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We present a proposal of an experiment for search for cosmic background neutrino decay. Due to the mass difference between neutrino generations, a heavier neutrino can decay into a lighter neutrino with a photon. Standard model predicts the neutrino lifetime is 1043 year, while the current experimental lower limit of neutrino lifetime is 3 × 1012 year. However, left-right symmetric model suggests much shorter neutrino lifetime down to 1017 year in the shortest. If we assume a mass of the heaviest neutrino is 50 meV, the expected photon energy at the neutrino rest frame is 25 meV. The energy spectrum of the photon from the cosmic background neutrino decay has a cutoff at this energy and a low energy tail due to a red shift effect. Thus we propose an experiment to search for the photon emission from the decay of cosmic background neutrino by measuring the continuous photon energy spectrum in the far infrared wavelength region. We plan to perform a rocket experiment with a superconducting tunnel junction (STJ) detector in 2016 in the earliest, aiming at improving the neutrino lifetime limit by two orders of magnitude. We aim at a 10-hour satellite experiment with 5σ sensitivity for the neutrino lifetime of 1017 year.
References
- 1) J.Beringer et al. Particle Data Group), Phys. Rev. D 86, 010001 (2012). 10.1103/PhysRevD.86.010001 Google Scholar
- 2) V. N.Aseev, A. I.Belesev, A. I.Berlev, E. V.Geraskin, A. A.Golubev, N. A.Likhovid, V. M.Lobashev, A. A.Nozik, V. S.Pantuev, V. I.Parfenov, A. K.Skasyrskaya, F. V.Tkachov, and S. V.Zadorozhny, Phys. Rev. D 84, 112003 (2011). 10.1103/PhysRevD.84.112003 Google Scholar
- 3) M.Moresco, L.Verde, L.Pozzetti, R.Jimenez, and A.Cimatti, J. Cosmology Astropar. Phys. 2012, 053 (2012). 10.1088/1475-7516/2012/07/053 Google Scholar
- 4) G.Drexlin, V.Hannen, S.Mertens, and C.Weinheimer, Adv. High Energy Phys. 2013, 293986 (2013). 10.1155/2013/293986 Google Scholar
- 5) P. A. R.Ade et al. Planck Collaboration), arXiv:1303.5076.Google Scholar
- 6) A. R.Taylor SKA Collaboration), Proc. IAU Symp., 2012, p. 291.Google Scholar
- 7) T.Ishida et al. T2K Collaboration), a talk at KEK seminar on July (2013) p. 19.Google Scholar
- 8) P. B.Pal and L.Wolfenstein, Phys. Rev. D 25, 766 (1982). 10.1103/PhysRevD.25.766 Google Scholar
- 9) K.Sato and M.Kobayashi, Prog. Theor. Phys. 58, 1775 (1977). 10.1143/PTP.58.1775 Google Scholar
- 10) R. E.Shrock, Nucl. Phys. B 206, 359 (1982). 10.1016/0550-3213(82)90273-5 Google Scholar
- 11) M. A. B.Bég, W. J.Marciano, and M.Ruderman, Phys. Rev. D 17, 1395 (1978). 10.1103/PhysRevD.17.1395 Google Scholar
- 12) A.Mirizzi, D.Montanino, and P. D.Serpico, Phys. Rev. D 76, 053007 (2007). 10.1103/PhysRevD.76.053007 Google Scholar
- 13) S.-H.Kim, K.Takemasa, Y.Takeuchi, and S.Matsuura, J. Phys. Soc. Jpn. 81, 024101 (2012). 10.1143/JPSJ.81.024101[Abstract] Google Scholar
- 14) M. G.Hauser, R. G.Arendt, T.Kelsall, E.Dwek, N.Odegard, J. L.Weiland, H. T.Freudenreich, W. T.Reach, R. F.Silverberg, S. H.Moseley, Y. C.Pei, P.Lubin, J. C.Mather, R. A.Shafer, G. F.Smoot, R.Weiss, D. T.Wilkinson, and E. L.Wright, Astrophys. J. 508, 25 (1998). 10.1086/306379 Google Scholar
- 15) D. P.Finkbeiner, M.Davis, and D. J.Schlegel, Astrophys. J. 544, 81 (2000). 10.1086/317177 Google Scholar
- 16) T.Wada, H.Nagata, H.Ikeda, Y.Arai, M.Ohno, and K.Nagase, J. Low Temp. Phys. 167, 602 (2012). 10.1007/s10909-012-0461-6 Google Scholar
- 17) S.-H.Kim, H.-S.Jeong, K.Kiuchi, S.Kanai, T.Onjo, K.Takemasa, Y.Takeuchi, H.Ikeda, S.Matsuura, H.Sato, M.Hazumi, and S.-B.Kim, Phys. Proc. 37, 667 (2012) (Proceedings of TIPP2011). 10.1016/j.phpro.2012.02.415 Google Scholar