Reheating processes after Starobinsky inflation in old-minimal supergravity

Terada, Takahiro; Watanabe, Yuki; Yamada, Yusuke; Yokoyama, Jun′ichi

doi:10.1007/jhep02(2015)105

Cited by 48 publications

(48 citation statements)

References 135 publications

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“…This transition could be facilitated in our setting [29,62,63] via the process of perturbative reheating, according to which the inflation after inflation experiences an oscillatory phase about the vacuum, given by (22) for the non-SUSY case or (41) for the SUGRA case. During this phase, the inflation can safely decay, provided that it couples to light degrees of freedom in the Lagrangian of the full theory.…”

Section: Discussionmentioning

confidence: 99%

“…In some cases [20,29,31,58], the employed 's parameterize specific Kähler manifolds, which appear in no-scale models [59][60][61]. Moreover, this scheme ensures naturally a low enough reheating temperature, potentially consistent with the gravitino constraint [29,62,63] if connected with a version of the Minimal SUSY Standard Model (MSSM).…”

Section: Introductionmentioning

confidence: 99%

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Starobinsky Inflation: From Non-SUSY to SUGRA Realizations

Pallis

Toumbas

2017

Advances in High Energy Physics

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We review the realization of Starobinsky-type inflation within induced-gravity supersymmetric (SUSY) and non-SUSY models. In both cases, inflation is in agreement with the current data and can be attained for sub-Planckian values of the inflation. The corresponding effective theories retain perturbative unitarity up to the Planck scale and the inflation mass is predicted to be 3 ⋅ 1013 GeV. The supergravity embedding of these models is achieved by employing two gauge singlet chiral superfields, a superpotential that is uniquely determined by a continuous and a discrete Z symmetry and several (semi)logarithmic Kähler potentials that respect these symmetries. Checking various functional forms for the noninflation accompanying field in the Kähler potentials, we identify four cases which stabilize it without invoking higher order terms.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Starobinsky Inflation: From Non-SUSY to SUGRA Realizations

Pallis

Toumbas

2017

Advances in High Energy Physics

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“…[62] for a similar situation). The two-body decay rate into scalar particles is of the order |J ij | 2 m 3 χ /M 2 G .…”

Section: Jhep12(2014)062mentioning

confidence: 84%

Generic scalar potentials for inflation in supergravity with a single chiral superfield

Ketov

Terada

2014

J. High Energ. Phys.

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We propose a large class of supergravity models in terms of a single chiral matter superfield, leading to (almost) arbitrary single-field inflationary scalar potentials similar to the F -term in rigid supersymmetry. Those scalar potentials are positively semidefinite (in our approximation), and can preserve supersymmetry at the end of inflation. The only scalar superpartner of inflaton is stabilized by a higher-dimensional term in the Kähler potential. We argue that couplings of the inflaton to other sectors of the particle spectrum do not affect the inflationary dynamics, and briefly discuss reheating of the universe by the inflaton decays.

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“…For a review on inflationary cosmology after the release of the Planck collaboration's results, and for an approach on the initial conditions problem see also [24]. Note that the embedding of the Starobinsky model has been also studied in the old-minimal supergravity [13,[25][26][27][28][29][30], in no-scale supergravity [31][32][33][34], in the linearized non-minimal (20/20) supergravity [35], and also in a generic supergravity setup via gravitino condensates [36,37].…”

Section: Introduction and Discussionmentioning

confidence: 99%

Starobinsky inflation from new-minimal supergravity

Farakos

2015

J. Phys.: Conf. Ser.

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Starobinsky inflation from new-minimal supergravity Fotis FarakosInstitute for Theoretical Physics, Masaryk University, 611 37 Brno, Czech Republic E-mail: fotisf@mail.muni.cz Abstract.In the new-minimal supergravity formulation we present the embedding of the R + R 2 Starobinsky model of inflation. Starting from the superspace action we perform the projection to component fields and identify the Starobinsky model in the bosonic sector. Since there exist no other scalar fields, this is by construction a single field model. This higher curvature supergravity also gives rise to a propagating massive vector. Finally we comment on the issues of higher order corrections and initial conditions. Introduction and discussionThe Planck collaboration's constraints on inflation [1, 2] have restricted the inflationary models to those which are characterized by a plateau potential for the inflaton field. More specifically, if the perturbations during inflation [3] are originated by the same field driving inflation, these restrictions can be quantified by the following constraints on the spectral index: n s = 0.9655 ± 0.0062 and the tensor-to-scalar ratio: r < 0.12. A model which lies in the heart of the data is the pure gravitational Starobinsky model [4]

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Reheating processes after Starobinsky inflation in old-minimal supergravity

Cited by 48 publications

References 135 publications

Starobinsky Inflation: From Non-SUSY to SUGRA Realizations

Starobinsky Inflation: From Non-SUSY to SUGRA Realizations

Generic scalar potentials for inflation in supergravity with a single chiral superfield

Starobinsky inflation from new-minimal supergravity

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