 [Deg.] 13 0 2 4 6 8 10 12 B −14 10$^{−13}$ 10$^{−12}$ 10$^{−11}$ 10$^{−10}$ 10 −9 10  [Deg.] 23 38 40 42 44 46 48 50 B −14 10$^{−13}$ 10$^{−12}$ 10$^{−11}$ 10$^{−10}$ 10 −9 10 FIG. 9: The same sa Fig. 8 except for M$_{3}$ ≃ 1TeV and δ$_{N}$$_{3}$$_{η}$ = 10 − $^{6}$. which indicates electron-flavor effect plays a crucial role in reproducing BAU. If we take, for example, δ$_{N}$$_{3}$$_{η}$ = 10 − 5 the magnitude of washout factors are given as and Fig. 8 shows the behavior of η$_{B}$ as functions of θ$_{13}$ and θ$_{23}$ , representing a successful leptogenesis in the range of 1 σ neutrino oscillation data. In weak wash-out regime K e 3 ≪ K µτ 3 < 1, assumed that N$_{3}$ is not initially present in the plasma, but they are generated by the inverse decays and scatterings, the resulting baryon-to-photon ratio η$_{B}$ including lepton flavor effects can be simply given as where in this approximation ε µ 3 + ε τ 3 = − ε e 3 is used, and K$_{3}$ = K e 3 + K µ 3 + K τ $_{3}$. This case indicates muon- and tau-flavor effects play a crucial role in reproducing BAU. For example, for δ$_{N}$$_{3}$$_{η}$ = 10 − 6 the magnitude of washout factors are given as and Fig. 9 shows the behavior of η$_{B}$ as functions of θ$_{13}$ and θ$_{23}$ , representing a successful leptogenesis in the range of 1 σ neutrino oscillation data. In the case of M$_{2}$ ⪆ ¯ m$_{η}$ , for M$_{1}$ > M$_{3}$ > M$_{2}$ ≳ ¯ m$_{η}$ which corresponds to degenerate normal mass ordering of light neutrinos, from Eq. (13) and Eq. (39), the wash-out parameters K e 3 = 0 . 0006 − 1 . 7 , K µ 3 = 55 − 101 , K τ 3 = 61 − 124 , (47) η$_{B}$ ≃ 2 × $_{10}$− $^{3}$x sin φK$_{3}$K µ $_{3}$( ε µ 3 − ε τ $_{3}$) , (48) K e 3 = 0 . 00001 − 0 . 017 , K µ 3 = 0 . 5 − 1 . 1 , K τ 3 = 0 . 6 − 1 . 3 , (49) 23