The exact parity symmetric model and big bang nucleosynthesis

Astroparticle Physics

Volumn 7, Issue 3, 1997, Pages 283-295

  Foot, R ^a   Volkas, R R ^a  

^a UNIVERSITY OF MELBOURNE   (Australia)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0031206373     PISSN: 09276505     EISSN: None     Source Type: Journal    
DOI: 10.1016/S0927-6505(97)00028-5     Document Type: Article

References (55)

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4. 2) was earlier proposed in the papers: R. Foot, H. Lew and R. R. Volkas, Mod. Phys. Lett. A7 (1992) 2567; R. Foot, Mod. Phys. Lett. A9 (1994) 169.
5. 2) was earlier proposed in the papers: R. Foot, H. Lew and R. R. Volkas, Mod. Phys. Lett. A7 (1992) 2567; R. Foot, Mod. Phys. Lett. A9 (1994) 169.
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24. [12] Note that in addition to ordinary-mirror neutrino mass mixing, the mirror world can interact with the ordinary particles through photon-minor photon mixing (discussed by B. Holdom, Phys. Lett. B 166 (1985) 196; S.L. Glashow, Phys. Lett. B 167 (1985) 35; E. Carlson and S. L. Giashow, Phys. Lett. B 193 (1986) 168; and independently in a slightly different way by R. Foot, H. Lew and R.R. Volkas, Phys. Lett. B 272 (1991) 67), and Higgs-boson-mirror-Higgs-boson mixing (discussed in the previous paper and in H. Lew (unpublished)). We assume that these interactions are either zero or small enough so as to preserve the dominance of matter over mirror matter.
25. [12] Note that in addition to ordinary-mirror neutrino mass mixing, the mirror world can interact with the ordinary particles through photon-minor photon mixing (discussed by B. Holdom, Phys. Lett. B 166 (1985) 196; S.L. Glashow, Phys. Lett. B 167 (1985) 35; E. Carlson and S. L. Giashow, Phys. Lett. B 193 (1986) 168; and independently in a slightly different way by R. Foot, H. Lew and R.R. Volkas, Phys. Lett. B 272 (1991) 67), and Higgs-boson-mirror-Higgs-boson mixing (discussed in the previous paper and in H. Lew (unpublished)). We assume that these interactions are either zero or small enough so as to preserve the dominance of matter over mirror matter.
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36. [17] R. Foot and R.R. Volkas, Phys. Rev. D 55 (1997) 5147.
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38. [19] The propagation of neutrinos in matter was first studied by: L. Wolfenstein, Phys. Rev. D 17 (1978) 2369; D 20 ( 1979) 2634; S.P. Mikheyev and A. Yu. Smirnov, Nuovo Cim. C9 (1986) 17. See also, V. Barger et al., Phys. Rev. D 22 (1980) 2718. For reviews, see e.g. T.K. Kuo and J. Pantaleone, Rev. Mod. Phys. 61 (1989) 937; G. Gelmini and E. Roulet, Rept. Prog. Phys. 58 (1995) 1207.
39. [19] The propagation of neutrinos in matter was first studied by: L. Wolfenstein, Phys. Rev. D 17 (1978) 2369; D 20 ( 1979) 2634; S.P. Mikheyev and A. Yu. Smirnov, Nuovo Cim. C9 (1986) 17. See also, V. Barger et al., Phys. Rev. D 22 (1980) 2718. For reviews, see e.g. T.K. Kuo and J. Pantaleone, Rev. Mod. Phys. 61 (1989) 937; G. Gelmini and E. Roulet, Rept. Prog. Phys. 58 (1995) 1207.
