<i>Homogeneous Relativistic Cosmologies</i>

Ryan, Maria; Shepley, L. C.; MacCallum, Malcolm

doi:10.1063/1.3023430

Cited by 15 publications

(25 citation statements)

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“…see for example Ellis andMacCallum (1969), MacCallum (1971), Collins (1971), Stephani et al (2003), Petrov (1969, Ryan and Shapley (1975), Raychaudhuri (1979). For a perfect fluid with energy-momentum tensor:…”

Section: The Model(s)mentioning

confidence: 96%

About Bianchi I with VSL

Belinchón

2008

Astrophys Space Sci

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In this paper we study how to attack, through different techniques, a perfect fluid Bianchi I model with variable G,c and Lambda, but taking into account the effects of a $c$-variable into the curvature tensor. We study the model under the assumption,div(T)=0. These tactics are: Lie groups method (LM), imposing a particular symmetry, self-similarity (SS), matter collineations (MC) and kinematical self-similarity (KSS). We compare both tactics since they are quite similar (symmetry principles). We arrive to the conclusion that the LM is too restrictive and brings us to get only the flat FRW solution. The SS, MC and KSS approaches bring us to obtain all the quantities depending on \int c(t)dt. Therefore, in order to study their behavior we impose some physical restrictions like for example the condition q<0 (accelerating universe). In this way we find that $c$ is a growing time function and Lambda is a decreasing time function whose sing depends on the equation of state, w, while the exponents of the scale factor must satisfy the conditions $\sum_{i=1}^{3}\alpha_{i}=1$ and $\sum_{i=1}^{3}\alpha_{i}^{2}<1,$ $\forall\omega$, i.e. for all equation of state$,$ relaxing in this way the Kasner conditions. The behavior of $G$ depends on two parameters, the equation of state $\omega$ and $\epsilon,$ a parameter that controls the behavior of $c(t),$ therefore $G$ may be growing or decreasing.We also show that through the Lie method, there is no difference between to study the field equations under the assumption of a $c-$var affecting to the curvature tensor which the other one where it is not considered such effects.Nevertheless, it is essential to consider such effects in the cases studied under the SS, MC, and KSS hypotheses.Comment: 29 pages, Revtex4, Accepted for publication in Astrophysics & Space Scienc

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Section: The Model(s)mentioning

confidence: 96%

About Bianchi I with VSL

Belinchón

2008

Astrophys Space Sci

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“…[21][22][23][24][25][26] and [27][28][29][30]) using canonical methods [31][32][33][34][35][36]. It has been gradually enlarged, with many cosmological scenarios extensively reported in the published literature [2][3][4][5][6][7][8][9][10][11][12][13], with the following properties enhancing a significant motivation:…”

Section: Introductionmentioning

confidence: 99%

A supersymmetric Vista for quantum cosmology

Moniz

2006

Gen Relativ Gravit

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“…In terms of the coordinates (57) and in the ω i basis characteristic of the particular Bianchi model into consideration, the vierbein is given by e 0 0 = N (t), e i 0 = N i , and e j α = exp (u ( j) )δ α j , where the parenthesis means no summation. The corresponding rotation coefficients read [19,30] …”

Section: Bianchi Class a Modelsmentioning

confidence: 99%

Is the non-physical states conjecture valid?

et al. 2009

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The canonical quantization for N = 1 supergravity in the context of gravitational minisuperspace described by Gowdy T 3 and Bianchi class A cosmological models is analyzed in order to search for physical states. There are indeed physical states in the minisuperspace sector of the theory. This fact entails that the non-physical states conjecture has a restricted validity, and in consequence it cannot be considered a general result.

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Homogeneous Relativistic Cosmologies

Cited by 15 publications

References 0 publications

About Bianchi I with VSL

About Bianchi I with VSL

A supersymmetric Vista for quantum cosmology

Is the non-physical states conjecture valid?

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