论文标题
关于银河系的核心倒塌超新星的速度
On the rate of core collapse supernovae in the Milky Way
论文作者
论文摘要
在世界各地运行的几个大型中微子望远镜，作为其主要目的，是对银河系中的重力崩溃散发出的中微子的首次检测。这些观察计划的成功取决于银河系中超新星核心崩溃的速度，即$ r $。在这项工作中，标准统计技术用于结合几个独立的结果。讨论了它们的一致性，并确定了最关键的输入数据。通过在银河系中以及从中微子望远镜和电磁调查中获得的有关重力崩溃事件的发生率的直接信息，进一步测试和完善了对$ r $的推断。对错误的保守处理可产生$ r = 1.63 \ pm 0.46 $（100 yr）$^{ - 1} $;核心崩溃超新星事件之间的相应时间是$ t = 61 _ { - 14}^{+24} $〜yr。强调更新恒星出生方法分析的重要性。
Several large neutrino telescopes, operating at various sites around the world, have as their main objective the first detection of neutrinos emitted by a gravitational collapse in the Milky Way. The success of these observation programs depends on the rate of supernova core collapse in the Milky Way, $R$. In this work, standard statistical techniques are used to combine several independent results. Their consistency is discussed and the most critical input data are identified. The inference on $R$ is further tested and refined by including direct information on the occurrence rate of gravitational collapse events in the Milky Way and in the Local Group, obtained from neutrino telescopes and electromagnetic surveys. A conservative treatment of the errors yields a combined rate $R=1.63 \pm 0.46$ (100 yr)$^{-1}$; the corresponding time between core collapse supernova events turns out to be $T=61_{-14}^{+24}$~yr. The importance to update the analysis of the stellar birthrate method is emphasized.
