Abstract
The Standard Model of particle physics fails to explain the important pieces in the standard cosmology, such as inflation, baryogenesis, and dark matter of the Universe. We consider the possibility that the sector to generate small neutrino masses is responsible for all of them; the inflation is driven by the Higgs field to break $B-L$ gauge symmetry which provides the Majorana masses to the right-handed neutrinos, and the reheating process by the decay of the $B-L$ Higgs boson supplies the second lightest right-handed neutrinos whose CP violating decays produce $B-L$ asymmetry, a la, leptogenesis. The lightest right-handed neutrinos are also produced by the reheating process, and remain today as the dark matter of the Universe. In the minimal model of the inflaton potential, one can set the parameter of the potential by the data from CMB observations including the BICEP2 and the Planck experiments. In such a scenario, the mass of the dark matter particle is predicted to be of the order of PeV. We find that the decay of the PeV right-handed neutrinos can explain the high-energy neutrino flux observed at the IceCube experiments if the lifetime is of the order of $10^{28}$ s.
Highlights
Same coupling allows the decay of the inflaton oscillation into the right-handed neutrinos to reheat the Universe
We consider the possibility that the sector to generate small neutrino masses is responsible for all of them; the inflation is driven by the Higgs field to break B − L gauge symmetry which provides the Majorana masses to the right-handed neutrinos, and the reheating process by the decay of the B − L Higgs boson supplies the second lightest right-handed neutrinos whose CP violating decays produce B − L asymmetry, `a la, leptogenesis
We find that this minimalistic scenario is consistent with various observations such as tensor-to-scalar ratio, spectral index of the CMB fluctuations, the neutrino masses, baryon asymmetry of the Universe, and the energy density of the dark matter
Summary
The dominant decay mode can either be into two right-handed neutrinos via the interaction term in eq (2.1) or two Higgs fields (including the Goldstone modes) via the term in eq (2.3). In the case where the φ → NiNi mode is dominated and for λ1 ≪ λ2 and M3 > mφ which are justified later, the decay width is given by, Γφ. By equating Γφ with the Hubble parameter H(TR) at the reheating temperature, TR, we obtain, TR ≃ 2 × 107 GeV. If the Higgs mode φ → hh, W W, ZZ is the dominant decay channel through eq (2.3), the reheating temperature can be arbitrarily higher than the above estimate. If TR is higher than mφ, the perturbative analysis of the reheating process becomes unreliable [70, 71]. We restrict ourselves to the region of TR < mφ ∼ 1013 GeV
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