content_image/356996.jpg content_image/357006.jpg content_image/357005.jpg content_image/357004.jpg
<img src='content_image/356996.jpg'>

δ$_{CP}$ behave depending on the parameter φ , which will be shown in Fig. 3 and Fig. 5. And, solar neutrino mixing is governed by 

which for x = 0 agrees with the result of tri-bimaximal, i.e. tan 2 θ$_{12}$ $_{= 2}$√$_{2. Note here that}$ in Eq. (26) the condition 

<img src='content_image/357006.jpg'>

<img src='content_image/357005.jpg'>

should be satisfied, in order for θ$_{12}$ to be lie in the experimental bounds in Table-I. Interesting points are that the deviation of θ$_{12}$ from tri-bimaximal is closely related with θ$_{13}$ through the parameters x and φ , and the deviation of θ$_{23}$ from maximality is governed by the phase φ which is related with δ$_{CP}$ in Eq. (25), if the parameter κ is determined by heavy neutrino mass ordering. 

Because of the observed hierarchy | Δ m 2 32 | ≫ Δ m 2 $_{21}$, and the requirement of MSW reso- nance for solar neutrinos, there are two possible neutrino mass spectrum: (i) m$_{1}$ < m$_{2}$ < m$_{3}$ (normal mass spectrum) which corresponds to ω 1 a < ω$_{2}$ < ω 3 b and (ii) m$_{3}$ < m$_{1}$ < m$_{2}$ (in- verted mass spectrum) which corresponds to ω 3 b < ω 1 a < ω$_{2}$ . Here we can approximate light neutrino masses in our model as m$_{i}$ ≈ m$_{0}$ ( ω 1 a , ω$_{2}$, ω 3 b ), by using Eqs. (18), (19) we can express neutrino masses as, 

<img src='content_image/357004.jpg'>

where Δ m 2 η = m$_{+}$$^{m}$− and m$_{+}$ ≃ 2 ¯ m$_{η}$ are used, and $^{m}$± denotes | m$_{R}$ ± m$_{I}$ | . And α is a dummy index, α = a, 1 , b refer to light neutrinos m$_{1}$, m$_{2}$, m$_{3}$ and also heavy neutrinos 

