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-based seesaw model for realistic neutrino masses and mixing
Phys. Rev. D 93, 033007 – Published 16 February, 2016
DOI: https://doi.org/10.1103/PhysRevD.93.033007
Abstract
We present an -based model where neutrino masses arise from a combination of seesaw mechanisms. The model is motivated by several small mixing and mass parameters indicated by the data. These are , the solar mass splitting, and the small deviation of from maximal mixing (). We take the above as indications that at some level the small quantities are well approximated by zero. In particular, the mixing angles to zeroth order should be either 0 or . Accordingly, in this model the type-II seesaw dominates and generates the larger atmospheric mass splitting and sets . The other mixing angles are vanishing as is the solar splitting. We show how the assignment for the lepton doublets leads to this form. We also specify the properties of the right-handed neutrinos which result in a smaller type-I seesaw contribution that acts as a perturbation and shifts the angles and into the correct range and the desired value of is produced. The symmetry results in relationships between these quantities as well as with a small deviation of from . If the right-handed neutrino mass matrix is chosen real then there is no leptonic violation and only normal ordering is admissible. If is complex then inverted ordering is also allowed with the proviso that the phase is large, i.e., or . The preliminary results from favoring normal ordering and near imply quasidegenerate neutrino masses in this model.
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References (23)
- For the present status of see presentations from Double Chooz, RENO, Daya Bay, , and T2K at Neutrino 2014, https://indico.fnal.gov/conferenceOtherViews.py?view=standard&confId=8022.
- B. Brahmachari and A. Raychaudhuri, Phys. Rev. D 86, 051302 (2012); S. Pramanick and A. Raychaudhuri, 88, 093009 (2013).
- S. Pramanick and A. Raychaudhuri, Phys. Lett. B 746, 237 (2015); Int. J. Mod. Phys. A 30, 1530036 (2015).
- F. Vissani, J. High Energy Phys. 11 (1998) 025. Models with somewhat similar points of view as those espoused here are E. K. Akhmedov, Phys. Lett. B 467, 95 (1999); M. Lindner and W. Rodejohann, J. High Energy Phys. 05 (2007) 089.
- For other recent work after the determination of , see S. Antusch, S. F. King, C. Luhn, and M. Spinrath, Nucl. Phys. B856, 328 (2012); B. Adhikary, A. Ghosal, and P. Roy, Int. J. Mod. Phys. A 28, 1350118 (2013); D. Aristizabal Sierra, I. de Medeiros Varzielas, and E. Houet, Phys. Rev. D 87, 093009 (2013); R. Dutta, U. Ch, A. K. Giri, and N. Sahu, Int. J. Mod. Phys. A 29, 1450113 (2014); L. J. Hall and G. G. Ross, J. High Energy Phys. 11 (2013) 091; T. Araki, Prog. Theor. Exp. Phys. 2013, 103B02 (2013); A. E. Carcamo Hernandez, I. de Medeiros Varzielas, S. G. Kovalenko, H. Päs, and I. Schmidt, Phys. Rev. D 88, 076014 (2013); M.-C. Chen, J. Huang, K. T. Mahanthappa, and A. M. Wijangco, J. High Energy Phys. 10 (2013) 112; B. Brahmachari and P. Roy, 02 (2015) 135.
- For a review see, for example, S. F. King and C. Luhn, Rep. Prog. Phys. 76, 056201 (2013).
- P. Minkowski, Phys. Lett. 67B, 421 (1977); M. Gell-Mann, P. Ramond, and R. Slansky, in Supergravity, edited by F. van Nieuwenhuizen and D. Freedman (North-Holland, Amsterdam, 1979), p. 315; T. Yanagida, in Proceedings of the Workshop on Unified Theory and the Baryon Number of the Universe (KEK, Japan, 1979); S. L. Glashow, NATO Sci. Ser. B 59, 687 (1980); R. N. Mohapatra and G. Senjanović, Phys. Rev. D 23, 165 (1981).
- E. Ma and G. Rajasekaran, Phys. Rev. D 64, 113012 (2001).
- G. Altarelli and F. Feruglio, Nucl. Phys. B741, 215 (2006); H. Ishimori, T. Kobayashi, H. Ohki, Y. Shimizu, H. Okada, and M. Tanimoto, Prog. Theor. Phys. Suppl. 183, 1 (2010).
- For a sampling see, for example, F. Bazzocchi, S. Morisi, and M. Picariello, Phys. Lett. B 659, 628 (2008); E. Ma, Phys. Rev. D 73, 057304 (2006); P. Ciafaloni, M. Picariello, E. Torrente-Lujan, and A. Urbano, 79, 116010 (2009).
- E. Ma and D. Wegman, Phys. Rev. Lett. 107, 061803 (2011); S. Gupta, A. S. Joshipura, and K. M. Patel, Phys. Rev. D 85, 031903 (2012); G. C. Branco, R. G. Felipe, F. R. Joaquim, and H. Serodio, 86, 076008 (2012); B. Adhikary, B. Brahmachari, A. Ghosal, E. Ma, and M. K. Parida, Phys. Lett. B 638, 345 (2006); B. Karmakar and A. Sil, Phys. Rev. D 91, 013004 (2015); E. Ma, Phys. Lett. B 752, 198 (2016).
- S. K. Kang and M. Tanimoto, Phys. Rev. D 91, 073010 (2015).
- J. Barry and W. Rodejohann, Phys. Rev. D 81, 093002 (2010); J. Barry, W. Rodejohann, and H. Zhang, J. High Energy Phys. 07 (2011) 091; A. Adulpravitchai and R. Takahashi, 09 (2011) 127.
- R. Gonzalez Felipe, H. Serodio, and J. P. Silva, Phys. Rev. D 87, 055010 (2013).
- S. F. King and M. Malinsky, Phys. Lett. B 645, 351 (2007); E. Ma, H. Sawanaka, and M. Tanimoto, 641, 301 (2006); S. Morisi, M. Nebot, K. M. Patel, E. Peinado, and J. W. F. Valle, Phys. Rev. D 88, 036001 (2013); S. Morisi, E. Peinado, Y. Shimizu, and J. W. F. Valle, 84, 036003 (2011).
- M. C. Gonzalez-Garcia, M. Maltoni, J. Salvado, and T. Schwetz, J. High Energy Phys. 12 (2012) 123.
- D. V. Forero, M. Tortola, and J. W. F. Valle, Phys. Rev. D 86, 073012 (2012).
- C. Bronner (for the T2K Collaboration), in Proceedings of the International Conference on Massive Neutrinos, Nanyang Technological University, Singapore, February, 2015 (to be published).
- M. Haag (KATRIN Collaboration), Proc. Sci., EPS-HEP2013 (2013) 518.
- R. Patterson (for the Collaboration), Joint Experimental and Theoretical Seminar, Fermilab, August 6, 2015.
- See, for example, G. Drexlin, V. Hannen, S. Mertens, and C. Weinheimer, Adv. High Energy Phys. 2013, 293986 (2013).
- A. Degee, I. P. Ivanov, and V. Keus, J. High Energy Phys. 02 (2013) 125.
- R. Gonzalez Felipe, H. Serodio, and J. P. Silva, Phys. Rev. D 88, 015015 (2013).