Sterile neutrinos and supernova nucleosynthesis

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 61, Issue 12, 2000, Pages

  Qian, Yong Zhong ^c  

^a UNIVERSITY OF CALIFORNIA   (United States)

^b UNIVERSITY OF CALIFORNIA   (United States)

^c University of Minnesota   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 17144422915     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.61.123005     Document Type: Article

References (77)

1. E. M. Burbidge, G. R. Burbidge, W. A. Fowler, and F. Hoyle, Rev. Mod. Phys. 29, 624 (1957)
2. A. G. W. Cameron, Astron. Soc. Pac. 69, 201 (1957).
3. J. N. Bahcall, Neutrino Astrophysics (Cambridge University Press, Cambridge, England, 1989)
4. for more recent discussions see W. C. Haxton, Annu. Rev. Astron. Astrophys. 33, 459 (1995)
5. J. N. Bahcall, Astrophys. J. 467, 475 (1996)
6. V. Castellani, Phys. Rep. 281, 1 (1997).
7. T. K. Gaiser, F. Halzen, and T. Stanev, Phys. Rep. 258, 173 (1995)
8. Y. Fukuda, Phys. Lett. B 433, 9 (1998)
9. Phys. Lett. BY. Fukuda436, 33 (1998)
10. Y. FukudaPhys. Rev. Lett. 81, 1562 (1998).
11. LSND Collaboration, C. Athanassopoulus, Phys. Rev. Lett. 75, 2650 (1995)
12. C. AthanassopoulusPhys. Rev. C 54, 2685 (1996)
13. C. AthanassopoulusPhys. Rev. Lett. 77, 3082 (1996)
14. Phys. Rev. Lett.C. Athanassopoulus81, 1774 (1998).
15. G. L. Fogli, E. Lisi, D. Montanino, and G. Scioscia, Phys. Rev. D 56, 4365 (1997)
16. G. L. Fogli, E. Lisi, A. Marrone, and G. Scioscia, hep-ph/9906450
17. C. Y. Cardall and G. M. Fuller, Phys. Rev. D 53, 4421 (1996)
18. A. Acker and S. Pakvasa, Phys. Lett. B 397, 209 (1997)
19. E. Ma and P. Roy, Phys. Rev. Lett. 80, 4637 (1998)
20. C. Y. Cardall, G. M. Fuller, and D. Cline, Phys. Lett. B 413, 246 (1997).
21. D. O. Caldwell, in Perspectives in Neutrinos, Atomic Physics and Gravitation, edited by J. Tran Thanh Van et al. (Editions Fronteres, Gif-sur-Yvette, France, 1993)
22. D. O. Caldwell and R. N. Mohapatra, Phys. Rev. D 48, 3259 (1993)
23. D. O. CaldwellR. N. MohapatraPhys. Lett. B 354, 371 (1995)
24. J. T. Peltoniemi and J. W. F. Valle, Nucl. Phys. B406, 409 (1993)
25. G. M. Fuller, J. R. Primack, and Y.-Z. Qian, Phys. Rev. D 52, 1288 (1995).
26. V. Barger, S. Pakvasa, T. J. Weiler, and K. Whisnant, Phys. Rev. D 58, 093016 (1998).
27. Particle Data Group, C. Caso, Eur. Phys. J. C 3, 1 (1998), p. 319.
28. B. S. Meyer, W. M. Howard, G. J. Mathews, S. E. Woosley, and R. D. Hoffman, Astrophys. J. 399, 656 (1992)
29. Astrophys. J.S. E. Woosley, J. R. Wilson, G. J. Mathews, R. D. Hoffman, and B. S. Meyer, 433, 299 (1994)
30. K. Takahashi, J. Witti, and H.-Th. Janka, Astron. Astrophys. 286, 857 (1994).
31. R. D. Hoffman, S. E. Woosley, and Y.-Z. Qian, Astrophys. J. 482, 951 (1996)
32. B. S. Meyer and J. S. Brown, Astrophys. J., Suppl. Ser. 112, 199 (1997).
33. Y.-Z. Qian and S. E. Woosley, Astrophys. J. 471, 331 (1996)
34. G. M. Fuller and Y.-Z. Qian, Nucl. Phys. A606, 167 (1996)
35. C. Y. Cardall and G. M. Fuller, Astrophys. J. Lett. 486, L111 (1997)
36. J. D. Salmonson and J. R. Wilson, Astrophys. J. 517, 859 (1999).
37. G. C. McLaughlin and G. M. Fuller, Astrophys. J. 472, 440 (1996). The neutron deficit problem will obtain for any neutrino-heated ejecta. So to the extent that neutrinos supply the energy for material ejection and set (Formula presented) in the ejecta, our nucleosynthesis considerations would also apply in the multi-dimensional scenarios of Ref. 16.
38. B. S. Meyer, G. C. McLaughlin, and G. M. Fuller, Phys. Rev. C 58, 3696 (1998).
39. W. C. Haxton, K. Langanke, Y.-Z. Qian, and P. Vogel, Phys. Rev. Lett. 78, 2694 (1997)
40. Y.-Z. Qian, W. C. Haxton, K. Langanke, and P. Vogel, Phys. Rev. C 55, 1532 (1997).
41. C. Sneden, A. McWilliam, G. W. Preston, J. J. Cowan, D. L. Burris, and B. J. Armosky, Astrophys. J. 467, 819 (1996)
42. Astrophys. J.C. Sneden, J. J. Cowan, D. L. Burris, and J. W. Truran, 496, 235 (1998);C. Sneden, J. J. Cowan, I. I. Ivans, G. M. Fuller, S. Burles, T. C. Beers, and J. E. Lawler, ibid. (to be published).
43. D. S. Miller, J. R. Wilson, and R. W. Mayle, Astrophys. J. 415, 278 (1993)
44. Astrophys. J.M. Herant, W. Benz, W. R. Hix, C. L. Fryer, and S. A. Colgate, 435, 339 (1994)
45. Astrophys. J.A. Burrows, J. Hayes, and B. A. Fryxell, 450, 830 (1995)
