Abstract
We study a version of Starobinsky-like inflation in no-scale supergravity (SUGRA) where a Polonyi term in the hidden sector breaks supersymmetry (SUSY) after inflation, providing a link between the gravitino mass and inflation. We extend the theory to the visible sector and calculate the soft-SUSY breaking parameters depending on the modular weights in the superpotential and choice of Kähler potential. We are led to either no-scale SUGRA or pure gravity mediated SUSY breaking patterns, but with inflationary constraints on the Polonyi term setting a strict upper bound on the gravitino mass m3/2< 103 TeV. Since gaugino masses are significantly lighter than m3/2, this suggests that SUSY may be discovered at the LHC or FCC.
Highlights
We are led to either no-scale SUGRA or pure gravity mediated SUSY breaking patterns, but with inflationary constraints on the Polonyi term setting a strict upper bound on the gravitino mass m3/2 < 103 TeV
We calculate the soft-SUSY breaking parameters depending on the modular weights in the superpotential and choice of Kahler potential and we are led to new phenomenological possibilities for supersymmetry (SUSY) breaking, based on generalisations of no-scale SUSY breaking and pure gravity mediated SUSY breaking
The linear Polonyi term provides a simple way to break SUSY after inflation, with the requirement of successful inflation leading to an upper bound on the gravitino mass m3/2 < 103 TeV, with gaugino masses considerably less than this
Summary
The tree-level supergravity scalar potential can be found using the Kahler function G, which is given in terms of the Kahler potential K and the superpotential W as, K. When the modulus field T is fixed with a vacuum expectation value of Re T = 1/2 and Im T = 0, the no-scale Kahler potential together with the Wess-Zumino superpotential is equivalent of an R + R2 model of gravity, in which Starobinsky inflation emerges at a particular point in parameter space [59]. The scalar amplitude observable, As, is sensitive to the overall scale of the potential, i.e to the p√arameter μ in eq (2.13) It is shown there [61] that, in the Starobinsky limit when λ = μ/ 3MP , the bilinear mass term parameter becomes μ 10−5MP and we use these values in the following computations
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