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Neutrino phenomenology of very low-energy seesaw scenarios

André de Gouvêa, James Jenkins, and Nirmala Vasudevan

  • Northwestern University, Department of Physics & Astronomy, 2145 Sheridan Road, Evanston, Illinois 60208, USA

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Phys. Rev. D 75, 013003 – Published 9 January, 2007

DOI: https://doi.org/10.1103/PhysRevD.75.013003

Abstract

The standard model augmented by the presence of gauge-singlet right-handed neutrinos proves to be an ideal scenario for accommodating nonzero neutrino masses. Among the new parameters of this “new standard model” are right-handed neutrino Majorana masses M. Theoretical prejudice points to M much larger than the electroweak symmetry breaking scale, but it has recently been emphasized that all M values are technically natural and should be explored. Indeed, M around 1–10  eV can accommodate an elegant oscillation solution to the liquid scintillator neutrino detector (LSND) anomaly, while other M values lead to several observable consequences. We consider the phenomenology of low-energy (M≲1  keV) seesaw scenarios. By exploring such a framework with three right-handed neutrinos, we can consistently fit all oscillation data—including those from LSND—while partially addressing several astrophysical puzzles, including anomalous pulsar kicks, heavy element nucleosynthesis in supernovae, and the existence of warm dark matter. In order to accomplish all of this, we find that a nonstandard cosmological scenario is required. Finally, low-energy seesaws—regardless of their relation to the LSND anomaly—can also be tested by future tritium beta-decay experiments, neutrinoless double-beta decay searches, and other observables. We estimate the sensitivity of such probes to M.

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References (70)

