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 $f_{\rm NL} = 5/3$. Implication to the mass spectrum of supersymmetric particles is discussed.
Highlights
The Universe starts from small fluctuations, which have grown and collapsed to form galaxies
The observations of the large scale structure and the cosmic microwave wave background (CMB) have revealed that the fluctuations are nearly Gaussian and scale invariant [1,2], which are naturally explained by quantum fluctuations of a nearly massless scalar field generated during inflation [3,4,5,6,7]
We investigate the possibility that scalar fields in the minimal supersymmetric standard model (MSSM) are responsible for the fluctuations
Summary
The Universe starts from small fluctuations, which have grown and collapsed to form galaxies. The radial direction has a mass as large as the Hubble scale, and its quantum fluctuations are suppressed. When the Hubble scale drops below the soft mass of φ at the vacuum, mφ, the flat direction begins oscillation around the origin. At this point, the irreducible explicit Uð1Þ symmetry breaking from the gravitino mass m3=2, ΔV ∼ m3=2λφn þ H:c:; ð2Þ which gives a nonzero potential energy of θ, is no more negligible. The fluctuation of θ, together with its potential, gives rise to the fluctuation of the energy density and may source the cosmic perturbations [27,28] This seems challenging for a MSSM flat direction, which has Oð1Þ gauge couplings. We describe the detail of the scenario as wellasits cosmological, astrophysical andcollider signatures
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