[Formula presented] violation versus the matter effect in long-baseline neutrino oscillation experiments

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 57, Issue 7, 1998, Pages 4403-4417

  Nunokawa, Hiroshi ^b,c  

^a TOKYO METROPOLITAN UNIVERSITY   (Japan)

^b UNIVERSITY OF VALENCIA   (Spain)

^c UNIVERSITY OF CAMPINAS   (Brazil)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0001402615     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.57.4403     Document Type: Article

References (53)

1. B. T. Cleveland, in Neutrino 94, Proceedings of the 16th International Conference on Neutrino Physics and Astrophysics, Eilat, Israel, edited by A. Dar et al. [Nucl. Phys. B (Proc. Suppl.) 38, 47 (1995)];
2. Y. Suzuki, 38, 54 (1995);
3. P. Anselmann, Phys. Lett. B 285, 376 (1992);
4. Phys. Lett. BP. Anselmann314, 445 (1993);
5. Phys. Lett. BP. Anselmann327, 377 (1994);
6. Phys. Lett. BP. Anselmann342, 440 (1995);J. N. Abdurashitov et al., in Neutrinos 94, p. 60.
7. K. S. Hirata, Phys. Lett. B 205, 416 (1988);
8. Phys. Lett. BK. S. Hirata280, 146 (1992);
9. Phys. Lett. BY. Fukuda, 335, 237 (1994);
10. R. Becker-Szendy, Phys. Rev. D 46, 3720 (1992);
11. W. W. M. Allison, Phys. Lett. B 391, 491 (1997).
12. N. Cabbibo, Phys. Rev. Lett. 10, 531 (1963);
13. M. Kobayashi and T. Maskawa, Prog. Theor. Phys. 49, 652 (1973).
14. M. Fukugita and T. Yanagida, Phys. Lett. B 174, 45 (1986).
15. N. Cabbibo, Phys. Lett. 72B, 333 (1978).
16. V. Barger, K. Wisnant, and R. J. N. Phillips, Phys. Rev. Lett. 45, 2084 (1980).
17. S. Pakvasa, in High Energy Physics, edited by L. Durand and L. G. Pondrom, AIP Conf. Proc. 68 (AIP, New York, 1981), Vol. 2, p. 1164.
18. S. M. Bilenky, J. Hosek, and S. T. Petcov, Phys. Lett. 94B, 495 (1980).
19. C. Jarlskog, Phys. Rev. Lett. 55, 1039 (1985).
20. K. Nishikawa et al., Proposal for a Long Baseline Neutrino Oscillation Experiment using KEK-PS and Super-Kamiokande, 1995.
21. MINOS Collaboration, MINOS Experiment R&D Plan: FY 1996–1998, 1996.
22. ICARUS Collaboration, ICARUS II, A Second-Generation Proton Decay Experiment and Neutrino Observatory at the Gran Sasso Laboratory, 1993.
23. M. Tanimoto, Phys. Rev. D 55, 322 (1997);
24. M. TanimotoProg. Theor. Phys. 97, 901 (1997).
25. J. Arafune and J. Sato, Phys. Rev. D 55, 1653 (1997).
26. L. Wolfenstein, Phys. Rev. D 17, 2369 (1978).
27. T. K. Kuo and J. Pantaleone, Phys. Lett. B 198, 406 (1987);
28. Phys. Lett. BP. I. Krastev and S. T. Petcov, 205, 84 (1988).
29. M. Aglietta, Europhys. Lett. 8, 611 (1989);
30. K. Daum, Z. Phys. C 66, 417 (1995).
31. J. A. Holtzman, Astrophys. J., Suppl. Ser. 71, 1 (1989);
32. J. A. Holtzman and J. R. Primack, Astrophys. J. 405, 428 (1993);
33. J. R. Primack, J. Holtzman, A. Klypin, and D. O. Caldwell, Phys. Rev. Lett. 74, 2160 (1995);
34. K. S. Babu, R. K. Schaefer, and Q. Shafi, Phys. Rev. D 53, 606 (1996);
35. D. Pogosyan and A. Starobinsky, astro-ph/9502019.
36. H. Minakata, Phys. Rev. D 52, 6630 (1995);
37. H. MinakataPhys. Lett. B 356, 61 (1995);
38. Phys. Lett. BS. M. Bilenky, A. Bottino, C. Giunti, and C. W. Kim, 356, 273 (1995);
39. G. L. Fogli, E. Lisi, and G. Scioscia, Phys. Rev. D 52, 5334 (1995).
40. LSND Collaboration, C. Athanassopoulos, Phys. Rev. Lett. 77, 3082 (1996);
41. C. AthanassopoulosPhys. Rev. C 54, 2685 (1996);
42. C. Athanassopoulosnucl-ex/9706006.
43. See also, J. E. Hill, Phys. Rev. Lett. 75, 2654 (1995).
44. A. Acker and S. Pakvasa, Phys. Lett. B 397, 209 (1997).
45. D. Ayres, presented at the 4th KEK Topical Conference on Flavor Physics, Tsukuba, Japan, 1996.
46. For a review, see, e.g., M. White and D. Scott, Comments. Astrophys. 18, 289 (1966).
47. M. Gell-Mann, P. Ramond, and R. Slansky, in Supergravity, Proceedings of the Workshop, Stony Brook, New York, 1979, edited by P. van Nieuwenhuizen and D. Freedman (North-Holland, Amsterdam, 1979), p. 315.
48. F. D. Stacey, Physics of the Earth, 2nd ed. (Wiley, New York, 1977).
49. We note that the mass spectrum (A-1) or (B-2) in Fig. 22 could be in conflict with successful heavy elements nucleosynthesis in supernova. The resonant conversion between (Formula presented) and (Formula presented) (or (Formula presented) would be very adiabatic, possibly except for very small mixing angles, just above the neutrino sphere if (Formula presented) a few eV(Formula presented). On the other hand, for the spectrum (A-2) or (B-1) the conversion between (Formula presented) and (Formula presented) (or (Formula presented) would again be very adiabatic and the nucleosynthesis could be enhanced. See Y.-Z. Qian, Phys. Rev. Lett. 71, 1965 (1993);
50. Y.-Z. Qian and G. M. Fuller, Phys. Rev. D 52, 656 (1995).
51. H. W. Zaglauer and K. H. Schwarzer, Z. Phys. C 40, 273 (1988). We note a typographical error in Eq. (50) in this paper; In the first term of the numerator in Eq. (50) (Formula presented) should be replaced by (Formula presented)
52. H. Minakata and H. Nunokawa, Phys. Lett. B (to be published), hep-ph/9706281.
53. J. Arafune, M. Koike, and J. Sato, Phys. Rev. D 56, 3093 (1997).