1997
DOI: 10.1103/physrevd.56.4640
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Density perturbations with relativistic thermodynamics

Abstract: We investigate cosmological density perturbations in a covariant and gauge-invariant formalism, incorporating relativistic causal thermodynamics to give a self-consistent description. The gradient of density inhomogeneities splits covariantly into a scalar part, equivalent to the usual density perturbations, a rotational vector part that is determined by the vorticity, and a tensor part that describes the shape. We give the evolution equations for these parts in the general dissipative case. Causal thermodynam… Show more

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Cited by 97 publications
(123 citation statements)
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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%
See 1 more Smart Citation
“…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%
“…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%
“…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%
“…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%