UHE中微子天文学和中微子振荡
UHE neutrino astronomy and neutrino oscillations
摘要：
$E>10^{17}$ eV的UHE中微子可以由超高能宇宙射线（UHECR）与CMB光子（宇宙成因中微子）相互作用产生，也可以由拓扑缺陷（TD）、超重暗物质（SHDM）和镜像物质等自上而下的源产生。宇宙成因中微子的预测是可靠的，它们的流量可以用数值计算UHECR的观测流量。的通量的下限得到的情况下，纯质子组成的观察到的UHECR。宇宙成因中微子流量的严格上限也是存在的。中微子的最大能量由最大加速能量决定，至少对于冲击波加速来说，最大加速能量预计不会超过$10^{21} - 10^{22}$ eV。自上而下的来源提供了高出几个数量级的中微子能量，这可以被认为是这些模型的特征。振荡在UHE中微子天文学中起着重要的作用。在宇宙成因中微子的产生过程中，$τ$ -中微子不存在，而$\barν_e$中微子被抑制。这些物种，重要的检测，出现在所观察到的通量由于振荡。镜像中微子不能被直接观测到，但由于普通中微子的振荡，它们可以在最高能量下提供最大的中微子通量。
英文摘要：
UHE neutrinos with $E>10^{17}$ eV can be produced by ultra-high energy cosmic rays (UHECR) interacting with CMB photons (cosmogenic neutrinos) and by top-down sources, such as topological defects (TD), superheavy dark matter (SHDM) and mirror matter. Cosmogenic neutrinos are reliably predicted and their fluxes can be numerically evaluated using the observed flux of UHECR. The lower limit for the flux is obtained for the case of pure proton composition of the observed UHECR. The rigorous upper limit for cosmogenic neutrino flux also exists. The maximum neutrino energy is determined by maximum energy of acceleration, which at least for the shock acceleration is expected not to exceed $10^{21} - 10^{22}$ eV. The top-down sources provide neutrino energies a few orders of magnitude higher, and this can be considered as a signature of these models. Oscillations play important role in UHE neutrino astronomy. At production of cosmogenic neutrinos $τ$-neutrinos are absent and $\barν_e$ neutrinos are suppressed. These species, important for detection, appear in the observed fluxes due to oscillation. Mirror neutrinos cannot be observed directly, but due to oscillations to ordinary neutrinos they can provide the largest neutrino flux at the highest energies.
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