高质量X射线双星中中子星质量的光学天体测量
Masses of Neutron Stars in High-Mass X-ray Binaries with Optical Astrometry
摘要：
确定中子星（NS）内部物质的类型一直是天体物理学的长期目标。尽管如此，大多数预测最大质量在1.4-2.8太阳质量范围内的NS状态方程（EOS）仍然可行。迄今为止，大多数精确的NS质量测量显示接近1.4太阳质量的值，但对超大质量NS的可靠测量将限制EOS的可能性。在这里，我们研究如何在微弧秒水平的光学天体测量可以用来映射出的轨道的高质量X射线双星（HMXB），导致NS质量的严格限制。虽然Unwin及其同事和Tomsick及其同事以前的研究讨论了未来空间干涉测量任务应该能够进行这种测量的事实，但目前的工作描述了6个HMXB系统的详细模拟，包括对所有轨道参数的预测约束。我们发现，直接NS质量可以测量到的准确度为2.5%（1西格玛）在最好的情况下（X每），船帆座X-1的6.5%，和10%的其他两个HMXB。
英文摘要：
Determining the type of matter that is inside a neutron star (NS) has been a long-standing goal of astrophysics. Despite this, most of the NS equations of state (EOS) that predict maximum masses in the range 1.4-2.8 solar masses are still viable. Most of the precise NS mass measurements that have been made to date show values close to 1.4 solar masses, but a reliable measurement of an over-massive NS would constrain the EOS possibilities. Here, we investigate how optical astrometry at the microarcsecond level can be used to map out the orbits of High-Mass X-ray Binaries (HMXBs), leading to tight constraints on NS masses. While previous studies by Unwin and co-workers and Tomsick and co-workers discuss the fact that the future Space Interferometry Mission should be capable of making such measurements, the current work describes detailed simulations for 6 HMXB systems, including predicted constraints on all orbital parameters. We find that the direct NS masses can be measured to an accuracy of 2.5% (1-sigma) in the best case (X Per), to 6.5% for Vela X-1, and to 10% for two other HMXBs.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
