Quantum origin of inflation in the geometric inflation model

Quirós, Israel; Arcia, Roberto De; García-Salcedo, Ricardo; González, Tamé; Cedeño, Francisco X. Linares; Nucamendi, Ulises

doi:10.1103/physrevd.103.064043

Cited by 11 publications

(4 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Among other things, it was found that the aforementioned cubic theory yields equations of motion for scalar perturbations on top of FLRW backgrounds which are of second order in time derivatives [80] and that they provide a mechanism for cosmic inflation devoid of additional fields to the metric [79,[81][82][83][84]. For other aspects of these theories, we refer the reader to [85][86][87][88][89][90] and references therein. Also, in the context of theories fulfilling a holographic c-theorem, higher-order gravities with second-order equations on top of FLRW backgrounds were derived at any curvature order in D = 3 [77], while for generic dimensions a recursive algorithm to find Cosmological Gravities at all curvature orders (although with explicit covariant derivatives of the curvature) was provided in [78].…”

Section: Introductionmentioning

confidence: 99%

Cosmological higher-curvature gravities

Moreno,

Murcia Gil

2024

Class. Quantum Grav.

View full text Add to dashboard Cite

We examine higher-curvature gravities whose FLRW conﬁgurations are speciﬁed by equations of motion which are of second order in derivatives, just like in Einstein gravity. We name these theories Cosmological Gravities and initiate a systematic exploration in dimensions D ≥ 3. First, we derive an instance of Cosmological Gravity to all curvature orders and dimensions D ≥ 3. Second, we study Cosmological Gravities admitting non-hairy generalizations of the Schwarzschild solution characterized by a single function whose equation of motion is, at most, of second order in derivatives. We present explicit instances of such theories for all curvature orders and dimensions D ≥ 4. Finally, we investigate the equations of motion for cosmological perturbations in the context of generic Cosmological Gravities. Remarkably, we ﬁnd that the linearized equations of motion for scalar cosmological perturbations in any Cosmological Gravity in D ≥ 3 contain no more than two time derivatives. We explicitly corroborate this aspect by presenting the equations for the scalar perturbations in some four-dimensional Cosmological Gravities up to ﬁfth order in the curvature.

show abstract

Section: Introductionmentioning

confidence: 99%

Cosmological higher-curvature gravities

Moreno,

Murcia Gil

2024

Class. Quantum Grav.

View full text Add to dashboard Cite

show abstract

“…Recently, various black hole solutions have been investigated in the Einsteinian cubic gravity theory [29,[35][36][37][38][39]. Furthermore, the properties of the inflationary era have been analyzed in some specific theories [40][41][42][43][44][45][46]. The coupling of a scalar field with a cubic term has been investigated by considering a dynamical system analysis [47].…”

Section: Introductionmentioning

confidence: 99%

Tachyonic cosmology with cubic contractions of the Riemann tensor

Marciu¹

2022

Preprint

View full text Add to dashboard Cite

A new cosmological theory is proposed in the theoretical framework of modified gravity theories which is based on a tachyonic field non-minimally coupled with a specific topological invariant constructed with third order contractions of the Riemann tensor. After proposing the action of the cosmological model, the modified Friedmann relations and the Klein-Gordon equations are obtained, describing the corresponding geometrical corrections to the Einstein-Hilbert action. The physical features of the cosmological system are investigated by adopting the dynamical system analysis in the case of an exponential function for the geometrical coupling term. The investigation revealed that the cosmological system can explain the current accelerated expansion of the Universe and the matter dominated epoch, showing a high compatibility to the recent history of our Universe for various values of the coupling coefficients.

show abstract

“…In general the cubic gravity term is expected to have a considerable influence especially at early times during the inflationary epoch [42]. The effects due to the cubic term in the inflationary epoch have been studied intensively in the last years [42][43][44][45][46]. In Ref.…”

Section: Introductionmentioning

confidence: 99%

Dark effects in $$\tilde{f}(R,P)$$ gravity

Marciu

2021

Eur. Phys. J. C

View full text Add to dashboard Cite

In the present paper a new cosmological model is proposed by extending the Einstein–Hilbert Lagrangian with a generic functional $$\tilde{f}(R,P)$$ f ~ ( R , P ) , which depends on the scalar curvature R and a term P which encodes a possible influence from specific cubic contractions of the Riemann tensor. After proposing the corresponding action, the associated modified Friedmann relations are deduced, in the case where the generic functional has the following decomposition, $$\tilde{f}(R,P)=f(R)+g(P)$$ f ~ ( R , P ) = f ( R ) + g ( P ) . The present study takes into account the power-law and the exponential decomposition for the specific form of the corresponding generic functional. For the analytical approach the specific method of dynamical system analysis is employed, revealing the fundamental properties of the phase space structure, discussing the dynamical consequences for the cosmological solutions obtained. It is revealed that the cosmological solutions associated to the critical points can explain various dynamical eras, with a high sensitivity to the values of the corresponding parameters, encoding different effects due to the geometrical nature of the specific couplings.

show abstract

Quantum origin of inflation in the geometric inflation model

Cited by 11 publications

References 47 publications

Cosmological higher-curvature gravities

Cosmological higher-curvature gravities

Tachyonic cosmology with cubic contractions of the Riemann tensor

Dark effects in $$\tilde{f}(R,P)$$ gravity

Contact Info

Product

Resources

About