Matter-enhanced antineutrino flavor transformation and supernova nucleosynthesis

Yong-Zhong Qian; George M. Fuller

doi:10.1103/PhysRevD.52.656

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Matter-enhanced antineutrino flavor transformation and supernova nucleosynthesis

Yong-Zhong Qian

George M. Fuller

Institute for Nuclear Theory, NK-12, University of Washington, Seattle, Washington 98195

Department of Physics, University of California, San Diego, La Jolla, California 92093-0319

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Phys. Rev. D 52, 656 – Published 15 July, 1995

DOI: https://doi.org/10.1103/PhysRevD.52.656

Abstract

Matter-enhanced antineutrino flavor transformation between ν $¯_{e}$ and ν $¯_{μ (τ)}$ can occur in supernovas if the vacuum masses for these species satisfy $m_{ν ¯ e}$ > $m_{ν ¯ μ (τ)}$ . For δ $m^{2}$ >1 ${eV}^{2}$ , such flavor transformation can affect the electron fraction $Y_{e}$ in the neutrino-heated supernova ejecta. We point out that such flavor transformations will not drive $Y_{e}$ >0.5 at the r-process nucleosynthesis epoch in the best available supernova model for such nucleosynthesis. Consequently, there is no obvious conflict between the matter-enhanced antineutrino flavor transformation ν $¯_{e ∥}$ ν $¯_{μ (τ)}$ and r-process nucleosynthesis in the neutrino-heated supernova ejecta.

References (8)

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).
Y. Z. Qian and G. M. Fuller, Phys. Rev. D 51, 1479 (1995).
Y. Z. Qian, Ph.D. thesis, University of California, San Diego, 1993.
S. E. Woosley, J. R. Wilson, G. J. Mathews, R. D. Hoffman and B. S. Meyer, Astrophys. J. 433, 229 (1994).
Ch. Weinheimer et al., Phys. Lett. B 300, 210 (1993).
The most recent work on the cold plus hot dark matter cosmological model which utilizes a specific scheme of neutrino masses is J. R. Primack, J. Holtzman, A. Klypin and D. O. Caldwell, Phys. Rev. Lett. 74, 2160 (1995). Although their specific scheme of $m_{ν_{μ}}$ approx $m_{ν_{τ}}$ approx 2.4 eV is motivated by both experimental and theoretical considerations, the cosmological part of their results does not depend on which neutrino flavors have the specified mass. Discussions involving schemes having one, two, or three massive neutrino flavors in the cold plus hot dark matter model can be found in D. Pogosyan and A. Starobinsky, Astrophys. J. (to be published) and G. M. Fuller, J. R. Primack, and Y. Z. Qian, this issue, Phys. Rev. D 52, 1288 (1995). For implications of neutrino masses from the cold plus hot dark matter model, see also the recent work of C. P. Ma and E. Bertschinger, Astrophys. J. 434, L5 (1994).
L. Wolfenstein, Phys. Rev. D 17, 2369 (1978); ibid. 20, 2364 (1979); S. P. Mikheyev and A. Yu. Smirnov, Nuovo Cimento Soc. Ital. Fis. 9C, 17 (1986); H. A. Bethe, Phys. Rev. Lett. 56, 1305 (1986).
T. J. Loredo and D. Q. Lamb, in Proceedings of the 14th Texas Symposium on Relativistic Astrophysics, Dallas, Texas, 1988, edited by E. Fenyves [Ann. N.Y. Acad. Sci. 571, (1989)].

[c1] 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).

[c2] Y. Z. Qian and G. M. Fuller, Phys. Rev. D 51, 1479 (1995).

[c3] Y. Z. Qian, Ph.D. thesis, University of California, San Diego, 1993.

[c4] S. E. Woosley, J. R. Wilson, G. J. Mathews, R. D. Hoffman and B. S. Meyer, Astrophys. J. 433, 229 (1994).

[c5] Ch. Weinheimer et al., Phys. Lett. B 300, 210 (1993).

[c6] The most recent work on the cold plus hot dark matter cosmological model which utilizes a specific scheme of neutrino masses is J. R. Primack, J. Holtzman, A. Klypin and D. O. Caldwell, Phys. Rev. Lett. 74, 2160 (1995). Although their specific scheme of $m_{ν_{μ}}$ approx $m_{ν_{τ}}$ approx 2.4 eV is motivated by both experimental and theoretical considerations, the cosmological part of their results does not depend on which neutrino flavors have the specified mass. Discussions involving schemes having one, two, or three massive neutrino flavors in the cold plus hot dark matter model can be found in D. Pogosyan and A. Starobinsky, Astrophys. J. (to be published) and G. M. Fuller, J. R. Primack, and Y. Z. Qian, this issue, Phys. Rev. D 52, 1288 (1995). For implications of neutrino masses from the cold plus hot dark matter model, see also the recent work of C. P. Ma and E. Bertschinger, Astrophys. J. 434, L5 (1994).

[c7] L. Wolfenstein, Phys. Rev. D 17, 2369 (1978); ibid. 20, 2364 (1979); S. P. Mikheyev and A. Yu. Smirnov, Nuovo Cimento Soc. Ital. Fis. 9C, 17 (1986); H. A. Bethe, Phys. Rev. Lett. 56, 1305 (1986).

[c8] T. J. Loredo and D. Q. Lamb, in Proceedings of the 14th Texas Symposium on Relativistic Astrophysics, Dallas, Texas, 1988, edited by E. Fenyves [Ann. N.Y. Acad. Sci. 571, (1989)].

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Matter-enhanced antineutrino flavor transformation and supernova nucleosynthesis

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