Similar couplings are used to generate mass terms for the charged leptons, the neutrino has no right handed partner, it remains massless within SM. In order to obtain neutrino masses, one would have to introduce right handed neutrinos with a Yukawa coupling, i.e. L ∼ h ( LH ) ν$_{R}$ . From the VEV of the Higgs the neutrinos will obtain masses ∝ hv . In order to get neutrino masses in the interesting range m$_{ν}$ ∼ 10 − 1 eV, for solar and atmospheric neutrino mixing, the Yukawa coupling has to be very tiny, i.e. h ∼ 10 − $^{12}$. The origin of neutrino masses can also arise from higher dimensional lepton number violating operator [347–350]: When the Higgs gets a VEV, these gives rise to Majorana masses for the neutrinos of order In order to get neutrino masses in the interesting range we require M ∼ 10 14 GeV, remark- ably close to the GUT scale. An effective field theory is a powerful tool to study the loop corrections of the scalars coupled to gravity [288, 290, 351–357]. The most general action for N dimensionless scalar fields, θ $^{i}$, and the metric g$_{µν}$ can be written in terms of derivative expansion, with terms involving up to two derivatives, see [288, 290, 353, 354]: where M ≪ M$_{P}$ is regarded as the lightest mass scale of particles which would be integrated out, the coefficient functions, V ( θ ), G$_{ij}$ ( θ ) , A ( θ ) , B ( θ ) , C ( θ ) , E ( θ ) , F ( θ ) are dimensionless, and R 3 collectively represents all possible independent invariants constructed from three Riemann tensors, or two Riemann tensors and two of its covariant derivatives; R ( ∂θ ) 2 de- notes all possible invariants involving one power of the Riemann tensor and two derivatives acting on θ $^{i}$. B. Radiative corrections in an effective field theory L ∼ 1 M ( LH )( LH ) . (92) m$_{ν}$ ∼ v 2 M . (93) − L eff √ − g = v $^{4}$V ( θ ) + M 2 P 2 g µν [ W ( θ ) R$_{µν}$ + G$_{ij}$ ( θ ) ∂$_{µ}$θ $^{i}$∂$_{ν}$ θ j ] (94) + A ( θ )( ∂θ ) 4 + B ( θ ) R 2 + C ( θ ) R ( ∂θ ) 2 + E ( θ ) M 2 ( ∂θ ) 6 + F ( θ ) M 2 R 3 + · · · , 43