HIGGS INFLATION IN f(Φ, R) THEORY

Chakravarty, Girish Kumar; Mohanty, Sanghamitra; Singh, Narayani P.

doi:10.1142/s0218271814500291

Cited by 13 publications

(15 citation statements)

References 82 publications

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“…In this section we will show that generalized non-minimally coupled inflation models ξ a R b [11] with the quantum corrected 4 -potential [12][13][14] can be reduced to the power law Starobinsky form. We consider the generalized non-minimal coupling ξ a R b and the quantum correction to quartic scalar potential 4(1+γ ) into the action…”

Section: Equivalence Of the Power Law Starobinsky Model With Generalimentioning

confidence: 99%

“…One can find similar equivalence between generalized Higgs-inflation models and the power law Starobinsky model whose common feature is violation of the global Weyl symmetry. A general scalar-curvature coupled ξφ a R b model was studied in [11]. The quantum correction on φ 4 -potential in Jordan frame was studied in [12][13][14] where the equivalence of the ξφ 2 R + λφ 4(1+γ ) model with 1 M 2 R β model was shown.…”

Section: Introductionmentioning

confidence: 99%

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Power law Starobinsky model of inflation from no-scale SUGRA

Chakravarty

Mohanty

2015

Physics Letters B

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We consider a power law $\frac{1}{M^2}R^{\beta}$ correction to Einstein gravity as a model of inflation. The interesting feature of this form of generalization is that small deviations from the Starobinsky limit $\beta=2$ can change the value of tensor to scalar ratio from $r \sim \mathcal{O}(10^{-3})$ to $r\sim \mathcal{O}(0.1)$. We find that in order to get large tensor perturbation $r\approx 0.1$ as indicated by BKP measurements, we require the value of $\beta \approx 1.83$ thereby breaking global Weyl symmetry. We show that the general $R^\beta$ model can be obtained from a SUGRA construction by adding a power law $(\Phi +\bar \Phi)^n$ term to the minimal no-scale SUGRA K\"ahler potential. We further show that this two parameter power law generalization of the Starobinsky model is equivalent to generalized non-minimal curvature coupled models with quantum corrected $\Phi^{4}$- potentials i.e. models of the form $\xi \Phi^{a} R^{b} + \lambda \Phi^{4(1+\gamma)}$ and thus the power law Starobinsky model is the most economical parametrization of such models.Comment: 6 pages, 4 figures, Matches version to appear in Phys. Lett.

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Section: Equivalence Of the Power Law Starobinsky Model With Generalimentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Power law Starobinsky model of inflation from no-scale SUGRA

Chakravarty

Mohanty

2015

Physics Letters B

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“…As a simple generalization of the R 2 inflation, many people (Martin et al 2014a,b,c;Codello et al 2014;Rinaldi et al 2014c,b,c;Motohashi 2014;Myrzakul et al 2015;Nojiri & Odintsov 2003, 2006Cognola et al 2008;Elizalde et al 2011;Bamba et al 2008Bamba et al , 2013Bamba et al , 2014Bamba & Odintsov 2015;Chakravarty et al 2013;Chakravarty & Mohanty 2014) have investigated the possibility of the power in R 2 to deviate slightly from two, named the R 2−q inflation, where q ≪ 1. The R 2−q inflation has been shown to be compatible with observations and predicts a larger scalar-to-tensor ratio than that in the R 2 inflation.…”

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confidence: 99%

Constraints on the combined models with R 2 − q $R^{2-q}$ inflation and viable f ( R ) $f(R)$ dark energy

Geng

Lee

Lin

2015

Astrophys Space Sci

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We investigate the observational constraints on the modified gravity, which combines the R 2−q inflation with the power-law (exponential) type of the viable f (R) dark energy models. We discuss the difference between the combined model and R 2−q gravity in the inflationary epoch and obtain the constraints on the deviation power q as well as the parameters in f (R) by using the CosmoMC package. The allowed ranges of the spectral index and tensor-to-scalar ratio from the Planck data are highly restricted, resulting in q < 2.66 × 10 −2 and 2.17 × 10 −2 for the power-law and exponential types of f (R) gravity, respectively.

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“…We start with a general Higgs inflationary scenario ξφ a R b in the framework of f (φ, R) gravity theory, which is a generalization of the Higgs inflation model ξφ 2 R [78]. In the light of discoveries by CMS [79] and ATLAS [80] it is of interest to consider the Standard Model Higgs boson as the candidate for inflaton.…”

Section: The Model ξφmentioning

confidence: 99%

Testing theories of gravity and supergravity with inflation and observations of the cosmic microwave background

Chakravarty

Mohanty

Lambiase

2017

Int. J. Mod. Phys. D

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Abstract. Cosmological and astrophysical observations lead to the emerging picture of a universe that is spatially flat and presently undertaking an accelerated expansion. The observations supporting this picture come from a range of measurements encompassing estimates of galaxy cluster masses, the Hubble diagram derived from type-Ia supernovae observations, the measurements of Cosmic Microwave Background radiation anisotropies, etc. The present accelerated expansion of the universe can be explained by admitting the existence of a cosmic fluid, with negative pressure. In the simplest scenario this unknown component of the universe, the Dark Energy, is represented by the cosmological constant (Λ), and accounts for about 70% of the global energy budget of the universe. The remaining 30% consists of a small fraction of baryons (4%) with the rest cold Dark Matter (CDM). The Lambda Cold Dark Matter (ΛCDM) model, i.e. General Relativity with cosmological constant, is in good agreement with observations. It can be assumed as the first step towards a new standard cosmological model. However, despite the satisfying agreement with observations, the ΛCDM model presents several lacks of congruence and shortcomings, and therefore theories beyond Einsteins General Relativity are called for. Many extensions of Einstein's theory of gravity have been studied and proposed with various motivations like the quest for a quantum theory of gravity to extensions of anomalies in observations at the solar system, galactic and cosmological scales. These extensions include adding higher powers of Ricci curvature R, coupling the Ricci curvature with scalar fields and generalized functions of R. In addition when viewed from the perspective of Supergravity (SUGRA) many of these theories may originate from the same SUGRA theory, but interpreted in different frames. SUGRA therefore serves as a good framework for organizing and generalizing theories of gravity beyond General Relativity. All these theories when applied to inflation (a rapid expansion of early Universe in which primordial gravitational waves might be generated and might still be detectable by the imprint they left or by the ripples that persist today) can have distinct signatures in the Cosmic Microwave Background radiation temperature and polarization anisotropies. We give a review of ΛCDM cosmology and survey the theories of gravity beyond Einsteins General Relativity, specially which arise from SUGRA, and study the consequences of these theories in the context of inflation and put bounds on the theories and the parameters therein from the observational experiments like PLANCK, Keck/BICEP etc. The possibility of testing these theories in the near future in CMB observations and new data coming from colliders like the LHC, provides an unique opportunity for constructing verifiable models of particle physics and General Relativity.

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HIGGS INFLATION IN f(Φ, R) THEORY

Cited by 13 publications

References 82 publications

Power law Starobinsky model of inflation from no-scale SUGRA

Power law Starobinsky model of inflation from no-scale SUGRA

Constraints on the combined models with R 2 − q $R^{2-q}$ inflation and viable f ( R ) $f(R)$ dark energy

Testing theories of gravity and supergravity with inflation and observations of the cosmic microwave background

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