论文标题
中子星的初始时间和磁场
Initial periods and magnetic fields of neutron stars
论文作者
论文摘要
脉冲星周期和磁场的初始分布是多种现代天体物理模型的重要组成部分。没有做足够的工作来使用直接测量来正确限制这些分布。在这里，我们的目标是通过严格分析与超新星残留物相关的年轻中子星的特性来填补这一空白。为了执行此任务，我们编制了56个中子星的目录，与已知年龄估计的超新星残留物唯一配对。此外，我们使用多种统计技术分析了该目录。我们发现，使用对数正态分布很好地描述了无线电脉冲星的磁场和周期的分布。平均磁场为$ \ log_ {10} [b/\ mathrm {g}] = 12.44 $，标准偏差为$σ_b= 0.44 $。磁铁和中央紧凑型物体不会遵循相同的分布。平均初始时间为$ \ log_ {10} p_0 [p / \ mathrm {s}] = -1.04 _ { - 0.2}^{+0.15} $，标准偏差为$σ_p= 0.53 _ { - 0.08}^{ - 0.08}^{+0.12} $。我们表明，正态分布不能很好地描述中子星的初始周期。初始周期分布的参数对制动指数的确切值不敏感。
Initial distributions of pulsar periods and magnetic fields are essential components of multiple modern astrophysical models. Not enough work has been done to properly constrain these distributions using direct measurements. Here we aim to fill this gap by rigorously analysing properties of young neutron stars associated to supernova remnants. In order to perform this task, we compile a catalogue of 56 neutron stars uniquely paired to supernova remnants with known age estimate. Further, we analyse this catalogue using multiple statistical techniques. We found that distribution of magnetic fields and periods for radio pulsars are both well described using the log-normal distribution. The mean magnetic field is $\log_{10} [B/\mathrm{G}] = 12.44$ and standard deviation is $σ_B = 0.44$. Magnetars and central compact objects do not follow the same distribution. The mean initial period is $\log_{10} P_0 [P / \mathrm{s}] = -1.04_{-0.2}^{+0.15}$ and standard deviation is $σ_p = 0.53_{-0.08}^{+0.12}$. We show that the normal distribution does not describe the initial periods of neutron stars sufficiently well. Parameters of the initial period distribution are not sensitive to the exact value of the braking index.
