论文标题
二进制中子星合并的进化起源：共同包膜效率和金属性的影响
Evolutionary Origins of Binary Neutron Star Mergers: Effects of Common Envelope Efficiency and Metallicity
论文作者
论文摘要
紧凑型二元合并的形成历史，尤其是恒星质量的二进制黑色孔合并，最近受到了审查和修订的增加。在本文中，我们重新审视了形成二进制中子星级合并的主要形成渠道和效率的问题。我们使用恒星和二进制进化代码MESA，并实现一种最新和详细的方法，用于公共信封和传质。我们使用不同的公共包膜效率和两个电子捕获超新星的供应量在8-20个太阳能质量之间进行了供体块，具有1.4和2.0太阳能质量的中子恒星伴侣。与二元黑孔合并的情况相反，对于1.4太阳能质量的中子星星伴侣，所有二元中子星星合并均在一个共同的信封阶段形成，而对于中子质量的2.0太阳能质量，我们仅在稳定的质量转移后，如果中子质量转移，则在中子质量的一小部分合并中，如果中子恒星获得了大型NATAL NATAL，则仅识别出稳定的合并。无论中子星伴侣质量如何，我们都会发现，在形成二进制中子星星合并的形成中，大型的超新星踢是受到青睐的，并且与太阳能相比，在近极金属性上找到更多合并。
The formation histories of compact binary mergers, especially stellar-mass binary-black hole mergers, have recently come under increased scrutiny and revision. In this paper we revisit the question of the dominant formation channel and efficiency of forming binary neutron-star mergers. We use the stellar and binary evolution code MESA and implement an up-to-date and detailed method for common envelope and mass transfer. We preform simulations for donor masses between 8-20 solar masses with a neutron star companion of 1.4 and 2.0 solar masses, at two metallicities, using varying common envelope efficiencies, and two prescriptions for electron-capture supernovae. In contrast to the case of binary-black hole mergers, for a neutron star companion of 1.4 solar masses, all binary neutron star mergers are formed following a common envelope phase, while for a neutron star mass of 2.0 solar masses we identify a small subset of mergers following only stable mass transfer if the neutron star receives a large natal kick. Regardless of neutron star companion mass, we find that large supernova natal kicks are favored in the formation of binary neutron star mergers, and find more mergers at subsolar metallicity compared to solar.
