Large solar neutrino mixing and radiative neutrino mechanism

Kitabayashi, Teruyuki; Yasuè, Masaki

doi:10.1016/s0370-2693(01)01368-5

Cited by 54 publications

(34 citation statements)

References 61 publications

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“…Namely, a has L e = 2, b, b ′ have L e = 1 and d, e, d ′ have L e = 0 [31,32]. In the case that the conservation of L e is perturbatively violated by an interaction of |∆L e | = 1 with an appropriate small parameter η [31], it is not absurd to expect a ∝ η 2 , b ∝ η and d, e ∝ η 0 , which explain the required suppression of b. This mechanism is only possible for the normal mass hierarchy.…”

Section: General Resultsmentioning

confidence: 99%

“…(14) and (15). Since the experimentally allowed value of sin 2 θ 13 = O(10 −2 ) can describe the hierarchical ratio of ∆m 2 ⊙ /∆m 2 atm , we retain terms of O(sin 2 θ 13 ) in our calculations.…”

Section: Approximately µ-τ Symmetric Texturementioning

confidence: 99%

“…This fact apparently disfavors the requirement of the µ-τ symmetry. To have µ-τ symmetric mass terms, we must introduce several Higgs scalars with the different Z 2 parity, where their vev's can provide charged lepton masses [15,17,18] in such a way that the charged leptons acquire almost diagonal masses, which badly break the µ-τ symmetry. The price to pay is to have flavor-changing neutral current interactions due to the direct exchanges of these Higgs scalars.…”

Section: Introductionmentioning

confidence: 99%

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What doesμ−τsymmetry imply about neutrino mixings?

Fuki¹,

Yasuè²

2006

Phys. Rev. D

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The requirement of the µ-τ symmetry in the neutrino sector that yields the maximal atmospheric neutrino mixing is shown to yield either sin θ13 = 0 (referred to as C1)) or sin θ12 = 0 (referred to as C2)), where θ 12(13) stands for the solar (reactor) neutrino mixing angle. We study general properties possessed by approximately µ-τ symmetric textures. It is argued that the tiny µ -τ symmetry breaking generally leads to cos 2θ23 ∼ sin θ13 for C1) and cos 2θ23 ∼ ∆m 2 ⊙ /∆m 2 atm (≡ R) for C2), which indicates that the smallness of cos 2θ23 is a good measure of the µ-τ symmetry breaking, where ∆m 2 atm (∆m 2 ⊙ ) stands for the square mass differences of atmospheric (solar) neutrinos. We further find that the relation R ∼ sin 2 θ13 arises from contributions of O(sin 2 θ13) in the estimation of the neutrino masses ( m1,2,3) for C1), and that possible forms of textures are strongly restricted to realize sin 2 2θ12 = O(1) for C2). To satisfy R ∼ sin 2 θ13 for C1), neutrinos exhibit the inverted mass hierarchy, or the quasi degenerate mass pattern with |m1,2,3| ∼ O( ∆m 2 atm ), and, to realize sin 2 2θ12 = O(1) for C2), there should be an additional small parameter η whose size is comparable to that of the µ-τ symmetry breaking parameter ε, giving tan 2θ12 ∼ ε/η with η ∼ ε to be compatible with the observed large mixing.

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Section: General Resultsmentioning

confidence: 99%

Section: Approximately µ-τ Symmetric Texturementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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What doesμ−τsymmetry imply about neutrino mixings?

Fuki¹,

Yasuè²

2006

Phys. Rev. D

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“…Two parameter texture of neutrino mass matrix [4,11] which naturally gives bi-maximal neutrino mixing is disfavoured by the recent SNO experimental results. It needs more parameters in the neutrino mass matrix in order to explain the present neutrino experimental results [12]. Moreover, in order to satisfy the limit on effective Majorana neutrino mass the ν e ν e element of the neutrino mass matrix should be non-zero.…”

Section: Introductionmentioning

confidence: 97%

“…Although, the atmospheric neutrino oscillation mixing angle θ atm is maximal as observed by Super-Kamiokande(SK) [5,6] however, the LMA solution for the solar neutrino oscillation is best fitted with a considerably lower value of θ ⊙ . If we identify the θ ⊙ as θ 12 and θ atm as θ 23 then the CHOOZ [7] experiment has also constrained the third mixing angle θ 13 < 13 o . Furthermore, recent result from neutrinoless double beta decay (ββ 0ν ) experiment [8] has reported the bound on the effective Majorana neutrino mass ( by considering uncertnity of the nuclear matrix elements upto ±50% and the contribution to this process due to particles other than Majorana neutrino is negligible [9]) as m = ( 0.05 − 0.84 ) eV at 95% c.l.…”

Section: Introductionmentioning

confidence: 99%

Texture of neutrino mass matrix in view of recent neutrino experimental results

Ghosal

Majumdar

2002

Phys. Rev. D

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In view of recent neutrino experimental results such as SNO, Super-Kamiokande (SK), CHOOZ and neutrinoless double beta decay (ββ0ν ) ,we consider a texture of neutrino mass matrix which contains three parameters in order to explain those neutrino experimental results. We have first fitted parameters in a model independent way with solar and atmospheric neutrino mass squared differences and solar neutrino mixing angle which satisfy LMA solution. The maximal value of atmospheric neutrino mixing angle comes out naturally in the present texture. Most interestingly, fitted parameters of the neutrino mass matrix considered here also marginally satisfy recent limit on effective Majorana neutrino mass obtained from neutrinoless double beta decay experiment. We further demonstrate an explicit model which gives rise to the texture investigated by considering an SU (2)L × U (1)Y gauge group with two extra real scalar singlets and discrete Z2 × Z3 symmetry. Majorana neutrino masses are generated through higher dimensional operators at the scale M . We have estimated the scales at which singlets get VEV's and M by comparing with the best fitted results obtained in the present work. PACS number(s): 13.38. Dg, 14.60.Pq.

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Determination of neutrino mass texture for maximal CP violation

2005

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We show a general form of neutrino mass matrix (M ), whose matrix elements are denoted by Mij (i.j=e, µ, τ ) as flavor neutrino masses, that induces maximal CP violation as well as maximal atmospheric neutrino mixing. The masses of Mµµ, Mττ and Mµτ + σMee (σ = ±1) turn out to be completely determined by Meµ and Meτ for given mixing angles. The appearance of CP violation is found to originate from the interference between the µ-τ symmetric part of M and its breaking part. If |Meµ| = |Meτ |, giving either Meµ = −σe iθ Meτ or Meµ = −σe iθ M * eτ with a phase parameter θ, is further imposed, we find that |Mµµ| = |Mττ | is also satisfied. These two constraints can be regarded as an extended version of the constraints in the µ-τ symmetric texture given by Meµ = −σMeτ and Mµµ = Mττ . Majorana CP violation becomes active if arg(Mµτ ) = arg(Meµ) + θ/2 for Meµ = −σe iθ Meτ and if arg(Mµτ ) = θ/2 for Meµ = −σe iθ M * eτ .

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Large solar neutrino mixing and radiative neutrino mechanism

Cited by 54 publications

References 61 publications

What doesμ−τsymmetry imply about neutrino mixings?

What doesμ−τsymmetry imply about neutrino mixings?

Texture of neutrino mass matrix in view of recent neutrino experimental results

Determination of neutrino mass texture for maximal CP violation

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