标题： 碰撞流形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Fornax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风味不稳定性（CFI）的影响。 我们将通过数值求解多组分色散关系计算得到的均匀CFI（hCFI）模式的增长率与使用单色近似计算得到的值进行比较。 我们发现，在多组分情况下应用广泛使用的单色近似会导致错误的增长率。 与单色近似给出的$\sim10^5$ s$^{-1}$值相反，非共振多组分hCFI的实际增长率在我们所有的模型中最多为$\sim$200 s$^{-1}$，它们太慢以至于无法影响CCSN的结果。 我们在模拟中采用BGK风味转换方案以包含类似共振的hCFI的影响。 我们发现CCSN的动力学和中微子发射特性仅受到微弱的影响，由于对流和中微子驱动湍流引起的内在随机性可以自然地导致相似的效果。 因此，我们对非共振和类似共振的hCFI进入CCSN模拟的分析表明，由hCFI模式触发的中微子风味转换的影响通常很小。 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 Fornax. 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.