Comparison of νμ↔ντ and νμ↔νs oscillations as solutions of the atmospheric neutrino problem

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 58, Issue 7, 1998, Pages

  Lipari, Paolo ^a   Lusignoli, Maurizio ^a  

^a UNIVERSITÀ DI ROMA LA SAPIENZA   (Italy)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0542418301     PISSN: 05562821     EISSN: None     Source Type: Journal    
DOI: None     Document Type: Review

References (65)

1. K. S. Hirata et al., Phys. Lett. B 205, 416 (1988); 280, 146 (1992); Y. Fukuda et al., ibid. 335, 237 (1994); D. Casper et al., Phys. Rev. Lett. 66, 2561 (1991); R. Becker-Szendy et al., Phys. Rev. D 46, 3720 (1992); Soudan-2 Collaboration, T. Kafka, Proceedings of TAUP97; Super-Kamiokande Collaboration, Y. Fukuda et al., hep-ex/9803006.
2. K. S. Hirata et al., Phys. Lett. B 205, 416 (1988); 280, 146 (1992); Y. Fukuda et al., ibid. 335, 237 (1994); D. Casper et al., Phys. Rev. Lett. 66, 2561 (1991); R. Becker-Szendy et al., Phys. Rev. D 46, 3720 (1992); Soudan-2 Collaboration, T. Kafka, Proceedings of TAUP97; Super-Kamiokande Collaboration, Y. Fukuda et al., hep-ex/9803006.
3. K. S. Hirata et al., Phys. Lett. B 205, 416 (1988); 280, 146 (1992); Y. Fukuda et al., ibid. 335, 237 (1994); D. Casper et al., Phys. Rev. Lett. 66, 2561 (1991); R. Becker-Szendy et al., Phys. Rev. D 46, 3720 (1992); Soudan-2 Collaboration, T. Kafka, Proceedings of TAUP97; Super-Kamiokande Collaboration, Y. Fukuda et al., hep-ex/9803006.
4. K. S. Hirata et al., Phys. Lett. B 205, 416 (1988); 280, 146 (1992); Y. Fukuda et al., ibid. 335, 237 (1994); D. Casper et al., Phys. Rev. Lett. 66, 2561 (1991); R. Becker-Szendy et al., Phys. Rev. D 46, 3720 (1992); Soudan-2 Collaboration, T. Kafka, Proceedings of TAUP97; Super-Kamiokande Collaboration, Y. Fukuda et al., hep-ex/9803006.
5. K. S. Hirata et al., Phys. Lett. B 205, 416 (1988); 280, 146 (1992); Y. Fukuda et al., ibid. 335, 237 (1994); D. Casper et al., Phys. Rev. Lett. 66, 2561 (1991); R. Becker-Szendy et al., Phys. Rev. D 46, 3720 (1992); Soudan-2 Collaboration, T. Kafka, Proceedings of TAUP97; Super-Kamiokande Collaboration, Y. Fukuda et al., hep-ex/9803006.
6. K. S. Hirata et al., Phys. Lett. B 205, 416 (1988); 280, 146 (1992); Y. Fukuda et al., ibid. 335, 237 (1994); D. Casper et al., Phys. Rev. Lett. 66, 2561 (1991); R. Becker-Szendy et al., Phys. Rev. D 46, 3720 (1992); Soudan-2 Collaboration, T. Kafka, Proceedings of TAUP97; Super-Kamiokande Collaboration, Y. Fukuda et al., hep-ex/9803006.
7. E. Kearns, Proceedings of TAUP97, hep-ex/9803007.
8. See, for example, V. Berezinsky, Invited Lecture at 25th ICRC, Durban, 1997, astro-ph/9710126.
9. LSND Collaboration, C. Athanassopoulos et al., Phys. Rev. Lett. 77, 3082 (1996); nucl-ex/9706006; nucl-ex/9709006.
10. e in this case, a positive signal for the CHOOZ experiment [9]; therefore both scenarios are currently not supported by the data.
11. C. Y. Cardall and G. M. Fuller, Phys. Rev. D 53, 4421 (1996).
12. G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 56, 4365 (1997).
13. A. Acker and S. Pakvasa, Phys. Lett. B 397, 209 (1997).
14. CHOOZ Collaboration, M. Apollonio et al., Phys. Lett. B 420, 397 (1998).
15. ν=2.995±0.061, see LEP Electroweak Working Group, CERN/PPE/95-172.
16. M. C. Gonzalez-Garcia, H. Nunokawa, O. L. G. Peres, T. Stanev, and J. W. F. Valle, Phys. Rev. D 58, 033004 (1998).
17. R. Foot, R. R. Volkas, and O. Yasuda, hep-ph/9802287.
18. E. Akhmedov, B. Lipari, and M. Lusignoli, Phys. Lett. B 300, 128 (1993).
19. R. Foot, Mod. Phys. Lett. A 9, 169 (1994); R. Foot and R. R. Volkas, Phys. Rev. D 52, 6595 (1995); S. M. Bilenky, C. Giunti, and W. Grimus, in Neutrino 96, Proceedings of the conference, Helsinki, 1996, edited by K. Enqvist et al. (World Scientific, Singapore, 1997), p. 174.
20. R. Foot, Mod. Phys. Lett. A 9, 169 (1994); R. Foot and R. R. Volkas, Phys. Rev. D 52, 6595 (1995); S. M. Bilenky, C. Giunti, and W. Grimus, in Neutrino 96, Proceedings of the conference, Helsinki, 1996, edited by K. Enqvist et al. (World Scientific, Singapore, 1997), p. 174.
21. R. Foot, Mod. Phys. Lett. A 9, 169 (1994); R. Foot and R. R. Volkas, Phys. Rev. D 52, 6595 (1995); S. M. Bilenky, C. Giunti, and W. Grimus, in Neutrino 96, Proceedings of the conference, Helsinki, 1996, edited by K. Enqvist et al. (World Scientific, Singapore, 1997), p. 174.
