用超新星爆发的上升时间探测中微子质量等级
Probing the neutrino mass hierarchy with the rise time of a supernova burst
摘要：
银河系超新星（SN）bar-nue光变曲线的上升时间，在高统计实验，如冰立方切伦科夫探测器，可以提供一个诊断工具的中微子质量等级在“大”1-3轻子混合角θ_1 - 3。由于一方面在早期后反弹时间的集体效应的物质抑制和另一方面在SN的外层中存在普通的Mikheyev-Smirnov-Wolfenstein效应的组合，O（100）ms尺度上足够快的上升时间表明了颠倒的质量等级。我们调查的结果，从一个广泛的恒星核心崩溃模拟，提供了第一次探索这些功能的天体物理学的鲁棒性。我们发现，对于所有的模型分析（共享相同的弱相互作用微观物理）的上升时间为同一层次是相似的，不仅定性，而且定量，与信号的两类层次显着分离。我们表明，通过蒙特卡罗模拟，这两种情况下应区分在冰立方SNe在一个典型的银河系距离99%的时间。最后，一个初步的调查似乎表明，更快的上升时间为倒置的层次结构相比，正常的层次结构是一个定性的强大功能预测的几个模拟组。由于这个签名的可行性最终取决于定量评估的理论/数值的不确定性，我们的研究结果激励了广泛的运动的比较不同的代码预测在早期的吸积时间与实施的微物理相当的复杂性，包括影响，如核子反冲在弱相互作用。
英文摘要：
The rise time of a Galactic supernova (SN) bar-nue lightcurve, observable at a high-statistics experiment such as the IceCube Cherenkov detector, can provide a diagnostic tool for the neutrino mass hierarchy at "large" 1-3 leptonic mixing angle theta_13. Thanks to the combination of matter suppression of collective effects at early postbounce times on one hand and the presence of the ordinary Mikheyev-Smirnov-Wolfenstein effect in the outer layers of the SN on the other hand, a sufficiently fast rise time on O(100) ms scale is indicative of an inverted mass hierarchy. We investigate results from an extensive set of stellar core-collapse simulations, providing a first exploration of the astrophysical robustness of these features. We find that for all the models analyzed (sharing the same weak interaction microphysics) the rise times for the same hierarchy are similar not only qualitatively, but also quantitatively, with the signals for the two classes of hierarchies significantly separated. We show via Monte Carlo simulations that the two cases should be distinguishable at IceCube for SNe at a typical Galactic distance 99% of the times. Finally, a preliminary survey seems to show that the faster rise time for inverted hierarchy as compared to normal hierarchy is a qualitatively robust feature predicted by several simulation groups. Since the viability of this signature ultimately depends on the quantitative assessment of theoretical/numerical uncertainties, our results motivate an extensive campaign of comparison of different code predictions at early accretion times with implementation of microphysics of comparable sophistication, including effects such like nucleon recoils in weak interactions.
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