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| Decoupling of Neutrinos and the |
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| Neutrino
Barrier |
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| • | Abundance
ratio of neutrons to protons |
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| “freezes out”
when neutrino interactions |
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| can no longer
maintain equilibrium |
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| abundances
(timescale > age of |
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| universe) – e
and p interactions |
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| contribute to
neutrino “opacity”: |
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