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Starobinsky-Type Inflation With Products of Kaehler Manifolds

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arxiv 1512.05657 v3 pith:7IQTF7EE submitted 2015-12-17 hep-ph astro-ph.COhep-th

C. Pallis , N. Toumbas This is my paper · ORCID
classification hep-phastro-ph.COhep-th
keywords kaehlerinflationinflatonobservablespotentialstarobinsky-typesuperpotentialchiral
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We present a novel realization of Starobinsky-type inflation within Supergravity using two chiral superfields. The proposed superpotential is inspired by induced-gravity models. The Kaehler potential contains two logarithmic terms, one for the inflaton T and one for the matter-like field S, parameterizing the SU(1,1)/U(1)x SU(2)/U(1) Kaehler manifold. The two factors have constant curvatures -m/n and 2/n2, where n, m are the exponents of T in the superpotential and Kaehler potential respectively, and 0<n2<=6. The inflationary observables depend on the ratio 2n/m only. Essentially they coincide with the observables of the original Starobinsky model. Moreover, the inflaton mass is predicted to be 3x10^13 GeV.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Kinetically Modified Palatini Inflation Meets ACT Data

    hep-ph 2025-05 conditional novelty 6.0 of 10

    Palatini chaotic inflation with kinetic mixing f_K = f_R^m can shift the predicted spectral index up to the ACT DR6 value n_s = 0.974 while keeping r below current bounds.

  2. Induced-Gravity Palatini-Like Higgs Inflation in Supergravity Confronts ACT DR6

    hep-ph 2026-02 unverdicted novelty 5.0 of 10

    A Palatini-supergravity Higgs-inflation model with induced gravity predicts a scalar spectral index ns≈0.972-0.974, consistent with ACT DR6, and favors split supersymmetry with gravitino mass 40-60 PeV.

  3. Starobinsky Inflation with T-Model Kaehler Geometries

    hep-ph 2025-02 conditional novelty 5.0 of 10

    Starobinsky-like inflation is embedded in supergravity via T-model Kähler potentials, yielding ns in the range 0.961 to 0.969 and a tensor-to-scalar ratio that rises with Kähler curvature.

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