Abstract
Weakly interacting massive particle (WIMP) as a dark matter (DM) candidate is further inspired by recent AMS-02 data, which confirm the excess of positron fraction observed earlier by PAMELA and Fermi-LAT experiments. Additionally, the excess of positron+electron flux is still significant in the measurement of Fermi-LAT. For solving the problems of massive neutrinos and observed excess of cosmic-ray, we study the model with an inert Higgs doublet (IHD) in the framework of type-II seesaw model by imposing a Z 2 symmetry on the IHD, where the lightest particle of IHD is the DM candidate and the neutrino masses originate from the Yukawa couplings of Higgs triplet and leptons. We calculate the cosmic-ray production in our model by using three kinds of neutrino mass spectra, which are classified by normal ordering, inverted ordering and quasi-degeneracy. We find that when the constraints of DM relic density and comic-ray antiproton spectrum are taken into account, the observed excess of positron/electron flux could be explained well in normal ordered neutrino mass spectrum. Moreover, excess of comic-ray neutrinos is implied in our model. We find that our results on 〈σv〉 are satisfied with and close to the upper limit of IceCube analysis. More data from comic-ray neutrinos could test our model.
Highlights
The origin of neutrino masses is one of most mysterious problems in high energy physics
For solving the problems of massive neutrinos and observed excess of cosmic-ray, we study the model with an inert Higgs doublet (IHD) in the framework of type-II seesaw model by imposing a Z2 symmetry on the IHD, where the lightest particle of IHD is the dark matter (DM) candidate and the neutrino masses originate from the Yukawa couplings of Higgs triplet and leptons
The measurement of the positron fraction in higher energy region is important to test the model and tell us the mass of DM. 4.4 Cosmic-ray neutrinos As known that the necessary boost factor (BF) in scenario-Ic and -II for explaining the positron excess has been excluded by the data of antiproton spectrum, in the following we focus on scenario-I as follows: (Ia),b and -III for cosmic-ray neutrinos induced by DM annihilation of galactic halo
Summary
We introduce the new interactions in the model. The SM particles and the triplet ∆ are Z2-parity even while the new doublet Φ is Z2-parity odd. With the new Z2-parity, the involved new gauge interactions, new Yukawa couplings and scalar potential are written as LNP = (DμΦ)†DμΦ+(Dμ∆)†Dμ∆−. Where v0(∆) are the VEV of neutral component of H(∆) and their values are related to the parameters of scalar potential. There are two ways to present ∆: for gauge interactions we use 3 × 1 column vector but for Yukawa couplings and scalar potential, we use 2 × 2 matrix. Since the mixing of H and ∆ is related to the small v∆, which is constrained by ρ parameter and the masses of neutrinos, the Goldstone bosons and Higgs boson are mainly from the SM Higgs doublet.
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