Resonant neutrino spin-flavor precession and supernova nucleosynthesis and dynamics

H. Nunokawa; Y.-Z. Qian; G. M. Fuller

doi:10.1103/PhysRevD.55.3265

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Resonant neutrino spin-flavor precession and supernova nucleosynthesis and dynamics

H. Nunokawa, Y.-Z. Qian, and G. M. Fuller

Institute for Nuclear Theory, University of Washington, Box 351550, Seattle, Washington 98195

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Phys. Rev. D 55, 3265 – Published 15 March, 1997

DOI: https://doi.org/10.1103/PhysRevD.55.3265

Abstract

We discuss the effects of resonant spin-flavor precession (RSFP) of Majorana neutrinos on heavy element nucleosynthesis in neutrino-heated supernova ejecta and the dynamics of supernovae. In assessing the effects of RSFP, we explicitly include matter-enhanced (MSW) resonant neutrino flavor conversion effects where appropriate. We point out that for plausible ranges of neutrino magnetic moments and protoneutron star magnetic fields, spin-flavor conversion of $ν_{τ}$ (or $ν_{μ}$ ) with a cosmologically significant mass (1–100 eV) into a light ${\bar{ν}}_{e}$ could lead to an enhanced neutron excess in neutrino-heated supernova ejecta. This could be beneficial for models of $r$ -process nucleosynthesis associated with late-time neutrino-heated ejecta from supernovae. Similar spin-flavor conversion of neutrinos at earlier epochs could lead to an increased shock reheating rate and, concomitantly, a larger supernova explosion energy. We show, however, that such increased neutrino heating likely will be accompanied by an enhanced neutron excess which could exacerbate the problem of the overproduction of the neutron number $N = 50$ nuclei in the supernova ejecta from this stage. In all of these scenarios, the average ${\bar{ν}}_{e}$ energy will be increased over those predicted by supernova models with no neutrino mixings. This may allow the SN 1987A data to constrain RSFP-based schemes.

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[c1] C. S. Lim and W. Marciano, Phys. Rev. D37, 1368 (1988).

[c2] E. Akhmedov, Phys. Lett. B213, 64 (1988); See also, J. Schechter and J. W. F. Valle, Phys. Rev. D24, 1883 (1981); 25, 283 (1982).

[c3] S. P. Mikheyev and A. Yu. Smirnov, Sov. J. Nucl. Phys.42, 913 (1985); L. Wolfenstein, Phys. Rev. D17, 2369 (1978).

[c4] E. Kh. Akhmedov, A. Lanza, S. T. Petcov, and D. W. Sciama, Phys. Rev. D55, 515 (1997).

[c5] E. M. Burbidge, G. R. Burbidge, W. A. Fowler, and F. Hoyle, Rev. Mod. Phys.29, 547 (1957); A. G. W. Cameron, Publ. Astron. Soc. Pac.69, 201 (1957).

[c6] S. E. Woosley and E. Baron, Astrophys. J.391, 228 (1992); S. E. Woosley, Astron. Astrophys. Suppl. Ser.97, 205 (1993).

[c7] S. E. Woosley and R. D. Hoffman, Astrophys. J.395, 202 (1992); B. S. Meyer, G. J. Mathews, W. M. Howard, S. E. Woosley, and R. D. Hoffman, 399, 656 (1992).

[c8] S. E. Woosley, J. R. Wilson, G. J. Mathews, R. D. Hoffman, and B. S. Meyer, Astrophys. J.433, 229 (1994).

[c9] 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).

[c10] B. S. Meyer, Astrophys. J.449, L55 (1995).

[c11] Y.-Z. Qian and S. E. Woosley, Astrophys. J.471, 331 (1996).

[c12] R. D. Hoffman, S. E. Woosley, and Y.-Z. Qian, Astrophys. J. (to be published); B. S. Meyer, L. Luo, and B. Brown, report, 1996 (unpublished).

[c13] G. M. Fuller, Y.-Z. Qian, and J. R. Wilson, in preparation.

[c14] Y.-Z. Qian, Nucl. Phys. A (to be published).

[c15] G. M. Fuller and B. S. Meyer, Astrophys. J.453, 792 (1995).

[c16] R. D. Hoffman, S. E. Woosley, G. M. Fuller, and B. S. Meyer, Astrophys. J.460, 478 (1996).

[c17] A. I. Derbin, A. V. Chernyi, L. A. Popeko, V. N. Muratova, G. A. Shishkina, and S. I. Bakhlanov, JETP Lett.57, 768 (1993).

[c18] G. G. Raffelt, Phys. Rev. Lett.64, 2856 (1990).

[c19] See for example, M. B. Voloshin, Sov. J. Nucl. Phys.48, 512 (1988); K. S. Babu and R. Mohapatra, Phys. Rev. Lett.63, 228 (1988); S. M. Barr, E. M. Freire, and A. Zee, 65, 2626 (1990); D. Chang, W.-Y. Keung, S. Lipovaca, and G. Senjanovic, 67, 953 (1991).

[c20] Y.-Z. Qian and G. M. Fuller, Phys. Rev. D51, 1479 (1995); G. Sigl, 51, 4035 (1995).

[c21] J. R. Wilson and R. W. Mayle (private communication).

[c22] S. J. Parke and T. P. Walker, Phys. Rev. Lett.57, 2322 (1986); W. C. Haxton, Phys. Rev. D36, 2283 (1987).

[c23] E. Kh. Akhmedov and Z. G. Berezhiani, Nucl. Phys.B373, 479 (1992).

[c24] H. A. Bethe and J. R. Wilson, Astrophys. J.263, 386 (1985).

[c25] G. M. Fuller, R. W. Mayle, B. S. Meyer, and J. R. Wilson, Astrophys. J.389, 517 (1992).

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Resonant neutrino spin-flavor precession and supernova nucleosynthesis and dynamics

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