  1. A. Strumia and F. Vissani, hep-ph/0606054; R. N. Mohapatra and A. Yu. Smirnov, hep-ph/0603118; R. N. Mohapatra et al., hep-ph/0510213; A. de Gouvêa, hep-ph/0411274; Mod. Phys. Lett. A 19, 2799 (2004).
  2. P. Minkowiski, Phys. Lett. 67B, 421 (1977); M. Gell-Mann, P. Ramond, and R. Slansky, in Supergravity, edited by D. Freedman and P. Van Niuenhuizen (North Holland, Amsterdam, 1979), p. 315; T. Yanagida, in Proceedings of the Workshop on Unified Theory and Baryon Number in the Universe, edited by O. Sawada and A. Sugamoto (KEK, Tsukuba, Japan, 1979); S. L. Glashow, 1979 Cargèse Lectures in Physics—Quarks and Leptons, edited by M. Lévy (Plenum, New York, 1980), p. 707; R. N. Mohapatra and G. Senjanović, Phys. Rev. Lett. 44, 912 (1980).
  3. A. de Gouvêa, Phys. Rev. D 72, 033005 (2005).
  4. A. Aguilar et al. (LSND Collaboration), Phys. Rev. D 64, 112007 (2001).
  5. A. Bazarko (MiniBooNE Collaboration), Nucl. Phys. B, Proc. Suppl. 91, 210 (2001).
  6. W. Krolikowski, Acta Phys. Pol. B 35, 2241 (2004).
  7. T. Asaka, S. Blanchet, and M. Shaposhnikov, Phys. Lett. B 631, 151 (2005).
  8. T. Asaka, A. Kusenko, and M. Shaposhnikov, Phys. Lett. B 638, 401 (2006).
  9. J. A. Casas and A. Ibarra, Nucl. Phys. B618, 171 (2001).
  10. M. Maltoni, T. Schwetz, M. A. Tortola, and J. W. F. Valle, New J. Phys. 6, 122 (2004).
  11. W.-M. Yao et al. (Particle Data Group), J. Phys. G 33, 1 (2006).
  12. A. Strumia, Phys. Lett. B 539, 91 (2002).
  13. M. Maltoni, T. Schwetz, M. A. Tortola, and J. W. F. Valle, Nucl. Phys. B643, 321 (2002).
  14. M. Maltoni, T. Schwetz, M. A. Tortola, and J. W. F. Valle, hep-ph/0305312.
  15. M. Sorel, J. M. Conrad, and M. Shaevitz, Phys. Rev. D 70, 073004 (2004).
  16. H. Murayama and T. Yanagida, Phys. Lett. B 520, 263 (2001); G. Barenboim, L. Borissov, J. D. Lykken, and A. Yu. Smirnov, J. High Energy Phys. 10 (2002) 001; M. C. Gonzalez-Garcia, M. Maltoni, and T. Schwetz, Phys. Rev. D 68, 053007 (2003).
  17. V. A. Kostelecky and M. Mewes, Phys. Rev. D 70, 076002 (2004); 69, 016005 (2004); L. B. Auerbach et al. (LSND Collaboration), 72, 076004 (2005); A. de Gouvêa and Y. Grossman, 74, 093008 (2006); T. Katori, A. Kostelecky, and R. Tayloe, 74, 105009 (2006).
  18. G. Barenboim and N. E. Mavromatos, J. High Energy Phys. 01 (2005) 034.
  19. S. Palomares-Ruiz, S. Pascoli, and T. Schwetz, J. High Energy Phys. 09 (2005) 048.
  20. M. Sorel (private communication).
  21. S. Avvakumov et al., Phys. Rev. Lett. 89, 011804 (2002).
  22. P. Astier et al. (NOMAD Collaboration), Phys. Lett. B 570, 19 (2003).
  23. E. Eskut et al. (CHORUS Collaboration), Phys. Lett. B 434, 205 (1998); 424, 202 (1998).
  24. D. N. Spergel et al., astro-ph/0603449.
  25. U. Seljak, A. Slosar, and P. McDonald, J. Cosmol. Astropart. Phys. 10 (2006) 014.
  26. S. Hannestad and G. G. Raffelt, J. Cosmol. Astropart. Phys. 11 (2006) 016.
  27. G. L. Fogli et al., hep-ph/0608060.
  28. M. Cirelli and A. Strumia, astro-ph/0607086.
  29. K. Enqvist, K. Kainulainen, and M. J. Thomson, Nucl. Phys. B373, 498 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
  30. A. Yu. Smirnov and R. Z. Funchal, Phys. Rev. D 74, 013001 (2006).
  31. S. Dodelson, A. Melchiorri, and A. Slosar, Phys. Rev. Lett. 97, 041301 (2006).
  32. See, for example, J. F. Beacom, N. F. Bell, and S. Dodelson, Phys. Rev. Lett. 93, 121302 (2004).
  33. See, for example, V. Barger, J. P. Kneller, H. S. Lee, D. Marfatia, and G. Steigman, Phys. Lett. B 566, 8 (2003).
  34. K. Abazajian, N. F. Bell, G. M. Fuller, and Y. Y. Y. Wong, Phys. Rev. D 72, 063004 (2005).
  35. G. Gelmini, S. Palomares-Ruiz, and S. Pascoli, Phys. Rev. Lett. 93, 081302 (2004).
