Neutrino flavor conversion in a neutrino background: Single- versus multi-particle description

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 68, Issue 1, 2003, Pages

  Friedland, Alexander ^a,b   Lunardini, Cecilia ^b  

^a LOS ALAMOS NATIONAL LABORATORY   (United States)

^b INSTITUTE FOR ADVANCED STUDY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; CALCULATION; COSMOS; ELEMENTARY PARTICLE; ENERGY; NEUTRINO; OSCILLATION; RADIATION SCATTERING;

EID: 0042387918     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.68.013007     Document Type: Article

References (31)

1. A.Y. Smirnov and S.P. Mikheev, in Proceedings of the Sixth Moriond Workshop on Massive Neutrinos in Astrophysics and in Particle Physics, Tignes, France, 1986, pp. 355–372.
2. G.M. Fuller, R.W. Mayle, J.R. Wilson, and D.N. Schramm, Astrophys. J. 322, 795 (1987).
3. D. Notzold and G. Raffelt, Nucl. Phys. B307, 924 (1988).
4. R. Barbieri and A. Dolgov, Phys. Lett. B 237, 440 (1990).
5. M.J. Savage, R.A. Malaney, and G.M. Fuller, Astrophys. J. 368, 1 (1991).
6. R. Barbieri and A. Dolgov, Nucl. Phys. B349, 743 (1991).
7. P. Langacker and J. Liu, Phys. Rev. D 46, 4140 (1992).
8. J. Pantaleone, Phys. Rev. D 46, 510 (1992).
9. J. Pantaleone, Phys. Lett. B 287, 128 (1992).
10. G. Sigl and G. Raffelt, Nucl. Phys. B406, 423 (1993).
11. B.H.J. McKellar and M.J. Thomson, Phys. Rev. D 49, 2710 (1994).
12. V.A. Kostelecky, J. Pantaleone, and S. Samuel, Phys. Lett. B 315, 46 (1993).
13. V.A. Kostelecky and S. Samuel, Phys. Lett. B 318, 127 (1993).
14. V.A. Kostelecky and S. Samuel, Phys. Rev. D 49, 1740 (1994).
15. V.A. Kostelecky and S. Samuel, Phys. Rev. D 52, 3184 (1995).
16. C. Lunardini and A.Y. Smirnov, Phys. Rev. D 64, 073006 (2001).
17. S. Hannestad, Phys. Rev. D 65, 083006 (2002).
18. A.D. Dolgov, Nucl. Phys. B632, 363 (2002).
19. Y.Y.Y. Wong, Phys. Rev. D 66, 025015 (2002).
20. K.N. Abazajian, J.F. Beacom, and N.F. Bell, Phys. Rev. D 66, 013008 (2002).
21. J. Pantaleone, Phys. Lett. B 342, 250 (1995).
22. Y.Z. Qian and G.M. Fuller, Phys. Rev. D 51, 1479 (1995).
23. G. Sigl, Phys. Rev. D 51, 4035 (1995).
24. G.C. McLaughlin, J.M. Fetter, A.B. Balantekin, and G.M. Fuller, Phys. Rev. C 59, 2873 (1999).
25. S. Pastor and G. Raffelt, Phys. Rev. Lett. 89, 191101 (2002).
26. S. Samuel, Phys. Rev. D 48, 1462 (1993).
27. S. Samuel, Phys. Rev. D 53, 5382 (1996).
28. J. Pantaleone, Phys. Rev. D 58, 073002 (1998).
29. S. Pastor, G. Raffelt, and D.V. Semikoz, Phys. Rev. D 65, 053011 (2002).
30. For physical applications, both in the case of the early Universe and supernova, the relevant neutrino energies are in the (Formula presented) range.
31. To avoid conflict with the Pauli’s principle and to make possible labelling of neutrinos by their momenta, we can assume that neutrinos have slightly different energies.