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De Sitter solutions in Einstein-Gauss-Bonnet gravity
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De Sitter solutions play an important role in cosmology because the knowledge of unstable de Sitter solutions can be useful to describe inflation, whereas stable de Sitter solutions are often used in models of late-time acceleration of the Universe. The Einstein-Gauss-Bonnet gravity cosmological models are actively used both as inflationary models and as dark energy models. To modify the Einstein equations one can add a nonlinear function of the Gauss-Bonnet term or a function of the scalar field multiplied on the Gauss-Bonnet term. The effective potential method essentially simplifies the search and stability analysis of de Sitter solutions, because the stable de Sitter solutions correspond to minima of the effective potential.
Forward citations
Cited by 5 Pith papers
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Unstable de Sitter inflationary solution in sixth-order gravity
For the sixth-order gravity action (2.1), the exact FLRW de Sitter solution is unstable whenever 3γ1+γ2<0, while the second-order limit admits a stable de Sitter attractor.
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Einstein--Gauss--Bonnet Inflationary Cosmology in Phase-$\theta$ Formalism
Phase-θ formalism maps EGB inflation backgrounds to closed-form observables beyond slow-roll; Starobinsky+linear-GB fits ACT DR6 ns and r while predicting a DECIGO-accessible GW plateau.
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From Quantum Correlations to Inflationary Tracking Scalar Field Evolution
The author argues, via condensed-matter-style analogies, that the inflationary tracking condition emerges when the correlation length of primordial quantum degrees of freedom scales as a power of the Hubble radius.
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GW170817 Viable Einstein-Gauss-Bonnet Inflation Compatible with the Atacama Cosmology Telescope Data
Einstein-Gauss-Bonnet inflation models with tuned small couplings can reproduce the ACT scalar spectral index and the Planck tensor-to-scalar ratio bound while keeping the gravitational wave speed within the GW170817 limit.
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On the stability of de Sitter inflationary solution in the Starobinsky-Bel-Robinson gravity
The exact de Sitter solution of Starobinsky-Bel-Robinson gravity is fixed by the quartic Bel-Robinson coupling alone and is an unstable saddle point for the physically allowed positive sign of the R^2 coefficient.
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