论文标题
恒星崩溃的多样性和弥漫性超新星中微子背景
Stellar Collapse Diversity and the Diffuse Supernova Neutrino Background
论文作者
论文摘要
弥漫性宇宙超新星中微子背景（DSNB）是加多琳负载的超级kamiokande（SK）检测器以及即将到来的Juno和Hyper-Kamiokande探测器的观察目标。我们对超新星（SN）爆炸机制以及对状态和最大质量的中子星（NS）方程的不完全理解，阻碍了当前的预测。在我们的全面研究中，我们基于Sukhbold等人获得的成功和失败的SN爆炸的景观来重新审视这个问题。和Ertl等。具有参数化的一维中微子发动机，用于大型单星和氦星祖细胞，后者是二元进化效应的代理。除了考虑不同强度的引擎，导致失败的SNE与黑洞（BH）形成不同之外，我们还改变了NS质量限制，中微子发射的频谱形状，并包括良好理解的替代NS形成通道（如积分诱导的或合并引起的崩溃或合并引起的崩溃事件）的贡献。由于大型模型集的中微子信号是近似的，因此我们通过使用原始中子恒星冷却的最新模拟来校准相关的自由度。我们的预测比最近的预测更高，因为大量失败的SNE很大，而BH形成很长。我们的最佳猜测模型预测DSNB电子抗激抗体28.8^{+24.6} _ { - 10.9} cm^{ - 2} s^{ - 1}，具有6.0^{+5.1} {+5.1} _ { - 2.1} _ {-2.1} cm^{-2.1} cm^{ - 2} cm^{-2} cm^{ - 2} s^s^s^s^{-1}和1.3^{+1.1} _ { - 0.4} cm^{ - 2} s^{ - 1}，带有电子 - antineutrino Energies> 17.3 MeV，大约低于当前SK限制的两个因子。不确定性范围仍由恒星核心崩溃事件的宇宙速率仍然不足。
The diffuse cosmic supernova neutrino background (DSNB) is observational target of the gadolinium-loaded Super-Kamiokande (SK) detector and the forthcoming JUNO and Hyper-Kamiokande detectors. Current predictions are hampered by our still incomplete understanding of the supernova (SN) explosion mechanism and of the neutron star (NS) equation of state and maximum mass. In our comprehensive study we revisit this problem on grounds of the landscapes of successful and failed SN explosions obtained by Sukhbold et al. and Ertl et al. with parametrized one-dimensional neutrino engines for large sets of single-star and helium-star progenitors, with the latter serving as proxy of binary evolution effects. Besides considering engines of different strengths, leading to different fractions of failed SNe with black-hole (BH) formation, we also vary the NS mass limit, the spectral shape of the neutrino emission, and include contributions from poorly understood alternative NS-formation channels such as accretion-induced or merger-induced collapse events. Since the neutrino signals of our large model sets are approximate, we calibrate the associated degrees of freedom by using state-of-the-art simulations of proto-neutron star cooling. Our predictions are higher than other recent ones because of a large fraction of failed SNe with long delay to BH formation. Our best-guess model predicts a DSNB electron-antineutrino-flux of 28.8^{+24.6}_{-10.9} cm^{-2}s^{-1} with 6.0^{+5.1}_{-2.1} cm^{-2}s^{-1} in the favorable measurement interval of [10,30] MeV, and 1.3^{+1.1}_{-0.4} cm^{-2}s^{-1} with electron-antineutrino energies > 17.3 MeV, which is roughly a factor of two below the current SK limit. The uncertainty range is dominated by the still insufficiently constrained cosmic rate of stellar core-collapse events.
