of the baryon asymmetry for the specific values of δ$_{N}$$_{i}$$_{η}$ . And, it seems difficult for resonant leptogenesis to be implemented, because of the constraints of solar mixing angle and the mass-squared differences Δ m 2 21 and Δ m 2 $_{32}$. From the mass-squared differences in Eq. (29) and Eq. (30), since for M$_{2}$ = M$_{3}$ (which means b = 1 and ω$_{2}$ = ω$_{3}$ ) could not give the value of R ≡ Δ m 2 $_{21}$/ | Δ m 2 32 | ∼ O (0 . 01), it is not possible for the resonant leptogenesis between N$_{2}$ and N$_{3}$ . In the case of degeneracy between N$_{1}$ and N$_{2}$ , introducing δ$_{12}$ ≡ 1 − M$_{1}$/M$_{2}$ , the solar mixing angle in Eq. (34) indicates δ$_{12}$ ≫ x cos φ to satisfy the low energy experi- mental data, with a large x and a relatively large θ$_{13}$ at around φ = 3 π/ 2. However, since its CP-asymmetries are proportional to ε e 1 ∼ sin 2 φ, ε µ 1 ∼ cos φ and ε µ 1 ∼ cos φ , at around φ = 3 π/ 2 the resonant leptogenesis of the degeneracy between N$_{2}$ and N$_{3}$ could not give a explanation of BAU. In order to explain the possibility of BAU, we will show the two cases corresponding to normal hierarchical and degenerate mass ordering, for example, Case-I and Case-II , respectively. In the case of M$_{3}$ ⪆ ¯ m$_{η}$ , from Eq. (13) and Eq. (39), the wash-out parameters associated with N$_{3}$ and the lepton flavors α = e, µ, τ are given as in which the common factor g 2 $^{$_{ν}$m}$∗ /bM is constrained by the overall factor of neutrino mass matrix in Eq. (19) as 8 π $^{$^{2}$m}$∗ m$_{0}$/b ¯ m$_{η}$$^{m}$− with ¯ m$_{η}$ ≃ M$_{3}$ = bM , all K -factors are evaluated at temperature T = M$_{3}$ , and M$_{3}$ is the lightest of the heavy Majorana neutrinos. Note here that wash-out factors associated with N$_{1}$$_{,}$$_{2}$ and the lepton flavors α = e, µ, τ are enormously huge compared to the factors K e,µ,τ 3 , and therefore the generated lepton asymmetries associated with N$_{1}$$_{,}$$_{2}$ are strongly washed out due to Eqs. (39,40). In a radiative seesaw being plus with A$_{4}$ symmetry, Eq. (44) explicitly shows how the Yukawa coupling matrix Eq. (13) determined by Eq. (32) allows for a heavy Majorana neutrino to decay relatively out of equilibrium, simultaneously protecting the N$_{3}$ lepton number from being washed out, even though large e, µ -and τ -Yukawa couplings to N$_{1}$$_{,}$$_{2}$$_{,}$$_{3}$ exist. And, the CP asymmetries ε α 3 are 21 K e 3 = x $^{2}$g2 $^{$_{ν}$m}$∗ δ 2 N 3 η 6 bM , K µ 3 ≃ g 2 $^{$_{ν}$m}$∗ δ 2 N 3 η 2 bM (1 + 2 x √$_{3}$ sin φ ) , K τ 3 ≃ g 2 $^{$_{ν}$m}$∗ δ 2 N 3 η 2 bM (1 − 2 x √$_{3}$ sin φ ) , (44)