发表机构
National Tsing Hua University; National Center for Theoretical Sciences（国立清华大学; 国家理论科学中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文研究超轻标量暗物质背景中微子振荡，计算AGN和DSNB源的味比变化，并与IceCube及HK/DUNE/JUNO灵敏度比较。
AI 中文摘要
中微子与物质的相互作用导致最终味组成偏离真空中的预期。本文考虑中微子与超轻标量暗物质 $\phi$（$m_\phi\ll 1\\,{\rm eV}$）的相互作用。当中微子从遥远源发射并穿过暗物质介质时，哈密顿量中的 MSW 势被假设的 $\nu\phi$ 有效势所取代。我们采用两类中微子源进行计算。第一类是点状中微子源，即活动星系核（AGN），主要通过带电π介子衰变产生 $\mathcal{O}({\rm TeV})$ 中微子，初始味比为（$\nu_e,\nu_\mu,\nu_\tau$）=（$1:2:0$）。我们重点分析两个具体 AGN：NGC 1068 和 TXS 0506+056，它们到地球的距离远大于中微子振荡长度。我们考虑 $\nu\phi$ 耦合常数的范围，使得绝热条件和平均自由程得到满足。因此，假设中微子从其冕区随机产生，我们计算了 $m_\phi=10,1,0.1\\,{\rm peV}$ 和 $m_\phi=1,0.1,0.01\\,{\rm feV}$ 情况下地球处的平均味比，生成中微子味的三元图，并与 IceCube 当前和未来的灵敏度进行比较。考虑的第二个源是弥散超新星中微子背景（DSNB），它是能量为 $\mathcal{O}({\rm MeV})$ 的各向同性中微子源。将核心坍缩模拟中微子温度应用于 DSNB 通量，我们对 $m_\phi=10^{-22}\\,{\rm eV}$ 的 DSNB 重复类似分析，并估计不同中微子味落在 HK/DUNE/JUNO 组合灵敏度极限内。
英文摘要
The neutrino-matter interaction cause the final flavor compositions deviating from those expected in vacuum. In this work we consider neutrinos interact with ultra-light scalar dark matters $ϕ$ ($m_ϕ\ll 1\,{\rm eV}$). When the neutrinos emitted from a distant source and propagate through the dark matter medium, the MSW potential in the Hamiltonian is replaced by the hypothetical $νϕ$ effective potential. Two types of neutrino sources are adopted in our calculations. The first is point-like neutrino source, the Active Galactic Nuclei (AGN), which produce $\mathcal{O}({\rm TeV})$ neutrinos primarily through charged pion decay, yielding an initial flavor ratio of ($ν_e,ν_μ,ν_τ$)=($1:2:0$). We focus on two specific AGNs, NGC 1068 and TXS 0506+056 in our analysis, whose distances from Earth are much larger than the neutrino oscillation lengths. We consider the range of $νϕ$ coupling constant such that the adiabatic condition and mean free path can be satisfied. Hence, by assuming neutrinos are produced randomly from their corona regions, we compute the averaged flavor ratio at Earth with $m_ϕ=10,1,0.1\,{\rm peV}$ and $m_ϕ=1,0.1,0.01\,{\rm feV}$, generate the ternary plots of neutrino flavors, and compare the results with the IceCube present and future sensitivities. The second source considered is the Diffuse Supernova Neutrino Background (DSNB), it is an isotropic neutrino source with energy $\mathcal{O}({\rm MeV})$. Applying the core-collapse simulation neutrino temperatures to the DSNB flux, we repeat the similar analysis for the DSNB with $m_ϕ=10^{-22}\,{\rm eV}$, and we estimate different neutrino flavors lies in the HK/DUNE/JUNO combined sensitivities limit.
