论文标题
在SMC中成为X射线二进制物作为传质效率的指标
Be X-ray binaries in the SMC as indicators of mass transfer efficiency
论文作者
论文摘要
是X射线二进制文件（BEXRB）由迅速旋转的恒星组成，中子恒星伴侣从折线发射磁盘中积聚。我们比较了小麦哲伦云中观察到的BEXRB与Compas种群合成代码产生的类似BEXRB的系统的模拟种群。我们关注的是BEXRB中明显更低的BE恒星质量比整个人口中的恒星更高。假设BEXRB仅经历了动态稳定的传质，它们的质量分布表明，B-Star Companion通常会积聚由中子星的祖细胞捐赠的质量的30％。我们预计这些结果会影响双重紧凑型物体合并人群的预测。模拟的BEXRB种群的卷积与小麦芽岩云的星形形成历史表明，Bexrbs的过量很可能是由于该星系在20--40 Myr Aoto左右的星系爆发而解释的。
Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star companions accreting from the circumstellar emission disk. We compare the observed population of BeXRBs in the Small Magellanic Cloud with simulated populations of BeXRB-like systems produced with the COMPAS population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stable mass transfer, their mass distribution suggests that at least 30% of the mass donated by the progenitor of the neutron star is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the Small Magellanic Cloud shows that the excess of BeXRBs is most likely explained by this galaxy's burst of star formation around 20--40 Myr ago.
