Renormalisation group corrections to the littlest seesaw model and maximal atmospheric mixing

The Littlest Seesaw (LS) model involves two right-handed neutrinos and a very constrained Dirac neutrino mass matrix, involving one texture zero and two independent Dirac masses, leading to a highly predictive scheme in which all neutrino masses and the entire PMNS matrix is successfully predicted in terms of just two real parameters. We calculate the renormalisation group (RG) corrections to the LS predictions, with and without supersymmetry, including also the threshold effects induced by the decoupling of heavy Majorana neutrinos both analytically and numerically. We find that the predictions for neutrino mixing angles and mass ratios are rather stable under RG corrections. For example we find that the LS model with RG corrections predicts close to maximal atmospheric mixing, θ23 = 45° ± 1°, in most considered cases, in tension with the latest NOvA results. The techniques used here apply to other seesaw models with a strong normal mass hierarchy.


Introduction
Although it has been well established by neutrino oscillation experiments that neutrinos are massive particles and lepton flavors are significantly mixed [1], the dynamical origin of neutrino mass generation and lepton flavor mixing is yet unknown [2][3][4][5][6][7]. Among a number of theoretical models for tiny neutrino masses, the simplest and most elegant one should be the canonical seesaw model [8][9][10][11][12], in which the standard model (SM) is extended with right-handed neutrino singlets N iR and the gauge-invariant Lagrangian relevant for neutrino masses and lepton flavor mixing reads where L andH ≡ iσ 2 H * stand respectively for the left-handed lepton and Higgs doublets, E R and N R are the right-handed charged-lepton and neutrino singlets, Y l and Y ν are the charged-lepton and Dirac neutrino Yukawa coupling matrices, M R is the Majorana mass matrix of right-handed neutrino singlets. After the Higgs field acquires its vacuum expectation value (vev), i.e., v ≡ H ≈ 174 GeV, and the gauge symmetry is spontaneously broken, the charged-lepton and Dirac neutrino mass matrices are given by

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However, the general seesaw model involves a large number of free parameters mainly arising from the Dirac neutrino Yukawa coupling matrix Y ν in the flavor basis, where the charged-lepton and right-handed neutrino mass matrices M l = M l ≡ Diag{m e , m µ , m τ } and M R = M R ≡ Diag{M 1 , M 2 , M 3 } are diagonal. In order to reduce the number of free parameters in a successful seesaw model, one may consider the so-called minimal version of only two right-handed neutrinos, which was first proposed by one of us in refs. [13,14], focussing on the decoupling case of M 3 M 2 > M 1 , and with one texture zero in the Dirac neutrino mass matrix M D . Therefore, the lightest neutrino is massless, namely, m 1 = 0 in the case of normal neutrino mass hierarchy (NH, i.e., m 1 < m 2 < m 3 ) and m 3 = 0 in the case of inverted neutrino mass hierarchy (IH, i.e., m 3 < m 1 < m 2 ). A further simplification of the minimal seesaw model has been considered by Frampton, Glashow and Yanagida [15], who assume two texture zeros in the Dirac neutrino mass matrix M D and demonstrate that both neutrino masses and the cosmological matter-antimatter asymmetry can be explained in this economical setup via the seesaw and leptogenesis mechanisms [16]. The phenomenology of the minimal seesaw model was subsequently fully explored in the literature [17][18][19][20][21][22][23]. In particular, the NH case in the Frampton-Glashow-Yanagida model has been shown to be already excluded by the latest neutrino oscillation data [22,23].
More recently, the Littlest Seesaw (LS) model was put forward in refs. [24][25][26][27][28], where two right-handed neutrino singlets N atm R and N sol R are introduced into the SM and a simple but viable structure of the Dirac neutrino Yukawa coupling matrix is conjectured as The low-energy phenomenology in the LS model case A has been studied in detail both numerically [24,25] and analytically [26], where it has been found that the best fit to experimental data of neutrino oscillations is obtained for n = 3 for a particular choice of phase η ≈ 2π/3, while for case B the preferred choice is for n = 3 and η ≈ −2π/3 [24,28]. The prediction for the baryon number asymmetry in our Universe via leptogenesis within case A is also studied [27], while a successful realization of the flavor structure of Y ν for case B in eq. (1.2) through an S 4 × U(1) flavor symmetry is recently achieved in ref. [28], where the symmetry fixes n = 3 and η = ±2π/3.
