Inflation in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si1.gif" overflow="scroll"><mml:msup><mml:mrow><mml:mi>R</mml:mi></mml:mrow><mml:mrow><mml:mn>2</mml:mn></mml:mrow></mml:msup></mml:math>supergravity with non-minimal superpotentials

Diamandis, G.A.; Georgalas, B.C.; Kaskavelis, K.; Kouroumalou, P.; Lahanas, A.B.; Pavlopoulos, Georgios A.

doi:10.1016/j.physletb.2015.03.034

Cited by 12 publications

(5 citation statements)

References 81 publications

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“…This is exactly the entropy we would have found using the standard expression 19) for the entropy in the Einstein frame and then using the conformal transformation, 20) to find the entropy in the R 2 theory. That the entropy is invariant under conformal transformations has been proven, at least for that class of transformations that approach identity at infinity in [36,37].…”

Section: Jhep05(2015)143supporting

confidence: 57%

“…Furthermore as was noticed by Starobinsky and others [3,4] the potential of φ is of great cosmological interest, since it can describe a slow transition from a de Sitter phase to a flat Minkowski phase leading to a viable realization of the inflationary scenario in the early Universe [5][6][7]. More recently the R + R 2 inflationary scenario was also investigated in the context of supergravity [8][9][10][11][12][13][14][15][16][17][18][19][20][21][22].…”

Section: Introductionmentioning

confidence: 99%

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Black hole solutions in R 2 gravity

Kehagias

Kounnas

Lüst

et al. 2015

J. High Energ. Phys.

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We find static spherically symmetric solutions of scale invariant R 2 gravity. The latter has been shown to be equivalent to General Relativity with a positive cosmological constant and a scalar mode. Therefore, one expects that solutions of the R 2 theory will be identical to that of Einstein theory. Indeed, we find that the solutions of R 2 gravity are in one-to-one correspondence with solutions of General Relativity in the case of nonvanishing Ricci scalar. However, scalar-flat R = 0 solutions are global minima of the R 2 action and they cannot in general be mapped to solutions of the Einstein theory. As we will discuss, the R = 0 solutions arise in Einstein gravity as solutions in the tensionless, strong coupling limit M P → 0. As a further result, there is no corresponding Birkhoff theorem and the Schwarzschild black hole is by no means unique in this framework. In fact, R 2 gravity has a rich structure of vacuum static spherically symmetric solutions partially uncovered here. We also find charged static spherically symmetric backgrounds coupled to a U(1) field. Finally, we provide the entropy and energy formulas for the R 2 theory and we find that entropy and energy vanish for scalar-flat backgrounds.

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Section: Jhep05(2015)143supporting

confidence: 57%

Section: Introductionmentioning

confidence: 99%

Black hole solutions in R 2 gravity

Kehagias

Kounnas

Lüst

et al. 2015

J. High Energ. Phys.

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“…Many SUGRA models have been constructed which can yield a range of r from 10 −3 to 10 −1 by changing the parameters of the Kähler potential and the superpotential [36][37][38][39][40][41][42][43][44][45][46][47][48][49][50][51][52][53].…”

Section: Introductionmentioning

confidence: 99%

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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“…Modifications and further properties can be found in [97,98,99,101,102,103,104,100,105,106,107,108,109,110]. We mention that attention should be paid to the full couplings of the inflaton field that may yield a different reheating temeprature in each of these models since not all of them are pure supergravitational.…”

Section: The R + R 2 Supergravity Inflationmentioning

confidence: 98%

Probing the BSM physics with CMB precision cosmology: an application to supersymmetry

Dalianis

Watanabe

2018

J. High Energ. Phys.

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The cosmic history before the BBN is highly determined by the physics that operates beyond the Standard Model (BSM) of particle physics and it is poorly constrained observationally. Ongoing and future precision measurements of the CMB observables can provide us with significant information about the pre-BBN era and hence possibly test the cosmological predictions of different BSM scenarios. Supersymmetry is a particularly motivated BSM theory and it is often the case that different superymmetry breaking schemes require different cosmic histories with specific reheating temperatures or low entropy production in order to be cosmologically viable. In this paper we quantify the effects of the possible alternative cosmic histories on the n s and r CMB observables assuming a generic non-thermal stage after cosmic inflation. We analyze TeV and especially multi-TeV supersymmetry breaking schemes assuming the neutralino and gravitino dark matter scenarios. We complement our analysis considering the Starobinsky R 2 inflation model to exemplify the improved CMB predictions that a unified description of the early universe cosmic evolution yields. Our analysis underlines the importance of the CMB precision measurements that can be viewed, to some extend, as complementary to the laboratory experimental searches for supersymmetry or other BSM theories.

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Inflation inR2supergravity with non-minimal superpotentials

Cited by 12 publications

References 81 publications

Black hole solutions in R 2 gravity

Black hole solutions in R 2 gravity

Power law Starobinsky model of inflation from no-scale SUGRA

Probing the BSM physics with CMB precision cosmology: an application to supersymmetry

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