三维核心坍缩超新星模拟：从壳层燃烧到激波 revival
Three-dimensional Core-Collapse Supernova Simulations: From shell burning to shock revival
- Stockholm University（斯德哥尔摩大学）
- University of Arizona（亚利桑那大学）
- Michigan State University（密歇根州立大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
通过三维模拟研究不同质量前身星的核心坍缩超新星，发现多维前身星可提升激波后非径向动能与激波半径，且最早出现激波 revival，引力波增强源于吸积流变化。
AI中文摘要：
核心坍缩超新星模拟的结果高度依赖于坍缩起始时前身星的多维结构。我们对5个无旋转、太阳金属丰度的前身星进行了恒星演化最后约10-15分钟的三维模拟，这些前身星的零龄主序质量分别为20、21.5、24.5、26和29倍太阳质量，由一维MESA模型映射到FLASH流体动力学代码中。所有5个模型的富氧层都出现了对流，对流速度达到每秒数百公里，部分模型的内部硅和氧燃烧壳层也出现了强对流。针对24.5倍太阳质量的前身星，我们进行了三次核心坍缩模拟：一次以完全三维模型为初始条件，一次以其角度平均对应物为初始条件，还有一次以原始一维MESA前身星为初始条件。我们发现，多维前身星导致激波后区域的非径向动能比角度平均模型高35%至50%，平均激波半径大5%至10%，且是三者中最早出现激波 revival 的。所有三个模型的引力波发射相似，且在激波 revival 后增强，这是由原中子星的吸积流变化驱动的，而非前身星的不对称性。
英文摘要：
The outcome of core-collapse supernova simulations depends sensitively on the multi-dimensional structure of the progenitor star at the onset of collapse. We perform three-dimensional simulations of the final ~10-15 minutes of stellar evolution for five non-rotating solar-metallicity progenitors with zero-age main-sequence masses of 20, 21.5, 24.5, 26, and 29 solar masses, mapped from one-dimensional MESA models into the FLASH hydrodynamics code. Convection develops in the oxygen-rich layers of all five models, with convective velocities reaching several hundred km/s, and in some models strong convection also develops in the inner silicon- and oxygen-burning shells. For the 24.5 solar mass progenitor, we carry out three core-collapse simulations: one initialised from the fully three-dimensional model, one from its angle-averaged counterpart, and one from the original one-dimensional MESA progenitor. We find that the multi-dimensional progenitor leads to 35 to 50% higher non-radial kinetic energy in the post-shock region and an average shock radius 5 to 10% larger than in the angle-averaged model, and shows the earliest shock revival of the three. The gravitational-wave emission is similar in all three models and strengthens after shock revival, driven by a change in the downflows reaching the protoneutron star rather than by progenitor asymmetries.