With the parameters n = 3 and η = ±2π/3 fixed, there are only two remaining real free Yukawa parameters in eq. (1.2), namely a, b, so the LS predictions then depend on only two real free input combinations m a = a 2 v 2 /M atm and m b = b 2 v 2 /M sol , in terms of which all neutrino masses and the PMNS matrix are determined. For instance, if m a and m b are chosen to fix m 2 and m 3 , then the entire PMNS mixing matrix, including phases, is determined with no free parameters. It turns out that the LS model predicts close to maximal atmospheric mixing at the high scale, θ 23 ≈ 46 • for case A , or θ 23 ≈ 44 • for JHEP12(2016)023 case B [28], where both predictions are challenged by the latest NOvA results in the ν µ disappearance channel [29,30] which indicates that θ 23 = 45 • is excluded at the 2.5 σ CL, although T2K measurements in the same channel continue to prefer maximal mixing [31].
In view of the great simplicity and high predictivity of the LS model, we are well motivated to consolidate its theoretical predictions by investigating the renormalizationgroup (RG) running of neutrino masses and lepton flavor mixing parameters, which is necessary to be taken into account as the seesaw scale is as high as Λ SS = 10 10−15 GeV, close to the scale of grand unified theories Λ GUT = 2×10 16 GeV. In particular, the threshold effects caused by the decoupling of two heavy right-handed neutrinos are examined in an analytical way. We demonstrate that the predictions for neutrino mixing angles and CPviolating phases are rather stable against the radiative corrections. For example, we find that the LS model including RG corrections for both cases A and B, both with and without supersymmetry, predicts maximal atmospheric mixing in the range θ 23 = 45 • ± 1 • . Both numerical and analytical calculations are implemented to understand our observations. The results are expected to be indicative of a large class of seesaw models with a strong mass hierarchy that predict close to maximal atmospheric mixing, so we conclude that RG corrections are not generally sufficient to rescue such models if maximal atmospheric mixing becomes excluded.
The remaining part of our paper is organized as follows. In section 2, the general formalism for RG running of neutrino parameters and the treatment of seesaw threshold effects are briefly reviewed. After a brief review on the basic idea of the LS model in section 3, the radiative corrections are calculated and discussed in section 4. Finally, we summarize our main results in section 5.

Renormalisation group running
As is well known [32], neutrino masses and flavor mixing parameters at the low-energy scale are governed by the dimension-five Weinberg operator κ( L ·H)(H T · c L )/2, which can be derived by integrating out the heavy Majorana neutrinos. The effective neutrino coupling matrix κ is related to the neutrino mass matrix as M ν = κv 2 in SM or M ν = κv 2 sin 2 β in the minimal supersymmetric standard model (MSSM), where tan β denotes the ratio between the vev's of two Higgs doublets in MSSM. If the mass spectrum of heavy Majorana neutrinos is not strongly hierarchical, it is an excellent approximation that all of them are simultaneously integrated out at a common seesaw scale, namely, In the case of M 1 M 2 M 3 , however, we have to decouple the heavy Majorana neutrino one by one and carefully deal with the matching between the effective theory below M i (for i = 1, 2, 3) and the other one above. The detailed discussions on the RG running of neutrino parameters and threshold effects in the canonical seesaw model can be found in refs. [33,35,36,39].
