Quark lepton complementarity and renormalization group effects

Small discrete family symmetries such as S 4 , A 4 or A 5 may lead to simple leading-order predictions for the neutrino mixing matrix such as the bimaximal, tribimaximal or golden ratio mixing patterns, which may be brought into agreement with experimental data with the help of corrections from the charged-lepton sector. Such scenarios generally lead to relations among the parameters of the physical leptonic mixing matrix known as solar lepton mixing sum rules. In this article, we present a simple derivation of such solar sum rules, valid for arbitrary neutrino and charged lepton mixing angles and phases, assuming only θ ν 13 = θ e 13 = 0. We discuss four leading-order neutrino mixing matrices with θ ν 13 = 0 which are well motivated from family symmetry considerations. We then perform a phenomenological analysis of the scope to test the resulting four solar sum rules, highlighting the complementarity between next-generation neutrino oscillation experiments such as the reactor experiment JUNO and a superbeam experiment.

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“…ref. [61] for a discussion in case of Cabibbo-like charged-lepton correction to BM mixing and charged-lepton corrections to TBM in ref. [62].…”

Section: Renormalisation Group Correctionsmentioning

confidence: 99%

Testing solar lepton mixing sum rules in neutrino oscillation experiments

Ballett

King

Luhn

et al. 2014

J. High Energ. Phys.

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“…As a possible symmetry between quarks and leptons, quarklepton complementarity relations, such as y 111,112 . Radiative corrections to these relations have been calculated in the type-I seesaw model 113 .…”

Section: Phenomenological Implicationsmentioning

confidence: 99%

Renormalization group running of neutrino parameters

Ohlsson

Zhou

2014

Nat Commun

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Neutrinos are the most elusive particles in our Universe. They have masses at least one million times smaller than the electron mass, carry no electric charge and very weakly interact with other particles, meaning that they are rarely captured in terrestrial detectors. Tremendous efforts in the past two decades have revealed that neutrinos can transform from one type to another as a consequence of neutrino oscillations-a quantum mechanical effect over macroscopic distances-yet the origin of neutrino masses remains puzzling. The physical evolution of neutrino parameters with respect to energy scale may help elucidate the mechanism for their mass generation.E ver since their discovery in the 1950s (ref. 1), neutrinos have continued to surprise us. In the Standard Model (SM) of elementary particle physics, neutrinos are massless particles. However, since the results from the Super-Kamiokande experiment in 1998 (ref. 2), the phenomenon of neutrino oscillations has been well established, indicating that neutrinos do have nonzero and non-degenerate masses and that they can convert from one flavour to another 3 . This important result was followed by a boom of results from several international collaborations. Certainly, these results have pinned down the values of the various neutrino parameters to an incredible precision, especially considering that neutrinos are extremely elusive particles and the corresponding experiments are extraordinarily complex 4 . Currently operating experiments and future investigations under construction are aimed at determining the missing neutrino parameters, such as the CP-violating phase (which can be important for understanding the matter-antimatter asymmetry in the Universe), the sign of the large mass-squared difference for neutrinos, and the absolute neutrino mass scale. In addition, the cubic kilometre scale neutrino telescope at the South Pole, IceCube 5 , has been successfully constructed to search for ultra-high energy astrophysical neutrinos, while a number of underground experiments are looking for neutrinoless double-beta decay (see refs 6-10) and others are waiting for neutrino bursts from galactic supernova explosions (see refs 11,12).However, the origin of neutrino masses and lepton flavour mixing remains a mystery, and calls for new physics beyond the SM. It is believed that new physics should appear somewhere above the electroweak scale (that is, L EW B10 2 GeV) but below the Planck scale (that is, L P B10 19 GeV) for the following reasons. First, the smallness of neutrino masses can be ascribed to the existence of superheavy particles, whose masses are close to the grand unified theory (GUT) scale (for example, L GUT B10 16 GeV), such as right-handed neutrinos in the canonical seesaw models [13][14][15][16][17] . Moreover, the out-of-equilibrium and CP-violating decays of

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“…These effects can have interesting consequences such as the generation of large mixing angles [33,34,35,36,37,38], small mass splittings for degenerate neutrinos [39,40,41,42,43,44,45,46,47], or radiative generation of θ 13 starting from a zero value at the high scale [48,49,50,51]. RG induced deviations from various high scale symmetries like tri-bimaximal mixing scenario [52,53,54] or quark-lepton complimentarity [54,55,56,57] and correlations with low scale observables have been explored. Such effects can have significant contributions from the threshold corrections [58,59,60].…”

Section: Introductionmentioning

confidence: 99%

Renormalization group evolution of neutrino masses and mixing in the Type-III seesaw mechanism

et al. 2009

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We consider the standard model extended by heavy right handed fermions transforming as triplets under SU(2) L , which generate neutrino masses through the Type-III seesaw mechanism.At energies below their respective mass scales, the heavy fields get sequentially decoupled to give an effective dimension-5 operator. Above their mass thresholds, these fields also participate in the renormalization of the wavefunctions, masses and coupling constants. We compute the renormalization group evolution of the effective neutrino mass matrix in this model, with particular emphasis on the threshold effects. The evolution equations are obtained in a basis of neutrino parameters where all the quantities are well-defined everywhere, including at θ 13 = 0. We also point out the important role of the threshold effects and Majorana phases in the evolution of mixing angles through illustrative examples.

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Quark lepton complementarity and renormalization group effects

Cited by 56 publications

References 83 publications

Testing solar lepton mixing sum rules in neutrino oscillation experiments

Testing solar lepton mixing sum rules in neutrino oscillation experiments

Renormalization group running of neutrino parameters

Renormalization group evolution of neutrino masses and mixing in the Type-III seesaw mechanism

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