Density perturbations with relativistic thermodynamics

Maartens, Roy; Triginer, Josep

doi:10.1103/physrevd.56.4640

Cited by 97 publications

(123 citation statements)

References 25 publications

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“…which is not invariant under equation (39). However it proves very useful in categorizing spacetimes [44] and vanishes in Petrov type-III and type-N spacetimes [13] (supporting the existence of gravitational waves in these spacetimes, since the analogous quantities vanish for purely radiative electromagnetic fields).…”

Section: The Bianchi Identities and Nonlinear Dualitymentioning

confidence: 99%

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Gravito-electromagnetism

Maartens

Bassett

1998

Class. Quantum Grav.

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245

353

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Abstract.We develop and apply a fully covariant 1 + 3 electromagnetic analogy for gravity. The free gravitational field is covariantly characterized by the Weyl gravito-electric and gravito-magnetic spatial tensor fields, whose dynamical equations are the Bianchi identities. Using a covariant generalization of spatial vector algebra and calculus to spatial tensor fields, we exhibit the covariant analogy between the tensor Bianchi equations and the vector Maxwell equations. We identify gravitational source terms, couplings and potentials with and without electromagnetic analogues. The nonlinear vacuum Bianchi equations are shown to be invariant under covariant spatial duality rotation of the gravito-electric and gravito-magnetic tensor fields. We construct the super-energy density and super-Poynting vector of the gravitational field as natural U (1) group invariants, and derive their super-energy conservation equation. A covariant approach to gravito-electric/magnetic monopoles is also presented.

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Section: The Bianchi Identities and Nonlinear Dualitymentioning

confidence: 99%

“…In the case where spacetime is almost spatially isotropic and homogeneous, i.e. a linearized perturbation of a Friedmann-Lemaitre-Robertson-Walker (FLRW) background, some of the main further identities take the linearized form [38,39] (…”

Section: Covariant Spatial Vector and Tensor Calculusmentioning

confidence: 99%

Gravito-electromagnetism

Maartens

Bassett

1998

Class. Quantum Grav.

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245

353

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“…The sources in the r.h.s. of equation (35) arising respectively from entropy perturbations, bulk viscous stress, energy flux, and shear viscous stress are given in [60]. Since in our case there are no shear viscous stress (σ ij = 0) and S[q] vanishes by choosing the energy frame (q i = 0), we reproduce here only the expressions for S[e] and S[π],…”

Section: Density Perturbationsmentioning

confidence: 99%

“…Also the comoving expansion gradient, the normalized pressure gradient, and normalized entropy gradient are defined by [57,60] …”

Section: Density Perturbationsmentioning

confidence: 99%

Quintessence dissipative superattractor cosmology

Chimento¹,

Jakubi²,

Zuccalá³

2001

Phys. Rev. D

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We investigate the simplest quintessence dissipative dark matter attractor cosmology characterized by a constant quintessence baryotropic index and a power-law expansion. We show that a class of accelerated coincidence-solving attractor solutions converge into this asymptotic behavior. Despite of its simplicity, such "superattractor" regime provides a model of the recent universe that also exhibits an excellent fit to supernovae luminosity observations and no age conflict. Our best fit gives α = 1.71 ± 0.29 for the power-law exponent. We calculate for this regime the evolution of density and entropy fluctuations. PACS number(s): 98.80.Hw, 04.20Jb 1

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“…homogeneity and isotropy) or small perturbations around it [49]. The Einstein field equations for homogeneous models with dissipative fluids can be decoupled and therefore are reduced to an autonomous system of first order ordinary differential equations, which can be analyzed qualitatively [50], [51].…”

Section: Introductionmentioning

confidence: 99%

Viscous Bianchi type I universes in brane cosmology

Harkó¹,

Mak²

2003

Class. Quantum Grav.

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We consider the dynamics of a viscous cosmological fluid in the generalized Randall-Sundrum model for an anisotropic, Bianchi type I brane. To describe the dissipative effects we use the IsraelHiscock-Stewart full causal thermodynamic theory. By assuming that the matter on the brane obeys a linear barotropic equation of state, and the bulk viscous pressure has a power-law dependence on the energy density, the general solution of the field equations can be obtained in an exact parametric form. The obtained solutions describe generally a non-inflationary brane world. In the large time limit the brane Universe isotropizes, ending in an isotropic and homogeneous state. The evolution of the temperature and of the comoving entropy of the Universe is also considered, and it is shown that due to the viscous dissipative processes a large amount of entropy is created in the early stages of evolution of the brane world.

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Density perturbations with relativistic thermodynamics

Cited by 97 publications

References 25 publications

Gravito-electromagnetism

Gravito-electromagnetism

Quintessence dissipative superattractor cosmology

Viscous Bianchi type I universes in brane cosmology

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