Above the seesaw thresholds, the one-loop RG equations of model parameters have been derived in refs. [33,35,36] and are collected as below 1, 2, 3) and the lepton flavor mixing matrix U can be found by diagonalizing M A ν , namely, In practice, we first perform a basis transformation via where U TB stands for the tri-bimaximal mixing pattern [40][41][42][43] After this transformation, we have which can be further diagonalized by a rotation U b (θ) in the 2-3 complex plane. The corresponding rotation angle θ is given by tan 2θ = 2|xy * + yz * |/(|z| 2 − |x| 2 ), and thus the mixing matrix is U = U TB U b (θ). As the lightest neutrino is massless, i.e., m 1 = 0, the lepton flavor mixing matrix U can be parametrized in terms of three mixing angles θ ij for ij = 12, 13, 23, one Dirac-type CP-violating phase δ and one Majorana-type CP-violating phase σ, namely, where c ij ≡ cos θ ij and s ij ≡ sin θ ij have been defined. As shown in ref. [26], neutrino masses {m 2 , m 3 }, flavor mixing angles {θ 12 , θ 13 , θ 23 }, and CP-violating phases {δ, σ} can be exactly calculated in terms of the model parameters m a , m b and η. However, in the sequential-dominance approximation, implying m a m b and |z| |x|, |y|, the neutrino masses turn out to be while the mixing angles are where tan 2θ ≈ √ 6m b (n − 1)/ m a + m b e iη (n − 1) 2 and ω = arg m a + m b e iη (n − 1) 2 − η. It is worthwhile to notice that the correlation between θ 12 and θ 13 in the above equation is exact, as a salient feature of the LS model. In addition, two CP-violating phases are [26] sin δ ≈ − where ∆m 2 ji ≡ m 2 j − m 2 i is the neutrino mass-squared difference.

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If the form of Y ν in case B in eq. (1.2) is taken, the corresponding effective neutrino mass matrix M B ν is related to that in case A via M B ν = P 23 M A ν P T 23 , where P 23 denotes the elementary transformation matrix that exchanges the second and third columns or rows of an arbitrary 3 × 3 matrix. While M A ν = U · Diag{0, m 2 , m 3 } · U T has been archived, we immediately arrive at M B ν = (P 23 U )·Diag{0, m 2 , m 3 }·(P 23 U ) T . Then, it is straightforward to verify that such a transformation leads to the following relations between two sets of mixing parameters Therefore, it is unnecessary to explicitly diagonalize M B ν , and all the mixing parameters can be calculated by using the above relations while neutrino mass eigenvalues remain the same. Some comments on the model predictions are in order: • Two predictive ansätze of Y ν with n = 3 will be considered. The first one is Y ν in case A, and η = 2π/3, together with m a = 25.67 meV and m b = 2.684 meV, is assumed. • As m 1 = 0 is implied in the LS, neutrino mass hierarchy is obviously normal. In this case, the effective neutrino mass for neutrinoless double-beta decays is as small as m ββ = m b = 2.684 meV, which is impossible to measure in the foreseeable future. These conclusions are applicable to both case A with η = 2π/3 and case B with η = −2π/3.
• For the chosen input parameters, the baryon number asymmetry is found to be Y B ≈ 8.4 × 10 −11 can be reproduced for M 1 ≈ 3.9 × 10 10 GeV [25]. As indicated by eq. (3.7), the CP violation in neutrino oscillations and that for the cosmological matter-antimatter asymmetry are determined by the same parameter η. For a different value of η, the heavy neutrino masses M 1 and M 2 can be changed by choosing suitable parameters a and b, without spoiling the low-energy predictions for neutrino masses and mixing angles.
Since the seesaw scale is extremely high, one may be worried about whether the RG running effects can significantly modify the above conclusions. This problem will be addressed in the following section.

JHEP12(2016)023 4 Renormalisation group corrections to the littlest seesaw model predictions
The RG running effects on neutrino mixing parameters in the SM and in the NH case are expected to be rather small. However, the strongly hierarchical mass spectrum M 1 M 2 implies that the seesaw threshold effects can be important, depending on the flavor structure of Dirac neutrino Yukawa coupling matrix Y ν . On the other hand, if the LS model is supersymmetrized, a large value of tan β leads to an increase of charged-lepton Yukawa couplings, which may enhance the RG running effects. Therefore, we are motivated to carry out a detailed study of those effects. Since the analysis is almost identical for both case A and B, for definiteness we only consider the RG corrections in full detail for one of the two cases, namely case A, then later highlight the differences which are important for case B.

