Published September 1, 2009 | Version v1
Journal article

Large |Ue3| and tribimaximal mixing

  • 1. Physical Research Laboratory, Ahmedabad 380 009 (India)
  • 2. SISSA and INFN Sezione di Trieste, Via Beirut 2-4, I-34014 Trieste (Italy) and Institute for the Physics of Mathematics of the Universe, 5-1-5 Kashiwa-no-Ha, Kashiwa Shi, Chiba 277-8568 (Japan)
  • 3. Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005 (India)
  • 4. Max-Planck-Institut fuer Kernphysik, Postfach 103980, D-69029 Heidelberg (Germany)

Description

We investigate in a model-independent way to what extent one can perturb tribimaximal mixing in order to generate a sizable value of |Ue3|, while at the same time keeping solar neutrino mixing near its measured value, which is close to sin2θ12=(1/3). Three straightforward breaking mechanisms to generate |Ue3|≅0.1 are considered. For charged lepton corrections, the suppression of a sizable contribution to sin2θ12 can be achieved if CP violation in neutrino oscillations is almost maximal. Generation of the indicated value of |Ue3|≅0.1 through renormalization group corrections requires the neutrinos to be quasidegenerate in mass. The consistency with the allowed range of sin2θ12 together with large running of |Ue3| forces one of the Majorana phases to be close to π. This implies large cancellations in the effective Majorana mass governing neutrinoless double beta ((ββ)0ν) decay, constraining it to lie near its minimum allowed value of m0cos2θ12, where m0 > or approx. 0.1 eV. Finally, explicit breaking of the neutrino mass matrix in the inverted hierarchical and quasidegenerate neutrino mass spectrum cases is similarly correlated with the (ββ)0ν-decay effective Majorana mass, although to a lesser extent. The implied values for the atmospheric neutrino mixing angle θ23 are given in all cases.

Additional details

Publishing Information

Journal Title
Physical Review. D, Particles Fields
Journal Volume
80
Journal Issue
5
Journal Page Range
p. 053013-053013.14
ISSN
0556-2821
CODEN
PRVDAQ

Optional Information

Notes
(c) 2009 The American Physical Society