标题： 快速旋转的16$M_{\odot}$星的三维坍缩 显示英文标题

标题： The Three-Dimensional Collapse of a Rapidly Rotating 16 $M_{\odot}$ Star

摘要： 我们报告了快速旋转的16$M_{\odot}$星体铁核坍缩的三维（3D）流体动力学演化。 首次，我们跟踪了铁核和对流壳层燃烧区域中角动量（AM）分布的3D演化，持续最后10分钟，直至引力不稳定性及核心坍缩。 在3D中，我们发现对流区域表现出高效的AM传输，导致AM分布的形状和大小与$\texttt{MESA}$在几个壳层对流周转时间尺度内有所不同。 对于不同的前体模型，例如那些具有紧密耦合的Si/O对流壳层，3D模拟中的高效AM传输可能导致恒星内部AM分布显著不同，从而影响对新生中子星或黑洞自转的估计。 我们的结果表明，对流和旋转壳层燃烧区域中的3D AM传输是大质量恒星模型中的关键组成部分，可能会定性地改变爆炸结果和推断出的致密残留物特性。 显示英文摘要

摘要： We report on the three-dimensional (3D) hydrodynamic evolution to iron core-collapse of a rapidly rotating 16 $M_{\odot}$ star. For the first time, we follow the 3D evolution of the angular momentum (AM) distribution in the iron core and convective shell burning regions for the final 10 minutes up to and including gravitational instability and core-collapse. In 3D, we find that convective regions show efficient AM transport that leads to an AM profile that differs in shape and magnitude from $\texttt{MESA}$ within a few shell convective turnover timescales. For different progenitor models, such as those with tightly coupled Si/O convective shells, efficient AM transport in 3D simulations could lead to a significantly different AM distribution in the stellar interior affecting estimates of the natal neutron star or black hole spin. Our results suggest that 3D AM transport in convective and rotating shell burning regions are critical components in models of massive stars and could qualitatively alter the explosion outcome and inferred compact remnant properties.