Cosmic perturbations, baryon asymmetry and dark matter from the minimal supersymmetric standard model

Abstract

Scalar fields in the minimal supersymmetric standard model may have large field values during inflation. Because of approximate global symmetry, it is plausible that the phase directions of them are nearly massless during inflation and obtain quantum fluctuations, which may be the origin of the cosmic perturbations. If perturbations are produced through Q-ball formation, baryon asymmetry and dark matter can be consistently generated. Significant baryon and dark matter isocurvature perturbations are produced, but they are predicted to nearly compensate each other. The lepton asymmetry is much larger than the baryon asymmetry. The scenario predicts local non-Gaussianity of fNL = 5/3. Implication to the mass spectrum of supersymmetric particles is discussed.

Increasing temperature toward the completion of reheating

“…A simple class of chaotic inflation [46] is excluded by the upper bound on the tensor fraction [45], but there exist models where the inflaton potential becomes flat at large field values so that the tensor fraction is suppressed [47][48][49][50][51][52][53][54][55][56][57][58][59][60]. Alternatively, the curvature perturbations of the universe may be sourced by spectator field models such as a curvaton [61][62][63][64][65][66][67][68] or modulated reheating [69][70][71][72]. If φ is a generic scalar field, the large initial field value may be a result of a flat potential of φ or a negative mass term given by the coupling with the inflaton [73].…”

Increasing Temperature toward the Completion of Reheating

“…A simple class of chaotic inflation [44] is excluded by the upper bound on the tensor fraction [43], but there exist models where the inflaton potential becomes flat at large field values so that the tensor fraction is suppressed [45][46][47][48][49][50][51][52][53][54][55][56][57][58]. Alternatively, the curvature perturbations of the universe may be sourced by spectator field models such as a curvaton [59][60][61][62][63][64][65][66] or modulated reheating [67][68][69][70]. If φ is a generic scalar field, the large initial field value may be a result of a flat potential of φ or a negative mass term given by the coupling with the inflaton [71].…”