Abstract
We study reheating after the end of inflation in models where the inflaton is the superpartner of goldstino and is charged under a gauged U(1) R-symmetry. We consider two classes of models – one is small field characterized by an almost flat Kähler space, and the other large field characterized by a hyperbolic Kähler space SU(1, 1)/U(1), while in both cases the inflaton superpotential is linear due to the R-symmetry. The inflationary observables of our models fit within 2sigma CMB values. Upon coupling the inflaton sector to the (supersymmetric) Standard Model, we compute the MSSM parameters, mass spectrum, and decay modes of the inflaton, with the resulting reheating temperature around 10^8 GeV. We also find that both models can accommodate superheavy LSP dark matter, depending on the parameter choice.
Highlights
C (2021) 81:1078 is proportional to the goldstino superfield Z and is added to the goldstino decay constant; (2) to have the same R-charge as Z so that Standard Model particles are neutral while their superpartners are charged, in which case is just added to the supersymmetry breaking sector superpotential
In our model II, MSSM scalars and inflatino are heavier than the inflaton, which means that the inflaton can only decay into the gaugini λ1,2,3
In our case the local U (1)R symmetry allows for interaction terms between matter fields φ and the inflaton Z, as in the Kähler potential
Summary
The starting point is a class of models with gauged U (1)R phase symmetry, defined by Kähler potential and superpotential In this class of models, the Z -dependent part of the potential drives inflation, after which Z and its auxiliary field F Z settle at non-zero vacuum expectation values (VEVs), spontaneously breaking both supersymmetry (SUSY) and U (1)R. Since we require that matter fields vanish at the minimum, vacuum structure is defined entirely by the choice of the Kähler potential J (Z , Z ) (as the superpotential is already fixed). Consider the limit of vanishing U (1)R coupling g, in which case the parameter of the superpotential a becomes an overall factor of the scalar potential.
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