Novel techniques to detect supernova neutrinos with scintillator and lead detectors

中微子的性质影响着广泛的物理学。近十年来最杰出的科学成就之一是基于中微子振荡效应的中微子静止质量不为零的证明。核心坍缩超新星爆炸是中微子的一个特殊来源，其首次观测发生在1987年。与此同时，更多的现代探测器已经存在，更多的正在计划中。一个重要的反应是中微子-质子弹性散射，一个中性流（NC）反应，可能对所有的味道。利用这种反应进行超新星观测，对观测者来说是幸运的。因此，然而，需要测量反冲质子相对于相应电子光产额的光产额（所谓的猝灭因子）。猝灭因子的值与能量有关，并且随闪烁体的不同而变化。因此，需要针对单个实验测量猝灭。由于星系核心坍缩超新星的罕见性，不同实验之间的互补性和协同作用也需要考虑，以充分利用下一次近超新星事件。SNO+和HALO实验在这方面特别令人感兴趣，因为它们使用完全不同的探测器技术，但在同一实验室进行。

Neutrino properties influence a wide range of physics. One of the outstanding scientific achievements of the last decade is the proof of a non-vanishing neutrino rest mass based on the effect of neutrino oscillations. Core collapse supernova explosions are a particular source of neutrinos whose first observation took place in 1987. Meanwhile far more modern detectors are existing and further are being planned. An important reaction is the neutrino-proton elastic scattering, a neutral current (NC) reaction possible for all flavours. The usage of this reaction for a supernova observation is fortunate for scintillators. Therefore, however, the light yield of the recoiled protons relative to the respective electron light yield (the so-called quenching factor) needs to be measured. The value of the quenching factor is energy dependent and varies from scintillator to scintillator. Thus the quenching needs to be measured for the individual experiment. Due to the rareness of a galactic core collapse supernova also complementarity and synergy between different experiments need to be considered to get the most out of a next near supernova event. The experiments SNO+ and HALO are in this context of special interest, as they make use of completely different detector technologies but are standing in the same laboratory.