2020
DOI: 10.3847/1538-4357/ab6a10
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Gauss–Bonnet Inflation after Planck2018

Abstract: We study the primordial perturbations and reheating process in the models where the Gauss-Bonnet term is non-minimally coupled to the canonical and non-canonical (DBI and tachyon) scalar fields. We consider several potentials and Gauss-Bonnet coupling terms as power-law, dilaton-like, cosh-type, E-model and T-model. To seek the observational viability of these models, we study the scalar perturbations numerically and compare the results with the Planck2018 TT, TE, EE+lowE+lensing+BK14+BAO joint data at 68% CL … Show more

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Cited by 39 publications
(15 citation statements)
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References 131 publications
(192 reference statements)
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“…There are a lot of inflationary scenarios in Einstein-Gauss-Bonnet gravity . The most of them includes a constant function F [63][64][65][66][67][68][69]71,73,[75][76][77][78][79][80][81][82]86]. Note that for models with a constant F, the problem of reconstructing the function V and ξ from the observational data has been considered in Ref.…”
Section: Introductionmentioning
confidence: 99%
“…There are a lot of inflationary scenarios in Einstein-Gauss-Bonnet gravity . The most of them includes a constant function F [63][64][65][66][67][68][69]71,73,[75][76][77][78][79][80][81][82]86]. Note that for models with a constant F, the problem of reconstructing the function V and ξ from the observational data has been considered in Ref.…”
Section: Introductionmentioning
confidence: 99%
“…At present, the interest in inflationary scenarios in the cosmological models with Gauss-Bonnet term is growing [25][26][27][28][29][30][31][32][33][34][35]. In the present paper, we construct a gravity model with the Gauss-Bonnet term multiplied by a function of a scalar field which allows one to reconstruct expressions for the spectral index and the tensor-to-scalar ratio from cosmological attractor models in the slow-roll regime.…”
Section: Introductionmentioning
confidence: 99%
“…In this simple model, the dominant modes of the primordial perturbations are predicted to be scale-invariant, adiabatic and Gaussian [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46]. However, there is a lot of attention to the extended inflation models predicting the non-Gaussian distributed perturbations [46][47][48][49][50][51][52][53][54][55].…”
Section: Introductionmentioning
confidence: 99%