22. F. Vissani and A. Yu. Smirnov, hep-ph/9710565.
23. Q. Y. Liu and A. Yu. Smirnov, hep-ph/9712493.
24. R. Foot, R. R. Volkas, and O. Yasuda, Phys. Rev. D 58, 013006 (1998).
25. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
26. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
27. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
28. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
29. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
30. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
31. A. Dolgov, Sov. J. Nucl. Phys. 33, 700 (1981); R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990); Nucl. Phys. B349, 743 (1991); K. Enqvist, K. Kainulainen, and M. Thomson, Phys. Rev. Lett. 68, 744 (1992); Nucl. Phys. B373, 498 (1992); J. Cline, Phys. Rev. Lett. 68, 3137 (1992); X. Shi, D. N. Schramm, and B. D. Fields, Phys. Rev. D 48, 2563 (1993).
32. D. Schramm and M. Turner, Rev. Mod. Phys. 70, 303 (1998).
33. R. Foot and R. Volkas, Phys. Rev. D 55, 5147 (1997); 56, 6653 (1997).
34. R. Foot and R. Volkas, Phys. Rev. D 55, 5147 (1997); 56, 6653 (1997).
35. S. J. Barish et al. Phys. Rev. D 19, 2521 (1979).
36. G. L. Fogli and G. Nardulli, Nucl. Phys. B160, 116 (1979).
37. L. Wolfenstein, Phys. Rev. D 17, 2369 (1978); S. P. Mikheyev and A. Yu. Smirnov, Yad. Fiz. 42, 1441 (1985) [Sov. J. Nucl. Phys. 42, 913 (1985)].
38. L. Wolfenstein, Phys. Rev. D 17, 2369 (1978); S. P. Mikheyev and A. Yu. Smirnov, Yad. Fiz. 42, 1441 (1985) [Sov. J. Nucl. Phys. 42, 913 (1985)].
39. L. Wolfenstein, Phys. Rev. D 17, 2369 (1978); S. P. Mikheyev and A. Yu. Smirnov, Yad. Fiz. 42, 1441 (1985) [Sov. J. Nucl. Phys. 42, 913 (1985)].
40. s mixing, can be understood [16] as a case of "parametric resonance" [25].
41. E. Akhmedov, Yad. Fiz. 47, 475 (1988); P. I. Krastev and A. Y. Smirnov, Phys. Lett. B 226, 341 (1989).
42. E. Akhmedov, Yad. Fiz. 47, 475 (1988); P. I. Krastev and A. Y. Smirnov, Phys. Lett. B 226, 341 (1989).
43. F. D. Stacey, Physics of the Earth (Wiley, New York, 1969).
44. z.
45. s transitions, if studied in great detail shows a complex dependence on the zenith angle that can be compared with the oscillation probability curves in Fig. 3.
46. T. K. Gaisser, M. Honda, K. Kasahara, H. Lee, S. Midorikawa, V. Naumov, and T. Stanev, Phys. Rev. D 54, 5578 (1996).
47. Y. Fukuda et al., Phys. Lett. B 335, 237 (1994).
48. 2<0 is somewhat larger than in the other case, because of the MSW resonance present for the neutrinos.
49. V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996).
50. P. Lipari, M. Lusignoli, and F. Sartogo, Phys. Rev. Lett. 74, 4384 (1995).
51. T. K. Gaisser and Todor Stanev, Phys. Rev. D 57, 1977 (1998).
52. -2. In the upper hemisphere this condition is satisfied at most in a small solid angle for the deepest detectors.
53. P. Lipari and M. Lusignoli, Phys. Rev. D 57, R3842 (1998).
54. W. Lohmann, R. Kopp, and R. Voss, CERN Yellow Report No. EP/85-03.
55. Baksan Collaboration, M. M. Boliev et al., ICRC '95, Rome, Vol. 1, pp. 686 and 722.
56. MACRO Collaboration, S. Ahlen et al., Phys. Lett. B 357, 481 (1995); F. Ronga et al., in Neutrino '96 [14].
57. MACRO Collaboration, S. Ahlen et al., Phys. Lett. B 357, 481 (1995); F. Ronga et al., in Neutrino '96 [14].
58. Kamiokande Collaboration, A. Suzuki et al., in Proceedings of 7th International Workshop on Neutrino Telescopes, Venice, 1996, edited by M. Baldo Ceolin, p. 263.
59. IMB Collaboration, R. Becker-Szendy et al., Phys. Rev. Lett. 69, 1010 (1992); D. W. Casper, in Proceedings of 3rd International Workshop on Neutrino Telescopes, Venice, 1991, edited by M. Baldo Ceolin, p. 213.
60. IMB Collaboration, R. Becker-Szendy et al., Phys. Rev. Lett. 69, 1010 (1992); D. W. Casper, in Proceedings of 3rd International Workshop on Neutrino Telescopes, Venice, 1991, edited by M. Baldo Ceolin, p. 213.
61. M. Honda, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 52, 4985 (1995).
62. M. Gluck, E. Reya, and A. Vogt, Z. Phys. C 67, 433 (1995).
63. W. Frati, T. K. Gaisser, A. K. Mann, and T. Stanev, Phys. Rev. D 48, 1140 (1993).
64. The acceptance for the muon flux increases with the area (as opposed to the volume) of the detector: SK does not dominate the other experiments as for the contained neutrino events.
65. G. L. Fogli, E. Lisi, and A. Marrone, Phys. Rev. D 57, 5893 (1998).