Traversable wormholes in Einsteinian cubic gravity

Mehdizadeh, Mohammad; Ziaie, Amir Hadi

doi:10.1142/s0217732320500170

Cited by 31 publications

(20 citation statements)

References 67 publications

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“…In this appendix we present the explicit form of the quartic and quintic GQTG and Quasitopological densities used in Section 3 to construct the recursive relations in eqs. (24) and (27).…”

Section: Final Commentsmentioning

confidence: 99%

(Generalized) quasi-topological gravities at all orders

Bueno¹,

Cano²,

Hennigar³

2019

Class. Quantum Grav.

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A new class of higher-curvature modifications of D(≥ 4)-dimensional Einstein gravity has been recently identified. Densities belonging to this "Generalized quasi-topological" class (GQTGs) are characterized by possessing non-hairy generalizations of the Schwarzschild black hole satisfying g tt g rr = −1 and by having second-order equations of motion when linearized around maximally symmetric backgrounds. GQTGs for which the equation of the metric function f (r) ≡ −g tt is algebraic are called "Quasi-topological" and only exist for D ≥ 5. In this paper we prove that GQTG and Quasi-topological densities exist in general dimensions and at arbitrarily high curvature orders. We present recursive formulas which allow for the systematic construction of n-th order densities of both types from lower order ones, as well as explicit expressions valid at any order. We also obtain the equation satisfied by f (r) for general D and n. Our results here tie up the remaining loose end in the proof presented in arXiv:1906.00987 that every gravitational effective action constructed from arbitrary contractions of the metric and the Riemann tensor is equivalent, through a metric redefinition, to some GQTG.

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“…In this appendix we present the explicit form of the quartic and quintic GQTG and Quasitopological densities used in Section 3 to construct the recursive relations in eqs. (24) and (27).…”

Section: Final Commentsmentioning

confidence: 99%

(Generalized) quasi-topological gravities at all orders

Bueno¹,

Cano²,

Hennigar³

2019

Class. Quantum Grav.

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“…In Appendix A, we show how one can obtain Eq. (15). We suppose that action (14) has an asymptotically (A)dS solution aroundḡ ab for which…”

Section: Conserved Quantitiesmentioning

confidence: 99%

“…Recently, a cubic order curvature model with contribution in four dimensions called Einsteinian cubic gravity (ECG) has been proposed [4]. This model has attracted a lot of attention [5][6][7][8][9][10][11][12][13][14][15][16][17][18][19]. ECG respects some of the constraints that Lovelock theories have.…”

Section: Introductionmentioning

confidence: 99%

Topological Born–Infeld charged black holes in Einsteinian cubic gravity

Zangeneh

Kazemi

2020

Eur. Phys. J. C

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In this paper, we study four-dimensional topological black hole solutions of Einsteinian cubic gravity in the presence of nonlinear Born–Infeld electrodynamics and a bare cosmological constant. First, we obtain the field equations which govern our solutions. Employing Abbott–Deser–Tekin and Gauss formulas, we present the expressions of conserved quantities, namely total mass and total charge of our topological black solutions. We disclose the conditions under which the model is unitary and perturbatively free of ghosts with asymptotically (A)dS and flat solutions. We find that, for vanishing bare cosmological constant, the model is unitary just for asymptotically flat solutions, which only allow horizons with spherical topology. We compute the temperature for these solutions and show that it always has a maximum value, which decreases as the values of charge, nonlinear coupling or cubic coupling grows. Next, we calculate the entropy and electric potential. We show that the first law of thermodynamics is satisfied for spherical asymptotically flat solutions. Finally, we peruse the effects of model parameters on thermal stability of these solutions in both canonical and grand canonical ensembles.

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“…After this direction has emerged, various authors have investigated different properties of the Einsteinian cubic gravity or in similar approaches, analyzing the black-holes solutions [22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38][39]. Moreover, for this scenario, the wormholes properties have been addressed in [40,41]. In general the cubic gravity term is expected to have a considerable influence especially at early times during the inflationary epoch [42].…”

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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Traversable wormholes in Einsteinian cubic gravity

Cited by 31 publications

References 67 publications

(Generalized) quasi-topological gravities at all orders

(Generalized) quasi-topological gravities at all orders

Topological Born–Infeld charged black holes in Einsteinian cubic gravity

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

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