Cosmologically Interesting Neutrinos and Heavy Element Nucleosynthesis in Supernovae

Details Cosmologically Interesting Neutrinos and Heavy Element Nucleosynthesis in Supernovae Cosmologically Interesting Neutrinos and Heavy Element Nucleosynthesis in Supernovae

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.8907q&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #89.07; Bulletin of the American Astronomical Society, Vol. 24, p.1264

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We show that the heavy element nucleosynthesis from the ``hot-bubble'' in the late evolution of a supernova is sensitive to neutrino flavor mixing. In particular, a nu_ μ or nu_ τ with a mass in the range of 1--100 eV (coincidentally the mass range of interest for neutrino dark matter) would have a mass-level-crossing with nu_e above the neutrino-sphere and below the region where nucleosynthesis takes place. Significant conversion between nu_e and nu_ τ (or nu_ μ) will drive the material in this region proton-rich and thus precludes any r-process nucleosynthesis of heavy elements. We show that this occurs whenever the vacuum mixing angle between nu_e and nu_ τ (or nu_ μ) satisfies sin (22theta >) 10(-6) --10(-4) depending on the nu_ τ (or nu_ μ) mass. If the ``hot-bubble'' is the site of r-process nucleosynthesis, then these results place severe constraints on neutrino dark matter. If, on the other hand, nu_ μ or nu_ τ are ever shown to have masses and mixing angles in the relevant range, then we conclude that the r-process must come from another site. We show that our results are independent of the uncertain details of supernova explosion physics. This work is supported by NSF grant PHY--9121623.

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