在三维核塌缩超新星模型中快速成对集体中微子振荡的发生
Where, when and why: occurrence of fast-pairwise collective neutrino oscillation in three-dimensional core-collapse supernova models
摘要：
快对集体中微子振荡是核心坍缩超新星理论中的一个关键不确定性。尽管对CCSN动力学的潜在重大影响，它通常被忽略在CCSN的数值模型，因为自洽地将这种物理的强大的技术困难。在本文中，我们调查的前景发生快速味转换诊断电子中微子轻子数（ELN）交叉在十几个国家的最先进的三维CCSN模型。ELN交叉是触发风味转换的必要条件。虽然只有零阶和第一个角动量是可从模拟，我们的新方法使我们能够看到中微子在动量空间中的角分布，并提供准确的洞察ELN交叉。我们的分析表明，快速的风味转换一般发生在CCSNe的冲击后区域，爆炸模型提供了更有利的条件比失败的CCSNe风味转换。我们还发现，有共同的和祖细胞依赖的特性。将ELN穿越分为两种类型，通过研究中微子辐射场和物质相互作用，分析了每种情况下ELN穿越的产生机制。我们发现CCSN动力学驱动ELN交叉的关键成分：原中子星（PNS）对流，不对称中微子发射，中微子散射和散射。这项研究表明，我们需要在现实的CCSN模型中适应快速的风味转换。
英文摘要：
Fast-pairwise collective neutrino oscillation represents a key uncertainty in the theory of core-collapse supernova (CCSN). Despite the potentially significant impact on CCSN dynamics, it is usually neglected in numerical models of CCSN because of the formidable technical difficulties of self-consistently incorporating this physics. In this paper, we investigate the prospects for the occurrence of fast flavor conversion by diagnosing electron neutrino lepton number (ELN) crossing in more than a dozen state-of-the-art three-dimensional CCSN models. ELN crossings is a necessary condition for triggering flavor conversion. Although only zeroth and first angular moments are available from the simulations, our new method enables us to look into the angular distributions of neutrinos in momentum space and provide accurate insight into ELN crossings. Our analysis suggests that fast flavor conversion generally occurs in the post-shock region of CCSNe, and that explosive models provide more favorable conditions for the flavor conversion than failed CCSNe. We also find that there are both common and progenitor-dependent characteristics. Classifying ELN crossings into two types, we analyze the generation mechanism of each case by scrutinizing the neutrino radiation field and matter interactions. We find key ingredients of CCSN dynamics driving the ELN crossings: proto-neutron star (PNS) convection, asymmetric neutrino emission, neutrino absorptions and scatterings. This study suggests that we need to accommodate fast flavor conversions in realistic CCSN models.
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