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Light element synthesis constraining the supernova neutrino spectrum

Published online by Cambridge University Press:  23 December 2005

Takashi Yoshida
Astronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba-ku, Sendai 980-8578, Japan email:
Toshitaka Kajino
National Astronomical Observatory, and The Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan Department of Astronomy, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Dieter H. Hartmann
Department of Physics and Astronomy, Clemson University, Clemson, SC29634, USA
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We constrain energy spectra of supernova neutrinos using the $\nu$-process light element synthesis in supernovae and the $^{11}$B abundance during Galactic chemical evolution. We calculate supernova nucleosynthesis due to the $\nu$-process assuming that neutrino energy spectra are Fermi-Dirac distributions with zero chemical potential. We investigate the dependence of the $^{11}$B yield on the total neutrino energy and the temperature of $\nu_{\mu,\tau}$ and $\bar{\nu}_{\mu,\tau}$. From the obtained yields and the contribution to the $^{11}$B yield from supernovae constrained by observed abundances and Galactic chemical evolution models, we find an acceptable range of the temperature of $\nu_{\mu,\tau}$ and $\bar{\nu}_{\mu,\tau}$ of 4.8 MeV to 6.6 MeV.

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© 2005 International Astronomical Union