AI 中文总结
本研究通过多能谱、多角度模拟，揭示超新星中微子的能量依赖型慢集体味转换会提升中微子加热率与电子丰度，凸显能量依赖处理的重要性。
AI 中文摘要
我们对超新星中微子的慢集体味转换（SFC）开展了多能谱、多角度模拟研究，涉及吸积早期、吸积晚期和冷却阶段的三类典型中微子能谱，这些能谱中存在初始电子味与重轻子味中微子能谱的多次交叉。通过在局域周期箱中数值求解中微子量子动力学方程，我们发现，主要由空间非均匀不稳定性触发的SFC会驱动系统向空间粗粒化的准稳态演化，其味转换概率强烈依赖于能量、角度以及中微子质量顺序。我们还发现，并非所有初始能谱交叉都会在末态完全消失，而受快味转换研究启发的、可消除能谱交叉的类箱型简单解析方案，能够合理近似SFC后的能谱。利用初始能谱和SFC后能谱，我们还评估了对应的νₑ和ν̄ₑ加热率以及吸收平衡电子丰度（Yₑ）的变化。在考虑的场景中，当交叉能量以上的能谱差异显著时，由于νₓ到νₑ（以及ν̄ₓ到ν̄ₑ）的净转换，加热率总体提升了约80%；对于吸收平衡Yₑ，SFC导致的能谱变化使其提升了约0.03，原因是νₑ的吸收速率比ν̄ₑ提升更显著，这可能使超新星物质更富质子。这些结果凸显了对超新星中微子开展能量依赖型SFC处理的重要性。
英文摘要
We study collective slow flavor conversion (SFC) of supernova neutrinos with multi-energy, multi-angle simulations for three representative neutrino spectra in the early accretion, late accretion, and cooling phases, in which multiple crossings between the initial electron- and heavy-lepton-flavor spectra are present. By numerically solving the neutrino quantum kinetic equations in a local periodic box, we find that SFC triggered predominantly by the spatially inhomogeneous instabilities drives the system toward a spatially coarse-grained, quasi-stationary state, whose flavor conversion probability depends strongly on energy, angle, and the neutrino mass ordering. While we find that not all of the initial spectral crossings are completely erased in the final state, a simple, box-like analytical prescription inspired by studies of fast flavor conversions, which eliminates the spectral crossings, can reasonably approximate the post-SFC spectra. Using the initial and post-SFC spectra, we also evaluate the changes of the corresponding $ν_e$ and $\barν_e$ heating rates as well as the absorption equilibrium electron fraction ($Y_e$). Within the considered scenarios, we find that the heating rates are generally enhanced by up to $\sim 80\%$ due to the net conversion of $ν_x$ to $ν_e$ (and $\barν_x$ to $\barν_e$) above their crossing energy, provided that the energy spectra above the crossing energy differ substantially. For the absorption equilibrium $Y_e$, spectra changes due to SFC increase it by $\sim 0.03$ due to the relatively more enhanced $ν_e$ absorption rate than $\barν_e$, which potentially drives supernova materials to be more proton-rich. These results highlight the importance of energy-dependent treatments of SFC for supernova neutrinos.
Comments17 pages, 11 figures