Case A from Λ GUT to M 2
First of all, we need to specify the input parameters at the initial scale µ 0 = Λ GUT .
In this subsection, we focus on the form of Y ν in case A, and the other scenario will be considered later. We first consider the mass ordering of right-handed neutrinos Later we shall consider the results for the alternative mass ordering. Note that the low energy effective neutrino mass matrix is independent of this heavy right-handed neutrino mass ordering, but the RG corrections in the heavy threshold region dependent on it.
To be consistent with the consequential dominance, we take M 1 = 10 12 GeV and M 2 = 10 15 GeV for illustration, implying M 2 M 1 . Furthermore, as shown in the previous section, the global-fit results of neutrino mixing parameters can be well reproduced for n = 3, together with m a = 25.67 meV, m b = 2.684 meV and η = 2π/3. In this case, Y ν (µ 0 ) is given by eq. (1.2) with a ≈ 0.03 and b ≈ 0.3, satisfying b a. Therefore, it is interesting to notice a strong hierarchy among the matrix elements of Y ν , and | (Y ν ) µ2 | = 3b is the largest one. Note that such a choice of Y ν (µ 0 ) also implies that we are in the flavor basis at this initial boundary scale, namely, both Y l (µ 0 ) and M R (µ 0 ) are diagonal.
Since the lepton flavor mixing matrix arises from the mismatch between the diagonalization of charged-lepton Yukawa matrix Y l and that of the neutrino mass matrix M ν , we therefore pay particular attention to the RG running of both Y l and M ν . It is well known that below the seesaw threshold (i.e., µ < M 1 ), Y l would always stay diagonal at one-loop level if it is diagonal initially at the boundary [see eq. (2.9)]. However, this is no longer the case when considering the RG running above the seesaw threshold, due to the term involving Y ν in eq. (2.1). In the following we then trace the evolution of both Y l and M ν analytically for the running between Λ GUT and M 2 .
Let us start with the RG running of M ν . Above the seesaw threshold µ = M 2 , the RG running of the would-be neutrino mass matrix M ν ≡ κv 2 in the SM (or M ν ≡ κv 2 sin 2 β in the MSSM) is governed by eq. (2.8). Neglecting the relatively small contribution from Y l , JHEP12(2016)023 the evolution of the flavor structure in M ν is mainly driven by the term involving where the approximation a b 3b has been made in Y ν to simplify our analytical discussions. If the second column of Y ν is fully kept, H ν will be a 3 × 3 real and symmetric matrix without any vanishing elements, and it is difficult to deal with the radiative corrections to neutrino mixing angles in an analytical way. In the approximation made in eq. (4.1), it is straightforward to solve the eq. (2.8) and obtain where all the parameters at the initial scale µ 0 = Λ GUT are denoted by a subscript or superscript "0". More explicitly, we have defined M 0 ν ≡ M ν (t 0 ), and the evolution functions I α and I ν are found to be Assuming that b(t) does not run much from the initial value At the threshold µ = M 2 = 10 15 GeV, one can obtain t 0 − t = ln(Λ GUT /M 2 )/(16π 2 ) ≈ 0.02 and thus ν ≈ 7.7 × 10 −3 , which serves as an excellent perturbation parameter. Therefore, we arrive at with (M 0 ν ) αβ for α, β = e, µ, τ being the matrix elements of M 0 ν . It is interesting to note that the one-loop RG corrections to M ν are quite similar to those for κ below the seesaw threshold, where the dominant corrections from the tau Yukawa coupling y τ modify the third row and column of κ.
