了解银河系中的普通恒星：一个飞跃
Understanding the Galactic population of normal pulsars: A leap forward
摘要：
我们重新审视人口的正常星系领域中的“进化”的方法。通过比较由Parkes多波束脉冲星巡天、Arecibo L波段馈源阵列巡天和两个Swinburne多波束巡天探测到的合成类星体的各种参数的分布与由相同巡天探测到的真实类星体的各种参数的分布，我们发现，使用制动指数在2.5到3.0范围内的均匀分布可以获得良好的物理上真实的模型，自旋与磁轴夹角的余弦在0 ~ 1范围内均匀分布，表面磁场的对数正态出生分布，其平均值和标准差分别为12.85和0.55，而其它参数的分布与文献中最常用的分布保持不变。我们还用每个脉冲星特有的“死亡条件”取代了普遍的“死亡线”。我们发现我们的模型比最流行的模型更好。我们的改进模型，我们预测，全天脉冲星调查与第一阶段SKA-MID将检测到约9000个正常的脉冲星在银河领域。在这些引力波中，有相当一部分将在未来LIGO A $+$等地基引力波探测器的工作范围内产生连续的引力波，在某些情况下，引力波应变的自旋下降极限将远低于探测灵敏度极限。我们还提供了一个适合的自旋周期和1400 MHz的光度分布的整个正常脉冲星人口在银河领域（这是潜在的可观察的），这些可以用于未来的人口研究下的快照方法。
英文摘要：
We revisit the population of normal pulsars in the Galactic field in an `evolutionary' approach. By comparing the distributions of various parameters of synthetic pulsars detectable by the Parkes Multibeam Pulsar Survey, the Pulsar Arecibo L-band Feed Array Survey, and two Swinburne Multibeam surveys with those of the real pulsars detected by the same surveys, we find that a good and physically realistic model can be obtained by using a uniform distribution of the braking index in the range of 2.5 to 3.0, a uniform distribution of the cosine of the angle between the spin and the magnetic axis in the range of 0 to 1, a log-normal birth distribution of the surface magnetic field with the mean and the standard deviation as 12.85 and 0.55 respectively while keeping the distributions of other parameters unchanged from the ones most commonly used in the literature. We have also replaced the universal 'death-line' by a `death-condition' specific to each individual pulsar. We find that our model is better than the most popular model. With our improved model, we predict that an all-sky pulsar survey with phase-I SKA-MID will detect about nine thousand normal pulsars in the Galactic field. Among these pulsars, a considerable number will produce continuous gravitational waves in the operational range of the future ground-based gravitational waves detectors like LIGO A$+$, and in certain cases, the spin-down limit of the gravitational wave strains will be well below the detection sensitivity limit. We also provide a fit for the present-day distributions of the spin periods and 1400 MHz luminosities of the whole normal pulsar population in the Galactic field (which are potentially observable) and those can be used in future population studies under the snapshot approach.
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