Higher Order Corrections in Minimal Supergravity Models of Inflation

Ferrara, Sergio; Kallosh, Renata; Linde, Andrei; Porrati, Massimo

doi:10.48550/arxiv.1309.1085

Cited by 29 publications

(54 citation statements)

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“…The smallness of the dimensionless coupling constant λ n does not certainly imply that a fine-tuning is necessary. For example, in [9], R 4 term was proposed to be suppressed by the Planck scale and then the upper bound on the effective dimensionless coupling becomes ξ ∼ λ 4 (M p /M ) 6 < ∼ 10 26 which is much larger than one.…”

Section: Discussionmentioning

confidence: 99%

“…+other higher derivative terms), (6) where c i are the dimensionless couplings. The higher derivative terms may also originate from the supergravity [8,9]. Here one point we want to mention is that in [9] the correction term of R 4 was proposed to be suppressed by the Planck scale M p = 1/κ, not M s , in the new minimal supergravity model.…”

Section: Introductionmentioning

confidence: 99%

“…The higher derivative terms may also originate from the supergravity [8,9]. Here one point we want to mention is that in [9] the correction term of R 4 was proposed to be suppressed by the Planck scale M p = 1/κ, not M s , in the new minimal supergravity model. More relevant fundamental aspects on the gravity with higher derivatives are considered in [10][11][12] etc.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A polynomial f(R) inflation model

Huang

2014

J. Cosmol. Astropart. Phys.

129

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Motivated by the ultraviolet complete theory of quantum gravity, for example the string theory, we investigate a polynomial f (R) inflation model in detail. We calculate the spectral index and tensorto-scalar ratio in the f (R) inflation model with the form of f (R) = R+ R 2 6M 2 + λn 2n R n (3M 2 ) n−1 . Compared to Planck 2013, we find that R n term should be exponentially suppressed, i.e. |λn| < ∼ 10 −2n+2.6 .PACS numbers:

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A polynomial f(R) inflation model

Huang

2014

J. Cosmol. Astropart. Phys.

129

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“…Originally, the model was motivated by the one-loop corrections to the Einstein-Hilbert action resulting from vacuum quantum fluctuations in the matter sector at sufficiently high energies [6,8,9], which can be taken into account effectively by adding an R 2 -term to the gravitational action. Recently, possibly motivated by its excellent fit to the CMB data (see for example [10]) there has been increased interest in the model in the context of supergravity [11][12][13][14][15][16][17][18][19][20][21][22][23] (see Ref. [24] for a more complete discussion on the subject), as well as in other quantum gravity contexts [25][26][27][28][29][30].…”

Section: Introductionmentioning

confidence: 99%

Asymptotically safe Starobinsky inflation

2015

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We revisit Starobinsky inflation in a quantum gravitational context, by means of the exact Renormalisation Group (RG). We calculate the non-perturbative beta functions for Newton's 'constant' G and the dimensionless R 2 coupling, and show that there exists an attractive UV fixed point where the latter one vanishes but not the former one, and we provide the corresponding beta functions. The smallness of the R 2 coupling, required for agreement with inflationary observables, is naturally ensured by its vanishing at the UV fixed point, ensuring the smallness of the primordial fluctuations, as well as providing a theoretical motivation for the initial conditions needed for successful inflation in this context. We discuss the corresponding RG dynamics, showing both how inflationary and classical observations define the renormalisation conditions for the couplings, and also how the UV regime is connected with lower energies along the RG flow. Finally, we discuss the consistency of our results when higher order curvature corrections are included, and show that they are robust to the inclusion of R 3 corrections.

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“…Under an appropriate Weyl transformation of the metric, that absorbs the auxiliary field dependent coefficient of the scalar curvature, the gravity sector becomes of the Einstein-Hilbert form and the auxiliary fields become dynamical. This duality between a given f (R) gravity and its Einstein form is not so easily implemented in the framework of a supergravity theory [3][4][5][6]. Nevertheless, there is strong motivation for studying f (R) supergravities based mainly on the fact that R + R 2 supergravities provide a fruitful framework to describe cosmological inflation [7,8].…”

Section: Introductionmentioning

confidence: 99%

Towards a formulation off(R)supergravity

2015

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The supersymmetric completion of R + R 2 gravity is known to be equivalent to standard supergravity coupled to two chiral supermultiples with a Kähler potential of the no-scale type. The generalization of this program to f (R) gravity can be carried out in an analogous framework in terms of four chiral multiplets with appropriately chosen superpotential and Kähler potential. Although the construction strategy has been known for sometime, we carry out this program further by setting these theories in a closed form. The general framework considered can accommodate supergravity actions local in the scalar curvature, dual to ordinary N = 1 supergravities. Although these are in general plagued by ghosts, the framework studied in this work offers a possibility that these can decouple as can be seen in specific examples.

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Higher Order Corrections in Minimal Supergravity Models of Inflation

Cited by 29 publications

References 0 publications

A polynomial f(R) inflation model

A polynomial f(R) inflation model

Asymptotically safe Starobinsky inflation

Towards a formulation off(R)supergravity

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