To extract the RG corrections to three mixing angles, we have to diagonalize the mass matrix in eq. (4.5). This can be achieved perturbatively in two steps. First, as shown in the previous section, the leading-order mass matrix M 0 ν can be diagonalized by a unitary matrix real and positive. Here U TB is the tri-bimaximal mixing matrix given in eq. (3.2), and
Second, after the unitary transformation we are left with a mass matrix M ν p , which is almost diagonal except for small corrections proportional to in both diagonal and off-diagonal entries. As we are interested in the radiative corrections to neutrino mixing angles, it is sufficient to find out a unitary matrix that diagonalize The unitary matrix U ν p can be found by using the standard perturbation theory [47], and the final mixing matrix in the neutrino sector is given by U ν = U ν 0 U ν p up to one physical Majorana-type CP-violating phase. Having obtained the mixing matrix U ν for the neutrino mass matrix M ν at M 2 , we then focus on the mixing matrix from the charged-lepton Yukawa matrix Y l . To this end, we first study the evolution of Y l from Λ GUT to M 2 with the help of eq. (2.1). Unlike the above discussions on the evolution of M ν , now we can keep all the non-zero elements in H ν , owing to the simpler structure of the RG equation for Y l , namely, Since we are interested in the flavor mixing induced by Y l , the first term with a flavorindependent coefficient α l in the above RG equation can be neglected. Then, we solve it analytically, with a diagonal form of Y l at the high-energy boundary Λ GUT . In view of the strong hierarchy y 2 e y 2 µ y 2 τ , the unitary matrix U l defined by U † l Y l Y † l U l = Diag{y 2 e , y 2 µ , y 2 τ } turns out to be where l ≡ 3b 2 0 (t 0 − t)/2 serves as another small parameter for expansion, and θ l = arctan(3/4)/2 stems from the diagonalization of H ν , which is needed to solve eq. (4.7) analytically.
With U l in eq. (4.8), we obtain the lepton mixing matrix U = U † l U ν at the scale of M 2 . Thus, three neutrino mixing angles at µ = M 2 can be exacted in the leading-order approximation    Numerically, we have made a comparison between the results from the analytical formulas and those from solving exactly the RG equations. For illustration, the RG running effects in the SM case are considered. The final results are shown in table 1. As one can see, the approximate formulas in eq. (4.9) yield very good predictions (namely, the fifth row in table 1) for θ 13 and θ 23 . However, for θ 12 , we obtain a slightly larger value, which can be ascribed to the rough approximation at the very beginning, namely, keeping only the dominant term in H ν . To see this point clearly, we calculate the mixing angles directly from eq. (4.5), while the exact U l is obtained from the actual RG running, and show the numerical results in the fourth row of table 1. An excellent agreement between the values in the fourth and fifth rows validates the above perturbation method leading to eq. (4.9).

Case
In this subsection we proceed with case A to consider the threshold effects due to the decoupling of heavy right-handed neutrinos on the neutrino mixing angles. Since M 2 is very close to Λ GUT , it is reasonable to assume that the RG running effects of both Y ν and M R in the first stage are negligible. Therefore, we have the following light neutrino mass matrix at µ = M 2 , which can be decomposed into two terms where Y ν and Y ν stand for the first and second columns of Y ν given in eq. (1.2), respectively. As we have shown in section 2, in the JHEP12(2016)023 SM the RG equations of M ν and κ in the effective theory after the decoupling of N 2 have different coefficients from the Higgs self-coupling and gauge coupling contributions, leading to significant threshold effects for a hierarchical mass spectrum of heavy neutrinos. In the MSSM, one has to replace v 2 with v 2 sin 2 β in eq. (4.7), but both M ν and κ evolve in the same way, which is not very interesting in view of threshold effects (although in the RG equations we need to use Y ν instead of Y ν ). For this reason, we focus on the case of SM.
For clarity, we recap the RG equations of M ν and κ in the SM, which have already been given in eqs. (2.8) and (2.10) and can be expressed as follows and α X is given by In the case of M 1 = 10 12 GeV and M 2 = 10 15 GeV under discussion, all three entries in Y ν are quite small, we thus neglect both H l and H ν in the RG equations for both M ν and κ. As an immediate consequence, the running of M ν and κ only differ in the flavorindependent coefficient α X . Following ref. [48], we can obtain the neutrino mass matrix M ν at µ = M 1 as Hence, the radiative corrections to three neutrino mixing angles come from the ξv 2 κ term, which reflects how large the running effects are between M 2 and M 1 .
