Comparing and contrasting the νμ→ντ and νμ→νs solutions to the atmospheric neutrino problem with SuperKamiokande data

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 58, Issue 1, 1998, Pages 130061-130069

  Foot, R ^a   Volkas, R R ^a   Yasuda, O ^b  

^a UNIVERSITY OF MELBOURNE   (Australia)

^b TOKYO METROPOLITAN UNIVERSITY   (Japan)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0542373876     PISSN: 05562821     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevD.58.013006     Document Type: Article

References (74)

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23. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
24. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
25. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
26. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
27. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
28. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
29. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
30. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
31. s solution for big bang nucleosynthesis for the case of maximal mixing are studied in R. Foot and R. R. Volkas, Phys. Rev. D 55, 5147 (1997); Astropart. Phys. 7, 283 (1997); Phys. Rev. D 56, 6653 (1997). For other models with large angle or maximal active-sterile mixing see, for instance, M. Kobayashi, C. S. Lim, and M. M. Nojiri, Phys. Rev. Lett. 67, 1685 (1991); C. Giunti, C. W. Kim, and U. W. Lee, Phys. Rev. D 46, 3034 (1992); J. Bowes and R. R. Volkas, University of Melbourne Report No. UM-P-97/09.
32. In this paper we focus on 2 flavor oscillations. For 3 flavor analyses of the atmospheric neutrino problem see, for example, O. Yasuda, TMUP-HEL-9706, hep-ph/9706546; S. M. Bilenky, C. Giunti, and C. W. Kim, Astropart. Phys. 4, 241 (1996): G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 55, 4385 (1997); M. Narayan, G. Rajasekaran, and S. Uma Sankar, ibid. 56, 437 (1997); P. H. Harrison, D. Perkins, and W. G. Scott, Phys. Lett. B 396, 186 (1997); 349, 137 (1995).
33. In this paper we focus on 2 flavor oscillations. For 3 flavor analyses of the atmospheric neutrino problem see, for example, O. Yasuda, TMUP-HEL-9706, hep-ph/9706546; S. M. Bilenky, C. Giunti, and C. W. Kim, Astropart. Phys. 4, 241 (1996): G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 55, 4385 (1997); M. Narayan, G. Rajasekaran, and S. Uma Sankar, ibid. 56, 437 (1997); P. H. Harrison, D. Perkins, and W. G. Scott, Phys. Lett. B 396, 186 (1997); 349, 137 (1995).
34. In this paper we focus on 2 flavor oscillations. For 3 flavor analyses of the atmospheric neutrino problem see, for example, O. Yasuda, TMUP-HEL-9706, hep-ph/9706546; S. M. Bilenky, C. Giunti, and C. W. Kim, Astropart. Phys. 4, 241 (1996): G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 55, 4385 (1997); M. Narayan, G. Rajasekaran, and S. Uma Sankar, ibid. 56, 437 (1997); P. H. Harrison, D. Perkins, and W. G. Scott, Phys. Lett. B 396, 186 (1997); 349, 137 (1995).
35. In this paper we focus on 2 flavor oscillations. For 3 flavor analyses of the atmospheric neutrino problem see, for example, O. Yasuda, TMUP-HEL-9706, hep-ph/9706546; S. M. Bilenky, C. Giunti, and C. W. Kim, Astropart. Phys. 4, 241 (1996): G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 55, 4385 (1997); M. Narayan, G. Rajasekaran, and S. Uma Sankar, ibid. 56, 437 (1997); P. H. Harrison, D. Perkins, and W. G. Scott, Phys. Lett. B 396, 186 (1997); 349, 137 (1995).
36. In this paper we focus on 2 flavor oscillations. For 3 flavor analyses of the atmospheric neutrino problem see, for example, O. Yasuda, TMUP-HEL-9706, hep-ph/9706546; S. M. Bilenky, C. Giunti, and C. W. Kim, Astropart. Phys. 4, 241 (1996): G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 55, 4385 (1997); M. Narayan, G. Rajasekaran, and S. Uma Sankar, ibid. 56, 437 (1997); P. H. Harrison, D. Perkins, and W. G. Scott, Phys. Lett. B 396, 186 (1997); 349, 137 (1995).
37. In this paper we focus on 2 flavor oscillations. For 3 flavor analyses of the atmospheric neutrino problem see, for example, O. Yasuda, TMUP-HEL-9706, hep-ph/9706546; S. M. Bilenky, C. Giunti, and C. W. Kim, Astropart. Phys. 4, 241 (1996): G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 55, 4385 (1997); M. Narayan, G. Rajasekaran, and S. Uma Sankar, ibid. 56, 437 (1997); P. H. Harrison, D. Perkins, and W. G. Scott, Phys. Lett. B 396, 186 (1997); 349, 137 (1995).
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52. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
53. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
54. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
55. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
56. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
57. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
58. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
59. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
60. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
61. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
62. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
63. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
64. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
65. L.V. Volkova, Sov. J. Nucl. Phys. 31, 784 (1980); T. K. Gaisser, T. Staney, S. A. Bludman, and H. Lee, Phys. Rev. Lett. 51, 223 (1983); A. Dar, ibid. 51, 227 (1983); K. Mitsui, Y. Minorikawa, and H. Komori, Nuovo Cimento C 9, 995 (1986); E. V. Bugaev and V. A. Naumov, Sov. J. Nucl. Phys. 45, 857 (1987); T. K. Gaisser, T. Stanev, and G. Bar, Phys. Rev. D 38, 85 (1988); A. V. Butkevich, L. G. Dedenko, and I. M. Zheleznykh, Sov. J. Nucl. Phys. 50, 90 (1989); M. Honda, K. Kasahara, K. Hidaka, and S. Midorikawa, Phys. Lett. B 248, 193 (1990); H. Lee and Y.S. Koh, Nuovo Cimento B 105, 883 (1990); M. Kawasaki and S. Mizuta, Phys. Rev. D 43, 2900 (1991); P. Lipari, Astropart. Phys. 1, 195 (1993); D. H. Perkins, ibid. 2, 249 (1994); V. Agrawal, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 53, 1314 (1996); T. K. Gaisser and T. Stanev, ibid. 57, 1977 (1998).
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