Abstract
We consider a possibility that one of the flat directions in the minimal supersymmetric standard model plays the role of the inflaton field and realizes large-field inflation. This is achieved by introducing a generalized shift symmetry on the flat direction, which enables us to control the inflaton potential over large field values. After inflation, higher order terms allowed by the generalized shift symmetry automatically cause a helical motion of the field to create the baryon number of the universe, while baryonic isocurvature fluctuations are suppressed.
Highlights
Inflation solves various theoretical difficulties of the standard big bang cosmology [1].1 The most plausible way to realize inflation with a graceful exit is to introduce a gauge singlet inflaton field with a relatively flat potential [6, 7]
In this Letter we revisit a possibility that one of the minimal supersymmetric standard model (MSSM) flat directions plays the role of the inflaton field
We have studied a possibility that one of the MSSM flat directions plays the role of the inflaton and realizes the large-field inflation, indicated by the recent detection of the primordial B-mode polarization by BICEP2
Summary
Inflation solves various theoretical difficulties of the standard big bang cosmology [1].1 The most plausible way to realize inflation with a graceful exit is to introduce a gauge singlet inflaton field with a relatively flat potential [6, 7]. With the running kinetic term, the standard model (SM) Higgs field (as well as its supersymmetric extension) can play the role of the inflaton with a simple quadratic (or fractional power) potential [20]. One of the flat directions in the minimal supersymmetric standard model (MSSM) could play the role of the inflaton field and various implications for phenomenology and cosmology were discussed in Ref. In this Letter we revisit a possibility that one of the MSSM flat directions plays the role of the inflaton field. To this end we identify φn with the flat direction and impose the generalized shift symmetry (2). In Appendix, we show a list of possible flat directions together with the predicted values of the scalar spectral index and the tensor-to-scalar ratio
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