No-scale supergravity provides a successful framework for Starobinsky-like inflation models. Two classes of models can be distinguished depending on the identification of the inflaton with the volume modulus, T (C models), or a matterlike field, φ (WZ models). When supersymmetry is broken, the inflationary potential may be perturbed, placing restrictions on the form and scale of the supersymmetry breaking sector. We consider both types of inflationary models in the context of high-scale supersymmetry. We further distinguish between models in which the gravitino mass is below and above the inflationary scale. We examine the mass spectra of the inflationary sector. We also consider, in detail, mechanisms for leptogenesis for each model when a right-handed neutrino sector, used in the seesaw mechanism to generate neutrino masses, is employed. In the case of C models, reheating occurs via an inflaton decay to two Higgs bosons. However, there is a direct decay channel to the lightest right-handed neutrino which leads to nonthermal leptogenesis. In the case of WZ models, in order to achieve reheating, we associate the matterlike inflaton with one of the right-handed sneutrinos whose decay to the lightest right-handed neutrino simultaneously reheats the Universe and generates the baryon asymmetry through leptogenesis.
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This work was supported by the France-US PICS MicroDark and by Institut Pascal at Universit Paris-Saclay with the support of the P2I and SPU research departments and the P2IO Laboratory of Excellence (program Investissements d’avenir ANR-11-IDEX-0003-01 Paris-Saclay and ANR-10-LABX-0038), as well as the IPhT. Y. M. acknowledges partial support from the European Union Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie: RISE InvisiblesPlus (Grant Agreement No. 690575), the ITN Elusives (Grant Agreement No. 674896) and the Red Consolider MultiDark . The work of K. K., K. A. O., and S. V. was supported in part by the DOE Grant No. DE–SC0011842 at the University of Minnesota. K. A. O. acknowledges support by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under the Contract No. DE-AC02-05CH11231. K. A. O. would also like to thank the Department of Physics and the high energy theory group at the University of California, Berkeley as well as the theory group at LBNL for their hospitality and financial support while finishing this work.
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