Black holes and dark energy from gravitational collapse on the brane

Gergely

2007

J. Cosmol. Astropart. Phys.

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The gravitational collapse of a pressureless fluid in general relativity (Oppenheimer-Snyder collapse) results in a black hole. The study of the same phenomenon in the brane-world scenario has shown that the exterior of the collapsing dust sphere cannot be static. We show that by allowing for pressure, the exterior of a fluid sphere can be static. The gravitational collapse on the brane proceeds according to the modified gravitational dynamics, turning the initial nearly dust-like configuration into a fluid with tension. The tension arises from the non-linearity of the dynamical equations in the energy-momentum tensor, and it vanishes in the general relativistic limit. Below the horizon the tension turns the star into dark energy. This transition occurs right below the horizon for astrophysical black holes and far beyond the horizon for intermediate mass and galactic black holes. Further, both the energy density and the tension increase towards infinite values during the collapse. The infinite tension however could not stop the formation of the singularity.

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Section: Introductionmentioning

confidence: 99%

Black holes and dark energy from gravitational collapse on the brane

Gergely

2007

J. Cosmol. Astropart. Phys.

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“…For latter use, it is convenient to perform an 1+3 decomposition of the above tensors into irreducible parts with respect to the brane fluid velocityũ α ≡ g A αũA . The decomposition of the bulk EM tensor reads [18] T bulk AB =ρũ AũB +ph AB + 2q (AũB) +π AB ,…”

Section: The Effect Of Bulk Matter On a Brane With Induced Gravitymentioning

confidence: 99%

“…wherep = T bulk AB n A n B is the bulk pressure in the direction perpendicular to the brane as measured by a brane observer [18]. The traceless tensorπ αβ is the contribution from the bulk anisotropic pressure to the effective 4-dimensional gravitational field.…”

Section: The Effect Of Bulk Matter On a Brane With Induced Gravitymentioning

confidence: 99%

“…In the absence of induced gravity on a Friedmann-Robertson-Walker (FRW) brane and for an AdS-Schwarzschild bulk, the size of this contribution is related to the mass of the black hole [17]. In the general case of an arbitrary bulk content, it is the total integrated mass in the bulk that determines the dark radiation [18]. The term in the Friedmann equation for the brane cosmological evolution does not, in general, scale ∼ ℓ −4 , where ℓ is the scale factor.…”

Section: Introductionmentioning

confidence: 99%

“…The term in the Friedmann equation for the brane cosmological evolution does not, in general, scale ∼ ℓ −4 , where ℓ is the scale factor. For this reason, this term has been characterized as generalized dark radiation [18,19]. Several examples of non-standard scaling are known [20,21,22].…”

Section: Introductionmentioning

confidence: 99%

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Late acceleration andw=−1crossing in induced gravity

Apostolopoulos

Tetradis

2006

Phys. Rev. D

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We study the cosmological evolution on a brane with induced gravity within a bulk with arbitrary matter content. We consider a Friedmann-Robertson-Walker brane, invariantly characterized by a six-dimensional group of isometries. We derive the effective Friedmann and Raychaudhuri equations. We show that the Hubble expansion rate on the brane depends on the covariantly defined integrated mass in the bulk, which determines the energy density of the generalized dark radiation. The Friedmann equation has two branches, distinguished by the two possible values of the parameter ǫ = ±1. The branch with ǫ = 1 is characterized by an effective cosmological constant and accelerated expansion for low energy densities. Another remarkable feature is that the contribution from the generalized dark radiation appears with a negative sign. As a result, the presence of the bulk corresponds to an effective negative energy density on the brane, without violation of the weak energy condition. The transition from a period of domination of the matter energy density by nonrelativistic brane matter to domination by the generalized dark radiation corresponds to a crossing of the phantom divide w = −1.

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Inhomogeneous brane models

Apostolopoulos,

Naidoo

2024

Gen Relativ Gravit

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Brane cosmological evolution with a general bulk matter configuration

Cited by 44 publications

References 29 publications

Black holes and dark energy from gravitational collapse on the brane

Black holes and dark energy from gravitational collapse on the brane

Late acceleration andw=−1crossing in induced gravity

Inhomogeneous brane models

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