标题： 碰撞流型不稳定性对核心坍缩超新星模型的影响 显示英文标题

标题： The Effect of the Collisional Flavor Instability on Core-Collapse Supernova Models

摘要： 我们基于使用先进的辐射流体动力学代码 F{\sc ornax}进行的一维和二维核心坍缩超新星 (CCSN) 模拟，探讨了中微子碰撞型味不稳定性 (CFI) 的影响。 我们将通过数值求解多群色散关系计算出的均匀 CFI{(hCFI)}模式的增长率与使用单色近似计算出的值进行比较。 我们发现，当在多群情况下应用广泛使用的单色近似{导致错误的增长率}时。 {与单色近似给出的$\sim10^5$的$^{-1}$值相反，}实际的非共振多群{高阶中心化流形方法}增长率最多为$\sim$200 秒$^{-1}$，在所有模型中它们都太慢而无法影响 CCSN 结果。 我们在模拟中采用BGK类型的风味转换方案，以包含类似共振的{高斯共轭因子分解}的影响。 我们发现CCSN动力学和中微子发射特性仅受到微弱影响，由于对流和中微子驱动湍流引起的固有随机性可以自然导致可比较的效果。 因此，我们的分析表明，将非共振和类似共振的{高阶中心流形方法}引入CCSN模拟中，由{高阶中心流形指标}模式引发的中微子风味转换的影响通常较小。 显示英文摘要

摘要： We explore the effects of the neutrino collisional flavor instability (CFI) based on 1D and 2D core-collapse supernova (CCSN) simulations done using the sophisticated radiation-hydrodynamic code F{\sc ornax}. We compare the growth rates of homogeneous CFI {(hCFI)} modes calculated by numerically solving the multi-group dispersion relation to those calculated using the monochromatic approximation. We find that the widely-used monochromatic approximation {leads to incorrect growth rates} when applied in multi-group scenarios. {As opposed to the $\sim10^5$ s$^{-1}$ values given by the monochromatic approximation,} the actual growth rates of non-resonance multi-group {hCFI} are at most $\sim$200 s$^{-1}$ in all our models and they are too slow to affect CCSN outcomes. We adopt a BGK flavor conversion scheme in the simulations to include the effects of resonance-like {hCFI}. We find that the CCSN dynamics and neutrino emission properties are only weakly influenced, and the intrinsic stochasticity due to convection and neutrino-driven turbulence can naturally lead to comparable effects. Hence, our analysis of the non-resonance and resonance-like {hCFI} into CCSN simulations suggests that the effects of neutrino flavor conversion triggered by {hCFI} modes are in general small.