  36. For a recent analysis, see Y. Z. Chu and M. Cirelli, Phys. Rev. D 74, 085015 (2006).
  37. For very recent discussions, see K. Abazajian, Phys. Rev. D 73, 063513 (2006); U. Seljak, A. Makarov, P. McDonald, and H. Trac, Phys. Rev. Lett. 97, 191303 (2006); K. Abazajian and S. M. Koushiappas, Phys. Rev. D 74, 023527 (2006); M. Viel, J. Lesgourgues, M. G. Haehnelt, S. Matarrese, and A. Riotto, Phys. Rev. Lett. 97, 071301 (2006).
  38. K. Abazajian, G. M. Fuller, and W. H. Tucker, Astrophys. J. 562, 593 (2001). Recent discussions can be found in K. Abazajian and S. M. Koushiappas in [37]; C. R. Watson, J. F. Beacom, H. Yuksel, and T. P. Walker, Phys. Rev. D 74, 033009 (2006).
  39. A. Kusenko, astro-ph/0608096.
  40. M. Cirelli, G. Marandella, A. Strumia, F. Vissaniand , Nucl. Phys. B708, 215 (2005).
  41. M. Sorel and J. M. Conrad, Phys. Rev. D 66, 033009 (2002).
  42. K. Kainulainen, J. Maalampi, and J. T. Peltoniemi, Nucl. Phys. B358, 435 (1991).
  43. H. A. Bethe, Rev. Mod. Phys. 62, 801 (1990).
  44. Z. Arzoumanian, D. F. Chernoffs, and J. M. Cordes, Astrophys. J. 568, 289 (2002).
  45. L. Scheck, T. Plewa, H. T. Janka, K. Kifonidis, and E. Mueller, Phys. Rev. Lett. 92, 011103 (2004); L. Scheck, K. Kifonidis, H. T. Janka, and E. Mueller, astro-ph/0601302.
  46. M. B. Voloshin, Phys. Lett. B 209, 360 (1988).
  47. A. de Gouvêa and J. Jenkins, Phys. Rev. D 74, 033004 (2006).
  48. Z. Daraktchieva et al. (MUNU Collaboration), Phys. Lett. B 615, 153 (2005).
  49. H. B. Li et al. (TEXONO Collaboration), Phys. Rev. Lett. 90, 131802 (2003).
  50. A. Kusenko and G. Segre, Phys. Rev. Lett. 77, 4872 (1996).
  51. A. Kusenko, Int. J. Mod. Phys. D 13, 2065 (2004).
  52. M. Barkovich, J. C. D’Olivo, and R. Montemayor, hep-ph/0503113.
  53. H. Nunokawa, V. B. Semikoz, A. Yu. Smirnov, and J. W. F. Valle, Nucl. Phys. B501, 17 (1997).
  54. S. Esposito and G. Capone, Z. Phys. C 70, 55 (1996).
  55. G. M. Fuller, A. Kusenko, I. Mocioiu, and S. Pascoli, Phys. Rev. D 68, 103002 (2003).
  56. K. Abazajian, G. M. Fuller, and M. Patel, Phys. Rev. D 64, 023501 (2001).
  57. S. Wanajo, T. Kajino, G. J. Mathews, and K. Otsuki, astro-ph/0102261.
  58. G. C. McLaughlin, J. M. Fetter, A. B. Balantekin, and G. M. Fuller, Phys. Rev. C 59, 2873 (1999).
  59. J. Fetter, G. C. McLaughlin, A. B. Balantekin, and G. M. Fuller, Astropart. Phys. 18, 433 (2003).
  60. J. Beun, G. C. McLaughlin, R. Surman, and W. R. Hix, Phys. Rev. D 73, 093007 (2006).
  61. Y. Farzan and A. Yu. Smirnov, Phys. Lett. B 557, 224 (2003).
  62. C. Kraus et al., Eur. Phys. J. C 40, 447 (2005).
  63. V. M. Lobashev et al., Nucl. Phys. B, Proc. Suppl. 91, 280 (2001).
  64. A. Osipowicz et al. (KATRIN Collaboration), hep-ex/0109033.
  65. Y. Farzan, O. L. G. Peres, and A. Yu. Smirnov, Nucl. Phys. B612, 59 (2001).
  66. S. R. Elliott and P. Vogel, Annu. Rev. Nucl. Part. Sci. 52, 115 (2002); F. T. Avignone, Nucl. Phys. B, Proc. Suppl. 143, 233 (2005).
  67. B. Kayser, Phys. Rev. D 30, 1023 (1984).
  68. A. M. Bakalyarov, A. Y. Balysh, S. T. Belyaev, V. I. Lebedev, and S. V. Zhukov (C03-06-23.1 Collaboration), Pisma Fiz. Elem. Chast. Atom. Yadra 2, 21 (2005) [C03-06-23.1 CollaborationPhys. Part. Nucl. Lett. 2, 77 (2005)].
  69. For a recent review, see W. Buchmuller, R. D. Peccei, and T. Yanagida, Annu. Rev. Nucl. Part. Sci. 55, 311 (2005).
  70. M. Shaposhnikov and I. Tkachev, Phys. Lett. B 639, 414 (2006).

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Phys. Rev. D 75, 013003– Published 9 January, 2007
  • Received 18 August 2006

© 2007 American Physical Society

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