A 4-neutrino model with a Higgs triplet

Grimus, Walter; Pfeiffer, R.; Schwetz, Thomas

doi:10.1007/s100520050680

Cited by 4 publications

(5 citation statements)

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“…However, if the coupling constants g αβ are about 0.01 ÷ 0.1, then in order to obtain small neutrino masses the triplet VEV must be much smaller, namely v T ∼ 0.1 ÷ 1 eV. There are two ways to get a small v T : Firstly, one can assume that M, |µ| v, then |v T | |µ|v 2 /M 2 (scalar or type II seesaw mechanism) [94,109]; secondly, with M ∼ v, |µ| v one has |v T | ∼ |µ| [108]. In some sense the mechanism for obtaining small neutrino masses in the triplet model is analogous to the seesaw mechanism [93,94] (see subsequent subsection) since in both cases one has to introduce a second scale much larger (smaller) than the electroweak scale in order to generate small neutrino masses.…”

Section: The Triplet Modelmentioning

confidence: 98%

Neutrino Physics – Theory

Grimus

2004

Lectures on Flavor Physics

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Abstract. We discuss recent developments in neutrino physics and focus, in particular, on neutrino oscillations and matter effects of three light active neutrinos. Moreover, we discuss the difference between Dirac and Majorana neutrinos, neutrinoless ββ-decay, absolute neutrino masses and electromagnetic moments. Basic mechanisms and a few models for neutrino masses and mixing are also presented. MotivationIn recent years neutrino physics has gone through a spectacular development (for reviews see, for instance, [1][2][3][4]). Data concerning solar and atmospheric neutrino deficits have been accumulated, these deficits have been established as neutrino physics phenomena and the Solar Standard Model [5] has been confirmed. The last steps of this exciting development were the results of the SNO [6] and KamLAND experiments [7]: The SNO experiment provided a model-independent proof of solar ν e → ν µ,τ transitions and the terrestrial disappearance ofν e reactor neutrinos in the KamLAND experiment has shown that the puzzle of the solar neutrino deficit is solved by neutrino oscillations [8]. This gives us confidence that the same is true for the atmospheric neutrino deficit as well. For information on the history of neutrino oscillations see [9,10], for the recent experimental history see the contribution of G. Drexlin to these proceedings [4]. General reviews on neutrino physics can be found, for instance, in [11][12][13][14].These lecture notes are motivated by this development and aim at supplying the theoretical background for understanding and assessing it. In view of the importance of neutrino oscillations in this context, we will give a thorough discussion of vacuum neutrino oscillations and matter effects [15,16] (see Sect. 2); the description of the latter is tailored for an understanding of the flavour transformation of solar neutrinos and effects in earth matter. Then, in Sect. 3, we will switch to the subject of the neutrino nature, which is a question of principal interest but has no impact on neutrino oscillations; we will work out the difference between Dirac and Majorana neutrinos and the basics of Majorana neutrino effects. Eventually, in Sect. 4, we will come to the least established field of neutrino physics: models for neutrino masses and mixing. In view of the huge number of models and textures, we cannot try to cover the field but rather discuss a small selection of basic mechanisms

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Section: The Triplet Modelmentioning

confidence: 98%

Neutrino Physics – Theory

Grimus

2004

Lectures on Flavor Physics

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“…We first give the reader a glimpse of the scenario with a single triplet ∆ = (∆ ++ , ∆ + , ∆ 0 ), over and above the usual Higgs doublet φ, using the notation of [4]. ∆ is equivalently denoted by the 2 × 2 matrix…”

Section: A Single Scalar Triplet With a Cp-violating Phasementioning

confidence: 99%

CP-violating phase in a two Higgs triplet scenario: Some phenomenological implications

Chaudhuri

Mukhopadhyaya

2016

Phys. Rev. D

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We consider a scenario where, along with the usual Higgs doublet, two scalar triplets are present. The extension of the triplet sector is required for the Type II mechanism for the generation of neutrino masses, if this mechanism has to generate a neutrino mass matrix with two-zero texture. One CP-violating phase has been retained in the scalar potential of the model, and all parameters have been chosen consistently with the observed neutrino mass and mixing patterns. We find that a large phase ( 60 • ) splits the two doubly-charged scalar mass eigenstates wider apart, so that the decay H ++ 1

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“…With (38) and the best-fit value of ∆m 2 atm , this upper limit translates into s 2 13 > ∼ 0.005. The cosmological bound may be improved by one order of magnitude in the near future [18]; lowering the bound on j m j will imply a rise of the lower bound on s 2 13 . Thus, future measurements of s 2 13 [22], j m j , and m ββ , together with the bound (38) and j m j /m ββ ≃ 3, will test case C with the normal spectrum.…”

Section: Discussionmentioning

confidence: 99%

“…We shall assume the mixing angles, the atmospheric mass-squared difference ∆m 2 atm , and the solar mass-squared difference ∆m 2 ⊙ to be known-see (12) and (13). These are five quantities.…”

Section: The General Casementioning

confidence: 99%

“…The merits of scalar triplets are that they can be made very heavy while, at the same time, their vacuum expectation values (VEVs) become very small, through the so-called 'type-II seesaw' mechanism [11,12]. The smallness of the triplet VEVs explains the smallness of the neutrino masses, as an alternative to the ordinary ('type-I') seesaw mechanism [12,13].…”

Section: Introductionmentioning

confidence: 99%

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On a model with two zeros in the neutrino mass matrix

Grimus

Lavoura²

2005

J. Phys. G: Nucl. Part. Phys.

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We consider a Majorana neutrino mass matrix M ν with (M ν ) µµ = (M ν ) τ τ = 0, in the basis where the charged-lepton mass matrix is diagonal. We show that this pattern for the lepton mass matrices can be enforced by extending the Standard Model with three scalar SU (2) triplets and by using a horizontal symmetry group 4 . The type-II seesaw mechanism leads to very small vacuum expectation values for the triplets, thus explaining the smallness of the neutrino masses; at the same time, that mechanism renders the physical scalars originating in the triplets very heavy. We show that the conditions (M ν ) µµ = (M ν ) τ τ = 0 allow both for a normal neutrino mass spectrum and for an inverted one. In the first case, the neutrino masses must be larger than 0.1 eV and the atmospheric mixing angle θ 23 must be practically equal to 45 • . In the second case, the product sin θ 13 |tan 2θ 23 | must be of order one or larger, thus correlating the large or maximal atmospheric neutrino mixing with the smallness of the mixing angle θ 13

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A 4-neutrino model with a Higgs triplet

Cited by 4 publications

References 11 publications

Neutrino Physics – Theory

Neutrino Physics – Theory

CP-violating phase in a two Higgs triplet scenario: Some phenomenological implications

On a model with two zeros in the neutrino mass matrix

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