Common origin of nonzero ${\theta }_{13}$ and dark matter in an $S_4$ flavor symmetric model with inverse seesaw mechanism

We study an inverse seesaw model of neutrino mass within the framework of $S_4$ flavor symmetry from the requirement of generating nonzero reactor mixing angle ${\theta }_{13}$ along with correct dark matter relic abundance. The leading order $S_4$ model gives rise to tribimaximal-type leptonic mixing, resulting in ${\theta }_{13}=0$. Nonzero ${\theta }_{13}$ is generated at one-loop level by extending the model with additional scalar and fermion fields which take part in the loop correction. The particles going inside the loop are odd under an in-built $Z_2^{\text{Dark}}$ symmetry such that the lightest $Z_2^{\text{Dark}}$ odd particle can be a dark matter candidate. Correct neutrino and dark matter phenomenology can be achieved for such one-loop corrections either to the light neutrino mass matrix or to the charged lepton mass matrix, although the latter case is found to be more predictive. The predictions for neutrinoless double beta decay are also discussed, and inverted hierarchy in the charged lepton correction case is found to be disfavored by the latest KamLAND-Zen data.

Figure 1

Radiative generation of nonzero ${\theta }_{13}$ from the light neutrino sector.

Figure 2

Radiative generation of nonzero ${\theta }_{13}$ from the light neutrino sector.

Figure 3

Radiative generation of nonzero ${\theta }_{13}$ from charged lepton sector.

Figure 4

Feynman diagram contributing to neutrinoless double beta decay due to light Majorana neutrino exchanges [32].

Figure 5

Model parameter as a function of the lightest neutrino mass and Majorana phase $\alpha$.

Figure 6

Model parameters as a function of the lightest neutrino mass and the atmospheric mixing angle ${\theta }_{23}$.

Figure 7

Corrections parameter (correction to neutrino mass matrix) as a function of the lightest neutrino mass and Majorana phase $\alpha$.

Figure 8

Corrections parameter (correction to the neutrino mass matrix) as a function of the lightest neutrino mass and Majorana phase $\zeta$.

Figure 9

Corrections parameter (correction to the neutrino mass matrix) as a function of the lightest neutrino mass and Majorana phase $\alpha$.

Figure 10

Correction parameters as a function of Majorana and Dirac phases while giving correction to the charged lepton mass matrix.

Figure 11

Correction parameters as a function of Majorana and Dirac phases while giving correction to the charged lepton mass matrix.

Figure 12

Variation of effective neutrino mass with the lightest neutrino mass in the model with neutrino mass correction. The purple line indicates the PLANCK bound on the sum of absolute neutrino masses. The green band shows the KamLAND-ZEN upper bound [54] on the effective neutrino mass.

Figure 13

Variation of effective neutrino mass with the lightest neutrino mass in the model with charged lepton correction. The purple line indicates the Planck bound on the sum of absolute neutrino masses. The green band shows the KamLAND-ZEN upper bound [54] on the effective neutrino mass.

Figure 14

Variation of effective neutrino mass with the lightest neutrino mass in the model with charged lepton correction.

Figure 15

Dark matter mass as a function of Yukawa coupling keeping the mediator mass fixed for each plots, such that the constraints on the DM relic abundance are satisfied.