核心坍缩超新星模拟得到的中子星质量函数
The Mass Function of Neutron Stars from Core-Collapse Supernova Simulations
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中文总结 AI 辅助
本研究通过三维超新星模拟推导映射关系，结合黑洞形成与 kick 速度影响，解释中子星质量函数，得出黑洞诞生占比约21%，预示超新星理论与观测协作时代将至。
中文摘要 AI 辅助
利用复杂三维超新星模拟推导得到的前身星核心结构与中子星引力质量之间的映射关系，我们确定了新生中子星的理论质量分布，并将其与中子星质量函数的测量结果进行比较。在此过程中，我们探究了黑洞形成岛及后续吸积的影响。研究表明，超新星理论可以解释观测到的中子星质量函数，从其约1.35倍太阳质量附近的低质量峰到高质量尾端。此外，低质量中子星诞生时预期的较低 kick 速度（ kick 译为“ kick 速度”，保留专业术语），以及高质量中子星平均预期的较高 kick 速度，均按预期方向塑造了观测到的质量函数。所有这些影响的最终结果是，在观测到的中子星质量函数上留下了反映中子星起源的不同物理过程以及中子星/黑洞二分性的特征。我们粗略推导得出黑洞诞生占比约为21%。综上，我们认为超新星理论如今可用于（尽管是暂时性地）解释致密天体群体的各种观测属性，且超新星理论与观测之间的高效协作时代即将到来。
英文摘要
Using the mapping between progenitor core structure and the gravitational mass of neutron stars derived from sophisticated 3D supernova simulations, we determine the theoretical mass distribution of neutron stars at birth and compare it with neutron star mass function measurements. In the process, we explore the effects of islands of black hole formation and subsequent mass accretion. We show that supernova theory can explain the observed neutron star mass function from its lower-mass peak near $\sim$1.35 $M_{\odot}$ to its higher-mass tail. Moreover, the lower predicted kick speeds expected during the birth of lower-mass neutron stars and the higher expected kick speeds expected on average for higher mass neutron stars both sculpt the observed mass function in desired directions. The upshot of all these influences is to imprint upon the measured neutron star mass function features that reflect the varied physics of both neutron star origins and the neutron-star/black-hole dichotomy. Very approximately, we derive a black hole birth fraction of $\sim$21\%. In summary, we suggest that supernova theory can now be used to explain, however provisionally, various measured attributes of the population of compact objects and that an era of productive engagement between supernova theory and observation is at hand.
