The Pulsar kick velocity distribution
The Pulsar kick velocity distribution
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DOI：
10.1093/mnras/291.3.569
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发表时间：
1997-08
影响因子：
4.8
通讯作者：
B. Hansen;E. T. H. C. F. Astrophysics;U. Toronto;T. Astrophysics;C. I. O. Technology.
中科院分区：
文献类型：
--
作者：
B. Hansen;E. T. H. C. F. Astrophysics;U. Toronto;T. Astrophysics;C. I. O. Technology.
我们分析了脉冲星自行的样本，详细考虑了原始调查的选择效应。我们使用生存统计数据来处理审查数据。通过将我们的结果与蒙特卡罗模拟进行比较，我们发现脉冲星的平均诞生速度为 250-300 km/s，而不是 Lyne & Lorimer (1994) 发现的 450 km/s。所得分布与色散 $ \sigma_v = 190 km/s$ 的麦克斯韦分布一致。尽管诞生速度很大，我们发现具有长特征年龄的脉冲星表现出不对称漂移，表明它们是动态老化的。这些脉冲星可能是由年轻群体的低速尾部产生的，尽管它们的双星起源和银河系潜力的演化对其进行了修改。
We analyse the sample of pulsar proper motions, taking detailed account of the selection effects of the original surveys. We treat censored data using survival statistics. From a comparison of our results with Monte Carlo simulations, we find that the mean birth speed of a pulsar is 250-300 km/s, rather than the 450 km/s foundby Lyne & Lorimer (1994). The resultant distribution is consistent with a maxwellian with dispersion $ \sigma_v = 190 km/s$. Despite the large birth velocities, we find that the pulsars with long characteristic ages show the asymmetric drift, indicating that they are dynamically old. These pulsars may result from the low velocity tail of the younger population, although modified by their origin in binaries and by evolution in the galactic potential.