Note on the dynamical features for the extended 
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 cubic gravity

Marciu, Mihai

doi:10.1103/physrevd.101.103534

Cited by 41 publications

(13 citation statements)

References 45 publications

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“…Ref [9] reported a novel extension of ECG in which the Ricci scalar in the action is replaced by a function of the curvature invariant P which represents the contractions of the Riemann tensor at the cubic order. This class of modified gravity theory have been very successful in several cosmological domains such as inflation [23], spherically symmetric black hole solutions [20][21][22], and late-time acceleration [9,12]. Energy conditions are interesting linear relationships between pressure and density and have been extensively employed to derive interesting results in Einstein's gravity.…”

Section: Introductionmentioning

confidence: 99%

Energy Conditions in $f(P)$ Gravity

Bhattacharjee

2021

Preprint

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f (P ) gravity is a novel extension of ECG in which the Ricci scalar in the action is replaced by a function of the curvature invariant P which represents the contractions of the Riemann tensor at the cubic order [9]. The present work is concentrated on bounding some f (P ) gravity models using the concept of energy conditions where the functional forms of f (P ) are represented as a) f (P ) = α √ P , and b) f (P ) = α exp(P ), where α is the sole model parameter. Energy conditions are interesting linear relationships between pressure and density and have been extensively employed to derive interesting results in Einstein's gravity, and are also an excellent tool to impose constraints on any cosmological model. To place the bounds, we ensured that the energy density must remain positive, the pressure must remain negative, and the EoS parameter must attain a value close to −1 to make sure that the bounds respect the accelerated expansion of the Universe and are also in harmony with the latest observational data. We report that for both the models, suitable parameter spaces exist which satisfy the aforementioned conditions and therefore posit the f (P ) theory of gravity to be a promising modified theory of gravitation.

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Section: Introductionmentioning

confidence: 99%

Energy Conditions in $f(P)$ Gravity

Bhattacharjee

2021

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“…The extended cubic gravity based on the third order contractions of the Riemann tensor has been proposed recently [51], a theory which further corrects the Einstein-Hilbert action with a generic functional f (P) which encodes specific effects due to the topological invariant P. In this case the topological invariant P is based on some specific contractions of the Riemann tensor [51]. The dynamical features for the generalized extended cubic gravity have been addressed in [52], by taking into account two possible configurations for the cubic term which corrects the Einstein-Hilbert action. An alternative proposal has been analyzed in [53] for the Einsteinian cubic gravity, a specific theory which also includes a cosmological constant.…”

Section: Introductionmentioning

confidence: 99%

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

Marciu

2021

Eur. Phys. J. C

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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.

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“…In [5], the authors generalized the ECG by substituting the Ricci scalar in the Einstein-Hilbert action with a suitable function of the curvature invariant P which denotes the cubic contractions of the Riemann tensor. Thereafter, f (P ) gravity have been successfully applied to explain the late-time acceleration [5,6], spherically symmetric black hole solutions [7], and inflation [8]. Recently, tight constraints on f (P ) gravity have been reported from the energy conditions [9].…”

Section: Introductionmentioning

confidence: 99%

Baryogenesis in $f(P)$ Gravity

Bhattacharjee

2021

Preprint

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In this work, we investigate gravitational baryogenesis in the framework of f (P ) gravity to understand the applicability of this class of modified gravity in addressing the baryon asymmetry of the Universe. For the analysis, we set f (P ) = αP where α is the model parameter. We found that in f (P ) gravity, the CP-violating interaction acquires a modification through the addition of the nontopological cubic term P in addition to the Ricci scalar R and the mathematical expression of the baryon-to-entropy ratio depends not only on the time derivative of R but also the time derivative of P . Additionally, we also investigate the consequences of a more complete and generalized CP-violating interaction proportional to f (P ) instead of P in addressing the baryon asymmetry of the Universe. For this type of interaction, we report that the baryon-to-entropy ratio is proportional to Ṙ, Ṗ and f (P ). We report that for both of these cases, rational values of α and χ generate acceptable baryon-to-entropy ratios compatible with observations.

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Note on the dynamical features for the extended f(P) cubic gravity

Cited by 41 publications

References 45 publications

Energy Conditions in $f(P)$ Gravity

Energy Conditions in $f(P)$ Gravity

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

Baryogenesis in $f(P)$ Gravity

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