40. [19] The propagation of neutrinos in matter was first studied by: L. Wolfenstein, Phys. Rev. D 17 (1978) 2369; D 20 ( 1979) 2634; S.P. Mikheyev and A. Yu. Smirnov, Nuovo Cim. C9 (1986) 17. See also, V. Barger et al., Phys. Rev. D 22 (1980) 2718. For reviews, see e.g. T.K. Kuo and J. Pantaleone, Rev. Mod. Phys. 61 (1989) 937; G. Gelmini and E. Roulet, Rept. Prog. Phys. 58 (1995) 1207.
41. [19] The propagation of neutrinos in matter was first studied by: L. Wolfenstein, Phys. Rev. D 17 (1978) 2369; D 20 ( 1979) 2634; S.P. Mikheyev and A. Yu. Smirnov, Nuovo Cim. C9 (1986) 17. See also, V. Barger et al., Phys. Rev. D 22 (1980) 2718. For reviews, see e.g. T.K. Kuo and J. Pantaleone, Rev. Mod. Phys. 61 (1989) 937; G. Gelmini and E. Roulet, Rept. Prog. Phys. 58 (1995) 1207.
42. [19] The propagation of neutrinos in matter was first studied by: L. Wolfenstein, Phys. Rev. D 17 (1978) 2369; D 20 ( 1979) 2634; S.P. Mikheyev and A. Yu. Smirnov, Nuovo Cim. C9 (1986) 17. See also, V. Barger et al., Phys. Rev. D 22 (1980) 2718. For reviews, see e.g. T.K. Kuo and J. Pantaleone, Rev. Mod. Phys. 61 (1989) 937; G. Gelmini and E. Roulet, Rept. Prog. Phys. 58 (1995) 1207.
43. [19] The propagation of neutrinos in matter was first studied by: L. Wolfenstein, Phys. Rev. D 17 (1978) 2369; D 20 ( 1979) 2634; S.P. Mikheyev and A. Yu. Smirnov, Nuovo Cim. C9 (1986) 17. See also, V. Barger et al., Phys. Rev. D 22 (1980) 2718. For reviews, see e.g. T.K. Kuo and J. Pantaleone, Rev. Mod. Phys. 61 (1989) 937; G. Gelmini and E. Roulet, Rept. Prog. Phys. 58 (1995) 1207.
44. [20] K. Enqvist et al., in [13].
45. eff ≲ 3.9, 4.5, 4.0 have been respectively obtained by: C.J. Copi, D.N. Schramm and M.S. Turner, Phys. Rev. Lett. 75 (1995) 3981; P.J. Kernan and S. Sarkar, Phys. Rev. D 54 (1996) 3681; K.A. Olive and D. Thomas, University of Minnesota Preprint UMN-TH-1515/96, hep-ph/9610319.
46. eff ≲ 3.9, 4.5, 4.0 have been respectively obtained by: C.J. Copi, D.N. Schramm and M.S. Turner, Phys. Rev. Lett. 75 (1995) 3981; P.J. Kernan and S. Sarkar, Phys. Rev. D 54 (1996) 3681; K.A. Olive and D. Thomas, University of Minnesota Preprint UMN-TH-1515/96, hep-ph/9610319.
47. eff ≲ 3.9, 4.5, 4.0 have been respectively obtained by: C.J. Copi, D.N. Schramm and M.S. Turner, Phys. Rev. Lett. 75 (1995) 3981; P.J. Kernan and S. Sarkar, Phys. Rev. D 54 (1996) 3681; K.A. Olive and D. Thomas, University of Minnesota Preprint UMN-TH-1515/96, hep-ph/9610319.
48. eff ≲ 3.9, 4.5, 4.0 have been respectively obtained by: C.J. Copi, D.N. Schramm and M.S. Turner, Phys. Rev. Lett. 75 (1995) 3981; P.J. Kernan and S. Sarkar, Phys. Rev. D 54 (1996) 3681; K.A. Olive and D. Thomas, University of Minnesota Preprint UMN-TH-1515/96, hep-ph/9610319.
49. p.
50. v′β can be obtained by replacing T → T′ in the above equation.
51. 2, including the effects of the neutrino asymmetry and momentum distribution.
52. αβ′).
53. -5) by performing a more accurate study using the density matrix equations (including the neutrino momentum distribution).
54. 2.
55. 2 (as suggested by the atmospheric neutrino anomaly).