基于超级神冈探测器（Super-Kamiokande）所指示的弥散超新星中微子背景（DSNB）给出的轴子约束
An axion constraint from the diffuse supernova neutrino background indicated by Super-Kamiokande
中文总结 AI 辅助
本研究利用超级神冈探测器指示的弥散超新星中微子背景，通过中微子辐射流体动力学模拟，得到轴子-质子耦合常数的1σ上限，该约束不依赖单个超新星性质，可用于其他相关弱相互作用粒子研究。
中文摘要 AI 辅助
近期，超级神冈探测器（Super-Kamiokande）合作组报告了弥散超新星中微子背景（DSNB）的一个迹象，统计显著性为2.6σ。受这一可能发现的推动，我们基于长期中微子辐射流体动力学模拟，研究轴子冷却对DSNB通量的影响。我们将观测通量与我们的模型进行比较，得到轴子-质子耦合常数的1σ上限|g_ap|<1.3×10⁻⁹，该上限可与基于SN 1987A中微子爆发的传统约束相比。与SN 1987A的约束不同，DSNB约束不依赖于单个观测到的超新星的性质，因为DSNB代表了宇宙中一系列核心坍缩事件的累积中微子发射。更广泛地说，该方法可应用于其他修改原中子星冷却的弱相互作用粒子。
英文摘要
Recently, the Super-Kamiokande Collaboration reported an indication of the diffuse supernova neutrino background (DSNB) with a statistical significance of $2.6σ$. Motivated by this possible discovery, we investigate the impact of axion cooling on the DSNB flux on the basis of long-term neutrino-radiation hydrodynamic simulations. We compare the observed flux and our models and obtain a $1σ$ upper limit $|g_{ap}|<1.3\times10^{-9}$ on the axion-proton coupling constant, which is comparable to the conventional limit based on the SN 1987A neutrino burst. In contrast to the SN 1987A bound, the DSNB constraint does not rely on the properties of a single observed supernova, because the DSNB represents the cumulative neutrino emission from a cosmic population of core-collapse events. More generally, this approach can be applied to other feebly interacting particles that modify protoneutron-star cooling.
