2013
DOI: 10.1142/s0218271813500557
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Quintessential and Phantom Power-Law Solutions in Scalar Tensor Model of Dark Energy

Abstract: We consider a scalar-tensor model of dark energy with kinetic and Gauss Bonnet couplings. We study the conditions for the existence of quintessential and phantom power-law expansion, and also analyze these conditions in absence of potential (closely related to string theory). A mechanism to avoid the Big Rip singularity in various asymptotic limits of the model has been studied. It was found that the kinetic and Gauss-Bonnet couplings might prevent the Big Rip singularity in a phantom scenario. The autonomous … Show more

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Cited by 11 publications
(18 citation statements)
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“…Combining this outcome with the previously noted η < 0, it follows that γ must be a negative quantity and hence the reason for the minus sign in Eq. (33). Thus, the signs η < 0 and γ < 0 become uniquely fixed.…”
Section: B Determination Of the Higgs Potentialmentioning
confidence: 92%
See 2 more Smart Citations
“…Combining this outcome with the previously noted η < 0, it follows that γ must be a negative quantity and hence the reason for the minus sign in Eq. (33). Thus, the signs η < 0 and γ < 0 become uniquely fixed.…”
Section: B Determination Of the Higgs Potentialmentioning
confidence: 92%
“…This equation is remarkable since it links in a specific way the expected large value of ω in BD-gravity with a possible mild "running" of the gravitational "constant", G, which is controlled by the coefficient γ in the third scaling relation (17). In particular, we can see from (33) that ω → ∞, if and only if γ → 0, which is the limit of GR in which G =const. We will come back to this point in the next section.…”
Section: B Determination Of the Higgs Potentialmentioning
confidence: 93%
See 1 more Smart Citation
“…So this model could describe an inflationary de Sitter solution that can evolve towards scaling solutions with saddle character or to stable attractor dominated by the scalar field, describing accelerated expansion [89]. Thus, the present model can provide a connection between early time inflation and late time accelerated expansion (in [90] special cases of quintessence and phantom solutions have been studied with exponential couplings). For unified description of early time inflation and late time accelerated expansion in the framework of scalar tensor theories see [91].…”
Section: Introductionmentioning
confidence: 87%
“…One important term appearing in the Horndeski Lagrangian is the kinetic coupling of a scalar field to curvature. This derivative coupling of matter to gravity has interesting cosmological implications, acting as a friction term in the early inflationary cosmological evolution [5][6][7][8][9]. Observational tests of inflation with a field coupled to Einstein tensor were presented in [10].…”
mentioning
confidence: 99%