46. H.-T. Janka and E. Müller, Astron. Astrophys. 306, 167 (1996)
47. A. Mezzacappa, A. C. Calder, S. W. Bruenn, J. M. Blondin, M. W. Guidry, M. R. Strayer, and A. S. Umar, Astrophys. J. 495, 911 (1998).
48. A. S. Burrows, presentation at ICAHTLT, Sedona, AZ, August 1999; and (in preparation).
49. Y.-Z. Qian, G. M. Fuller, G. J. Mathews, R. W. Mayle, J. R. Wilson, and S. E. Woosley, Phys. Rev. Lett. 71, 1965 (1993).
50. C. J. Horowitz and G. Li, Phys. Rev. Lett. 82, 5198 (1999).
51. See, for example, A. Burrows and R. F. Sawyer, Phys. Rev. C 58, 554 (1998) for effects of refined neutrino opacities in nuclear matter on neutrino emission in supernovas.
52. G. M. Fuller and B. S. Meyer, Astrophys. J. 453, 792 (1995).
53. J. N. Bahcall, P. Krastev, and A. Yu. Smirnov, Phys. Rev. D 58, 096016 (1998)
54. see also M. C. Gonzalez-Garcia, P. C. de Holanda, C. Peña-Garay, and J. W. F. Valle, hep-ph/9906469. Note that the “just-so” (Formula presented) vacuum mixing solution to the solar neutrino puzzle is currently disfavored. However, this does not affect our discussion as the matter-enhanced (Formula presented) mixing solution works adequately in our scheme of evading the alpha effect for supernova r-process nucleosynthesis.
55. G. C. McLaughlin and J. N. Ng, Phys. Lett. B 464, 232 (1999).
56. J. R. Primack, J. Holtzman, A. Klypin, and D. O. Caldwell, Phys. Rev. Lett. 74, 2160 (1995).
57. S. M. Bilenky, G. Giunti, and W. Grimus, Eur. Phys. J. C 1, 247 (1998).
58. X. Shi, D. N. Schramm, and B. Fields, Phys. Rev. D 48, 2563 (1993). It should be noted, however, that the whole issue of the (Formula presented)He yield in BBN in the presence of matter-enhanced active-sterile neutrino transformations is controversial. See, e.g.
59. Phys. Rev. DX. Shi, 54, 2753 (1996)
60. X. Shi and G. M. Fuller, Phys. Rev. Lett. 833120 (1999)
61. X. Shi, G. M. Fuller, and K. Abazajian, Phys. Rev. D 60, 063002 (1999)
62. Phys. Rev. DR. Foot and D. Volkas, 56, 6653 (1997).
63. S. P. Mikheyev and A. Yu. Smirnov, Yad. Fiz. 42, 1441 (1985) [Sov. J. Nucl. Phys. 42, 913 (1985)]
64. L. Wolfenstein, Phys. Rev. D 17, 2369 (1978).
65. J. T. Peltoniemi hep-ph/9511323 has suggested that this scheme of neutrino transformation could circumvent the r-process constraints of Ref. 18 on neutrino mixing, and could possibly lower (Formula presented) Along these lines
66. H. Nunokawa, J. T. Peltoniemi, A. Rossi, and J. Valle, Phys. Rev. D 56, 1704 (1997), suggested that (Formula presented) and (Formula presented) transformation would cause (Formula presented) to reach the fixed point at (Formula presented). However, this will not occur in a rapid outflow (see Ref. 33). In addition, the simultaneous occurrence of (Formula presented) and (Formula presented) transformation envisioned by Nunokawa et al. could not circumvent the alpha effect discussed in the present work as their scenario would leave a significant (Formula presented) flux in the region where this effect would occur.
67. G. M. Fuller, R. W. Mayle, B. S. Meyer, and J. R. Wilson, Astrophys. J. 389, 517 (1992).
68. Y.-Z. Qian and G. M. Fuller, Phys. Rev. D 49, 1762 (1996).
69. A. Mezzacappa and S. W. Bruenn, in Proceedings of Future Directions of Supernova Research: Progenitors to Remnants, Memoirs of the Italian Astronomical Society; A. Mezzacappa and S. W. Bruenn, in Proceedings of the Second International Workshop on the Identification of Dark Matter (World Scientific, Singapore, in press).
70. H. Nunokawa, Y.-Z. Qian, and G. M. Fuller, Phys. Rev. D 55, 3265 (1997)
71. E. Akhmedov, Phys. Lett. B 213, 64 (1988)
72. E. Akhmedov, A. Lanza, S. T. Petcov, and D. W. Sciama, Phys. Rev. D 55, 515 (1997)
73. E. Akhmedov and Z. G. Berezhiani, Nucl. Phys. B373, 479 (1992).
74. G. C. McLaughlin, J. Fetter, A. B. Balantekin, and G. M. Fuller, Phys. Rev. C 59, 2873 (1999).
75. X. Shi, G. M. Fuller, and K. Abazajian, astro-ph/9908081.
76. R. D. Hoffman, S. E. Woosley, G. M. Fuller, and B. S. Meyer, Astrophys. J. 460, 478 (1996).
77. See, for example, J. T. Peltoniemi, D. Tommasini, and J. W. F. Valle, Phys. Lett. B 298, 383 (1993).See also Fuller et al. in Ref. 6 for discussions in connection with supernova r-process nucleosynthesis.