Yoshida Takashi, Kajino Toshitaka, Hartmann Dieter H
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan.
Phys Rev Lett. 2005 Jun 17;94(23):231101. doi: 10.1103/PhysRevLett.94.231101. Epub 2005 Jun 15.
We constrain energy spectra of supernova neutrinos through the avoidance of an overproduction of the 11B abundance during Galactic chemical evolution. In supernova nucleosynthesis calculations with a parametrized neutrino spectrum as a function of temperature of nu(mu,tau) and nu(mu,tau) and total neutrino energy, we find a strong neutrino temperature dependence of the 11B yield. When the yield is combined with observed abundances, the acceptable range of the nu(mu,tau) and nu(mu,tau) temperature is found to be 4.8 to 6.6 MeV. Nonzero neutrino chemical potentials would reduce this temperature range by about 10% for a degeneracy parameter eta(nu) = mu(nu)/kT(nu) smaller than 3.
我们通过避免在银河系化学演化过程中硼 - 11丰度的过度产生来限制超新星中微子的能谱。在将中微子能谱参数化为μ子中微子和τ子中微子温度以及μ子中微子和τ子中微子与总中微子能量函数的超新星核合成计算中，我们发现硼 - 11产率对中微子温度有很强的依赖性。当将该产率与观测到的丰度相结合时，发现μ子中微子和τ子中微子温度的可接受范围为4.8至6.6兆电子伏特。对于简并参数η(ν)=μ(ν)/kT(ν)小于3的情况，非零中微子化学势会使该温度范围降低约10%。