To start with, we can diagonalize the neutrino mass matrix at M 2 via a unitary transformation, i.e., M ν = U D ν U T with D ν = Diag{0, m 2 , m 3 }. The unitary matrix U is given by where P ρ ≡ Diag{e iρ 1 , e iρ 2 , e iρ 3 } and P ω ≡ Diag{1, e iω 2 , 1} are diagonal phase matrices, s ij ≡ sin θ ij and c ij ≡ cos θ ij for ij = 12, 13, 23 have been defined. Here the symbols with a single prime indicate the parameters at the scale of M 2 , while those with double primes are the parameters at M 1 . Note that there in general will be two Majorana-type CP-violating

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phases in the last matrix on the right-hand side of eq. (4.13), of which however only one is physical because of one massless neutrino (i.e., m 1 = 0). Next, we consider the flavor structure of κ, which is reconstructed by the second column of Y ν and M 2 . Keeping all the elements of κ, one can obtain would be a small expansion parameter. We then diagonalize M ν perturbatively following the same procedure as that in the previous section. In the final step, we multiply the obtained mixing matrix U ν from the M ν by the previously found U l so as to construct the flavor mixing matrix at M 1 , i.e., U(M 1 ) = U † l U ν . Note that Y l does not run much from M 2 to M 1 . The three mixing angles are then extracted as where t ij ≡ tan θ ij and t ij ≡ tan θ ij have been introduced for ij = 12, 23, and α ij ≡ η − ρ i − ρ j − 2ω 2 , β ij ≡ δ + η − ρ i − ρ j , and γ ij ≡ ρ i − ρ j have been defined for i, j = 1, 2, 3. Note that only the leading-order contributions from , m 2 /m 3 and θ 13 are kept in eq. (4.18), except that for θ 12 we also include corrections of the order of θ 13 for better accuracy. Numerical verification of our approximate formulas is also given in table 1. Using the exact results of three mixing angles at M 2 as input, we compute the approximate results at M 1 from eq. (4.18), which have been shown in the last row. In comparison with the exact results in the third row, we can observe that the approximate formulas indeed capture the major threshold effects.
As is well known, the running effects of neutrino mixing parameters below the seesaw scale µ = M 1 are insignificant, in particular for the NH case. On the other hand, even in the leading-order approximation, it is complicated to derive any analytical results for the CP-violating phases and neutrino masses. Therefore, in order to fully address the RG  Table 2. Three mixing angles {θ 12 , θ 13 , θ 23 }, two CP-violating phases {δ, σ} and non-zero light neutrino masses {m 2 , m 3 } at various energy scales according to two scenarios in Case A given in figure 1. For comparison, we also show the best-fit results from ref. [44] in the last column.
running effects from Λ GUT = 2 × 10 16 GeV to Λ EW = 10 3 GeV, we numerically solve the full set of RG equations with the REAP package [35] for three neutrino mixing angles {θ 12 , θ 13 , θ 23 }, two CP-violating phases {δ, σ}, and two neutrino masses {m 2 , m 3 }. The final results are depicted in figure 1 (together with numerical values at various energy scales in table 2), and the main features are summarized as follows: (1) All the mixing angles and CP-violating phases are rather stable against the RG corrections. The largest deviation from the initial value is observed for θ 23 , but even in this case the deviation is only around one degree. Therefore, the theoretical predictions for mixing angles and CPviolating phases in the LS model can be applied at both low-and high-energy scales. (2) However, it should be noticed that the running of absolute neutrino masses is remarkable.
To be consistent with neutrino oscillation data, the initial values of Y ν should be multiplied by a factor of 1.25 (or 1.15) for SM (or MSSM), which has already been taken into account in figure 1. This overall scaling of Y ν does not alter the results for three flavour mixing angles at the high-energy boundary, but it does modify the absolute values of Y ν , leading to slightly larger a and b.

Case B
We now discuss case B in eq. (1.2) with n = 3 and η = −2π/3. It has been found [24,28] that this alternative scenario of Y ν also yields a phenomenologically successful and predictive description of neutrino masses and lepton mixing parameters, if RG corrections are ignored [28]. Following a similar treatment as in the previous case, we now study the RG running effects given this new form of Y ν . The analytical formulas for flavour mixing angles are almost the same as before, except for two differences.
