P-Pdot图上孤立脉冲星的自旋演化
Isolated pulsar spin evolution on the P-Pdot Diagram
摘要：
我们看两个对比的自旋模型孤立的无线电卫星，占选择效应，合成可观察到的人口。虽然我们的目标是再现所有可观察到的特征，但在本文中，我们特别注意自旋周期与周期导数（P-Pdot）图的形式及其对各种脉冲星性质的依赖性。我们分析了脉冲星的初始自旋周期、制动指数、磁场、各种聚束模型以及光度。除了考虑脉冲星自旋下降的标准磁偶极子模型外，我们还考虑了Contopoulos和Spitkovsky最近提出的混合模型。然而，磁偶极子模型在再现观测到的脉冲星数量方面做得更好。我们得出结论，随机排列角度和周期依赖的光度分布是必不可少的重现所观察到的P-Pdot图。我们还考虑了对准角的时间衰减，并试图调和目前正在研究的各种模型。我们的结论是，为了解释最近的证据，由Weltevrede和Johnston发现的对齐，制动扭矩的中子星不应该强烈依赖于倾角。我们的模拟代码是可访问的，包括一个基于Web的界面，以检查结果，并预测当前和未来的调查产量。
英文摘要：
We look at two contrasting spin-down models for isolated radio pulsars and, accounting for selection effects, synthesize observable populations. While our goal is to reproduce all of the observable characteristics, in this paper we pay particular attention to the form of the spin period vs. period derivative (P-Pdot) diagram and its dependence on various pulsar properties. We analyse the initial spin period, the braking index, the magnetic field, various beaming models, as well as the pulsar's luminosity. In addition to considering the standard magnetic dipole model for pulsar spin-down, we also consider the recent hybrid model proposed by Contopoulos & Spitkovsky. The magnetic dipole model, however, does a better job of reproducing the observed pulsar population. We conclude that random alignment angles and period dependent luminosity distributions are essential to reproduce the observed P-Pdot diagram. We also consider the time decay of alignment angles, and attempt to reconcile various models currently being studied. We conclude that, in order to account for recent evidence for the alignment found by Weltevrede & Johnston, the braking torque on a neutron star should not depend strongly on the inclination. Our simulation code is publically available and includes a web-based interface to examine the results and make predictions for yields of current and future surveys.
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