Asymmetric Self-interacting Dark Matter via Dirac Leptogenesis

Abstract

The nature of neutrinos, whether Dirac or Majorana, is hitherto not known. Assuming that the neutrinos are Dirac, which needs $B-L$ to be an exact symmetry, we make an attempt to explain the observed proportionality between the relic densities of dark matter (DM) and baryonic matter in the present Universe $i.e.,{\Omega }_{\mathrm{DM}}\approx 5{\Omega }_{\mathrm{B}}$. Assuming the existence of heavy $SU(2{)}_L$ scalar doublet $(X=(X^0,X^{-}{)}^T)$ in the early Universe, an equal and opposite $B-L$ asymmetry can be generated in left and right-handed sectors by the CP-violating out-of-equilibrium decay $X^0\to {\nu }_L{\nu }_R$ since $B-L$ is an exact symmetry. We ensure that ${\nu }_L-{\nu }_R$ equilibration does not occur until below the electroweak (EW) phase transition during which a part of the lepton asymmetry gets converted to dark matter asymmetry through a dimension eight operator, which conserves $B-L$ symmetry and is in thermal equilibrium. The remaining $B-L$ asymmetry then gets converted to a net B-asymmetry through EW-sphalerons which are active at a temperature above 100 GeV. To alleviate the small-scale anomalies of $\Lambda$CDM, we assume the DM to be self-interacting via a light mediator, which not only depletes the symmetric component of the DM, but also paves a way to detect the DM at terrestrial laboratories through scalar portal mixing.

17 pages, 10 captioned figures, Version accepted for publication in PRD

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Cited by in corpus (6)

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• Asymmetric dark matter with a spontaneously broken $U(1{)}^{\prime }$: self-interaction and gravitational waves
• Investigating Boson Sector in an Extended Standard Model with $U(1{)}_D$ Symmetry
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• Cogenesis of visible and dark matter in type-I Dirac seesaw