(1) During the running from Λ GUT to M 2 , we shall take a form of H ν as instead of that in eq. (4.1). Consequently, in order to obtain M ν at M 2 , we need to consider corrections to the third row and column of M 0 ν at Λ GUT . In this case, we have to replace eq. (4.5) with the following Adopting the previous diagonalization procedure, we find that the analytical formulas JHEP12(2016)023   Table 3. Three mixing angles {θ 12 , θ 13 , θ 23 }, two CP-violating phases {δ, σ} and non-zero light neutrino masses {m 2 , m 3 } at various energy scales according to two scenarios in Case B given in figure 2. For comparison, we also show the best-fit results from ref. [44] in the last column.
1. Now that the mass ordering of two heavy Majorana neutrinos is inverted, we have to exchange the two columns of Y ν in eq. (1.2), namely, (4.24) When crossing the seesaw thresholds, we first decouple the heaviest neutrino at M 2 (by ignoring the second column of Y ν for µ < M 2 ), and then the second one at M 1 . It is evident that the flavour structure of Y ν at each stage is distinct from that for the normal ordering.
2. During the running from Λ GUT to M 2 , the evolution of neutrino mixing angles is mainly governed by where the dominant element a 2 ≈ 0.88 is much larger than the others. Moreover, H ν is not diagonal, and thus affects greatly the flavour structure of M ν . For the same reason, it seems impossible to solve the RG equation of M ν analytically.
3. During the running from M 2 to M 1 , the reduced Yukawa coupling matrix involves only the parameter b ≈ 0.01, which is much smaller than that in the previous case. Therefore, we expect insignificant running effects from the neutrino sector.
Instead of an analytical approach, we adopt the exact numerical approach to solve the RG equations and show the final results in figures 3 and 4 for cases C and D, respectively. The values at various energy scales are summarized in tables 4 and 5. Note that the same scaling factor of 1.25 (1.15) has been applied to Y ν for SM (MSSM) so as to obtain better JHEP12(2016)023  • When running towards low energies, the ratio of m 2 /m 3 becomes increasing while in the previous case it is decreasing. Moreover, the running of such a ratio is also more appreciable, and becomes in contradiction with the data. This can be attributed  Table 4. Three mixing angles {θ 12 , θ 13 , θ 23 }, two CP-violating phases {δ, σ} and non-zero light neutrino masses {m 2 , m 3 } at various energy scales according to two scenarios in Case C given in figure 3. The best-fit results from ref. [44] are shown in the last column.  Table 5. Three mixing angles {θ 12 , θ 13 , θ 23 }, two CP-violating phases {δ, σ} and non-zero light neutrino masses {m 2 , m 3 } at various energy scales according to two scenarios in Case D given in figure 4. The best-fit results from ref. [44] are shown in the last column.
to a more significant running of m 3 . In principle, we can adjust both m a and m b such that neutrino masses are in good agreement with data, and even the tension of mixing angles with observations may also get reduced. For this purpose, a complete scan of model parameters should be carried out, which however is beyond the scope of the present work.
It is very interesting to notice that a deviation of θ 23 from the maximal mixing by 3 • can only be realised in the case of M atm M sol and the flavour structure of Y ν takes the form case D in eq. (4.24). In the other cases, we are left with a nearly maximal mixing θ 23 = 45 • ± 1 • , including the radiative corrections.  To compare with the current experimental data, we also include the 1σ and 3σ allowed regions according to the global-fit results in ref. [44]. Several observations are then made: • In the entirely considered ranges of M atm and M sol , the running effects for the three mixing angles are all rather small, at most one degree for θ 13 and θ 23 .
• In comparison with the global-fit results, we see that having θ 12 to be compatible with the data, even at the level of 1σ, is easy to achieve. However, for θ 13 and θ 23 , although a 3σ level of agreement is also not difficult, reaching a compatibility at the 1σ level becomes impossible in θ 23 , and for θ 13 it is only in the case of SM that there exists some parameter space of M atm and M sol .
