论文标题
双中性星星合并的质量
Masses of double neutron star mergers
论文作者
论文摘要
目标。通过无线电脉冲星观测和重力波观测观察到的双中性恒星二进制群体之间的质量差异需要解释。 方法。进行了二元种群合成计算，并将其结果与无线电和重力波的观测进行比较。 结果。二进制进化的模拟用于将双中性恒星二进制二进制的不同观察结果联系起来。 GW190425的祖先进行了更详细的研究。提出了可能的祖细胞的质量和合并时间的分布。 结论。在银河系中，无线电脉冲星与另一个中子星的伴侣和从重力波观测到的这些合并系统的重力观测质量之间存在质量差异，这是二进制进化中的。
Aims. The mass discrepancy between the observed population of double neutron star binaries by radio pulsar observations and gravitational-wave observation requires an explanation. Methods. Binary population synthesis calculations are performed, and their results are compared with the radio and the gravitational-wave observations simultaneously. Results. Simulations of binary evolution are used to link different observations of double neutron star binaries with each other. The progenitor of GW190425 is investigated in more detail. A distribution of masses and merger times of the possible progenitors is presented. Conclusions. A mass discrepancy between the radio pulsars in the Milky Way with another neutron star companion and the inferred masses from gravitational-wave observations of those kind of merging systems is naturally found in binary evolution.
