引力波源探测中微子的能力及附加探测器在未来反应堆中微子实验中的贡献
The determination capability of potential neutrinos from gravitational wave sources and contributions of extra detector at the future reactor neutrino experiment
摘要：
自2015年以来，在发现了多个引力波瞬变事件之后，研究与引力波事件相一致的中微子信号现在成为现有中微子实验的重要任务。不幸的是，目前还没有发现候选中微子。本文介绍了在未来的反应堆中微子实验（如JUNO和RENO-50）中寻找中微子过剩的一种方法，以便从引力波源中寻找潜在的中微子。根据我们的计算和模拟，在标称JUNO实验中未检测到与引力波相关的$\barν_e$，导致$\barν_e$信号灵敏度为90 $\%$置信水平（C.L.），$μ_{90}$ = 2.44。这对应于中微子在地球上的注量范围，约为6 $\times$ 10 $^{10}$ cm $^{-2}$至4 $\times$ 10 $^{10}$ cm $^{-2}$，中微子能量范围为1.8 MeV至120 MeV，假设为单色能谱。基于某些流行的描述引力波源的模型，我们计算了相应的注量（$F_{UL}^{90}$），对于单色能谱假设和费米-狄拉克能谱假设，其值约为1 - 3 $\times$ × 10 $^{8}$ cm $^{-2}$。然后，我们将$F_{UL}^{90}$转换成可检测的距离（$D_\text{UL}^{90}$），约1 - 3 Mpc的两个假设，在这些已知的模型中预测的光度。为了进一步提高灵敏度，我们讨论了额外的探测器的潜在好处，不同的目标质量和基线。特别是，如果额外的探测器被设计为与JUNO探测器相同，则将有大约38%的灵敏度提高和大约28%的$\%$可探测距离增加。另一方面，如果我们将JUNO实验与RENO-50实验结合起来，而不是建造额外的探测器，灵敏度也将显著提高。
英文摘要：
After several gravitational wave transients were discovered since 2015, studying neutrino signals coincident with the gravitational wave events now becomes an important mission for the existing neutrino experiments. Unfortunately, no candidate neutrinos have been found yet. This article introduces a method to find the neutrino excess to search for the potential neutrinos from gravitational wave sources at the future reactor neutrino experiment (such as JUNO and RENO-50). According to our calculations and simulations, the non-detection of $\barν_e$ associated with gravitational waves at the nominal JUNO experiment gives rise to the $\barν_e$ signal sensitivity at 90$\%$ confidence level (C.L.), $μ_{90}$ = 2.44. This corresponds to the range of neutrino fluence on the Earth around 6 $\times$ 10$^{10}$ cm$^{-2}$ to 4 $\times$ 10$^{10}$ cm$^{-2}$ with neutrino energy range from 1.8 MeV to 120 MeV at monochromatic energy spectrum assumption. Based on certain popular models which describe the gravitational wave sources, we calculate the corresponding fluence ($F_{UL}^{90}$), which is around 1 - 3 $\times$ 10$^{8}$ cm$^{-2}$ for both monochromatic energy spectrum assumption and Fermi-Dirac energy spectrum assumption. Then we convert $F_{UL}^{90}$ into the detectable distance ($D_\text{UL}^{90}$), about 1 - 3 Mpc for two assumptions, with the predicted luminosities in these known models. To further improve the sensitivity, we discuss the potential benefits from an extra detector, with different target masses and baselines. Particularly, there will be around 38\% sensitivity improvement and around 28$\%$ detectable distance increasing if the extra detector is designed to be identical to the JUNO detector. On the other hand, instead of building an extra detector, if we combine the JUNO experiment with the RENO-50 experiment, the sensitivity will also be significantly improved.
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