On the detection of pre-low-mass X-ray binaries
On the detection of pre-low-mass X-ray binaries
复制标题
关于低质量前 X 射线双星的探测
DOI：
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发表时间：
2003
期刊：
影响因子：
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通讯作者：
Ulrich Kolb
中科院分区：
文献类型：
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作者：
Bart Willems;Ulrich Kolb
我们探索人口的候选人前低质量的X射线双星中，中子星星吸积质量从风的低质量的同伴（质量为2 M）的二元人口合成研究的框架。模拟的吸积光度分布显示出一个接近1031 erg/s的主峰和一个接近1028 erg/s的次峰。这两个峰值的相对贡献主要取决于中子星星出生时所受反冲速度的大小。当平均反冲速度大于200 km/s时，次峰可以忽略不计，但当平均反冲速度小于50 km/s时，次峰占主导地位。无论这两个峰的相对贡献如何，我们的计算表明，前低质量X射线双星可能对银河系中离散低光度X射线源的数量有不可忽视的贡献。
We explore the population of candidate pre-low-mass X-ray binaries in which a neutron star accretes mass from the wind of a low-mass companion (mass � 2 M⊙) in the framework of a binary population synthesis study. The simulated accretion-luminosity distribution shows a primary peak close to 10 31 erg/s and a secondary peak near 10 28 erg/s. The relative contribution of the two peaks depends primarily on the magnitude of the kick velocity imparted to the neutron star at birth. The secondary peak is negligible for average kick velocities larger than � 200 km/s, but becomes dominant for average kick velocities smaller than � 50 km/s. Regardless of the relative contributions of the two peaks, our calculations suggest that pre-low-mass X-ray binaries may provide a non-negligible contribution to the population of discrete low-luminosity X-ray sources in the Galaxy.