It should be pointed out that in figure 5 we also consider the case where M atm and M sol are almost degenerate, while the previously derived analytical results are only applicable to the hierarchical cases. We then turn to the other form of Y ν , namely, Case B in eq. (1.2) and Case D of eq. (4.24). In figure 6 we show the numerical results obtained in the same way as the above. As one can see, the running of three mixing angle is again rather insignificant, except for θ 23 in the case of SM, for which the decrease of θ 23 around 3 • can appear when M atm ∼ 10 15 GeV as discussed in the previous section. Therefore, we have extended our previous conclusion, i.e., in the presence of radiative corrections a close to maximal atmospheric mixing of θ 23 = 45 • ± 1 • can be achieved in most of cases, to the scenario that both M atm and M sol are varied in a wide range. Such a robust prediction on θ 23 calls for scrutiny under future neutrino experimental results.

Summary
Seesaw models are able to explain simultaneously both tiny neutrino masses and the cosmological matter-antimatter asymmetry, but generally involve a large number of parameters. By contrast, the LS model involves two right-handed neutrinos and a very constrained Dirac mass matrix, involving one texture zero and two independent Dirac masses, leading to a highly predictive scheme in which all neutrino masses and the entire PMNS matrix is JHEP12(2016)023 successfully predicted in terms of just two real parameters. To be precise, we have considered two simple structures of the Dirac neutrino Yukawa coupling matrix Y ν , denoted as cases A and B, with M atm M sol each of which contains only three real parameters a, b, and η, which may be fixed by symmetry arguments to be a cube root of unity, leading to testable predictions for low-energy neutrino experiments. We also considered two related cases C and D corresponding to M sol M atm .
Each case predicts a normal neutrino mass hierarchy with {m 1 , m 2 , m 3 } = {0, 8.6, 50} meV, where the effective neutrino mass m ββ = 2.7 meV for neutrinoless double-beta decays is so small that observation of such decays is impossible in the foreseeable future. The LS model also predicts an almost maximal CP-violating phase δ = −87 • (cases A,C) or −93 • (cases B,D) which will be verified or ruled out in the future oscillation experiments. The LS model also predicts close to maximal atmospheric mixing at the high scale, θ 23 ≈ 46 • (cases A,C), or θ 23 ≈ 44 • (cases B,D), where both predictions are challenged by the latest NOvA results in the ν µ disappearance channel which indicates that θ 23 = 45 • is excluded at the 2.5 σ CL, although T2K measurements in the same channel continue to prefer maximal mixing.
In this paper, motivated by the simplicity and predictivity of the LS, we have calculated the RG corrections to the LS predictions, for both cases A and B, with and without supersymmetry, including also the threshold effects induced by the decoupling of heavy Majorana neutrinos both analytically and numerically. We also performed a numerical RG analysis for cases C and D. In particular we have investigated the RG running of three neutrino mixing angles, taking account of the threshold effects induced by the decoupling of heavy Majorana neutrinos, including both possible mass orderings of right-handed neutrinos. Although the running effects are rather small both in the SM and in the MSSM with tan β = 30, we have carried out an analytical treatment of the RG running between two seesaw thresholds for cases A,B. We emphasise that the full numerical calculation was performed to verify our analytical and approximate results. We find that the predictions for neutrino mixing angles and mass ratios are rather stable under RG corrections. For example we find that the LS model with RG corrections always predicts close to maximal atmospheric mixing θ 23 = 45 • ± 1 • , for most considered cases, which remains in tension with the latest NOvA results. The one exception is case D for the SM, where θ 23 = 41.5 • after RG corrections.
Finally we mention that the techniques used here may be applied to other seesaw models with a strong normal mass hierarchy. We hope that such future studies would be helpful in revealing how the RG running modifies theoretical predictions for neutrino mixing parameters, for other related neutrino mass models with flavour symmetries. In particular, the results here are expected to be indicative of a large class of seesaw models with a strong mass hierarchy that predict close to maximal atmospheric mixing, so we conclude that RG corrections are not generally sufficient to rescue such models if maximal atmospheric mixing becomes excluded.