论文标题
了解正常脉冲星的银河系种群：飞跃
Understanding the Galactic population of normal pulsars: A leap forward
论文作者
论文摘要
我们以“进化”方法重新审视银河系中正常脉冲星的种群。通过比较可以通过Parkes Multibeam Pulsar调查可检测到的合成PULSAR的各种参数的分布，脉冲星arecibo l频段饲料阵列调查以及两次Swinburne多峰调查与由同一调查检测到的真实脉冲的分布，我们发现，我们发现使用良好和物理模型的模型可以通过2.使用范围的范围2.在0到1的范围内，自旋和磁轴之间的角度的余弦的均匀分布，表面磁场的对数正态分出生分别具有平均值和标准偏差为12.85和0.55，同时保持与文献中最常用的参数的分布不变的其他参数的分布。我们还通过特定于每个脉冲星的“死亡条件”代替了普遍的“死亡线”。我们发现我们的模型比最受欢迎的模型更好。借助我们改进的模型，我们预测一项具有I期SKA-MID的全套脉冲星调查将在银河系中检测到大约9000个正常脉冲星。在这些脉冲星中，大量数量将在未来的地面重力波探测器（如Ligo a $+$）的操作范围内产生连续的重力波，并且在某些情况下，重力波菌株的旋转极限将远低于检测敏感性极限。我们还为银河场中整个正常脉冲星人群的自旋时期和1400 MHz发光度（可能可观察到）的当今分布提供了适合，并且可以在快照方法中使用这些分布。
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.
