中微子在银河系暗物质晕中的传播
Neutrino propagation in the galactic dark matter halo
摘要：
中微子振荡是一种被广泛观察到的和公认的现象。众所周知，由于中微子与物质的相互作用，真空中的味道转换概率会出现偏差。在这项工作中，我们分析了中微子和银河系中的暗物质之间的新的相互作用对中微子振荡模式的影响。暗物质-中微子相互作用的模型是通过使用一个有效的耦合成正比的费米常数$G_F$，没有进一步的限制，其风味结构。对于银河系的暗物质配置文件，我们认为一个均匀的分布，以及几个密度分布，估计在所有情况下的相互作用所需的大小，以获得在不同的中微子能量的可观察到的效果。我们的讨论主要集中在PeV中微子能量范围内，将在IceCube和KM 3 NeT等天文台进行探索。所获得的结果可以解释在轻$\mathcal{O}$（sub-eV-keV）或WIMP类暗物质粒子或作为一个新的相互作用与介体的$\mathcal{O}$（sub-eV-keV）质量。
英文摘要：
Neutrino oscillations are a widely observed and well established phenomenon. It is also well known that deviations with respect to flavor conversion probabilities in vacuum arise due to neutrino interactions with matter. In this work, we analyze the impact of new interactions between neutrinos and the dark matter present in the Milky Way on the neutrino oscillation pattern. The dark matter-neutrino interaction is modeled by using an effective coupling proportional to the Fermi constant $G_F$ with no further restrictions on its flavor structure. For the galactic dark matter profile we consider an homogeneous distribution as well as several density profiles, estimating in all cases the size of the interaction required to get an observable effect at different neutrino energies. Our discussion is mainly focused in the PeV neutrino energy range, to be explored in observatories like IceCube and KM3NeT. The obtained results may be interpreted in terms of a light $\mathcal{O}$(sub-eV--keV) or WIMP-like dark matter particle or as a new interaction with a mediator of $\mathcal{O}$(sub-eV--keV) mass.
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