中文摘要：

统计分析了目前发现的几种脉冲星的自转周期和表面磁场以及空间的分布情况，揭示出毫秒脉冲星比普通射电脉冲星、LMXB（低质量X射线双星）比HMXB（高质量X射线双星）的空间分布要更加弥散；孤立毫秒脉冲星自转周期分布的峰值为4．7ms，而普通脉冲星的相应值为0．6S，双星中毫秒脉冲星这一值为3．5ms；FERMI脉冲星（Fermi Gamma-ray Space Telescope发现的伽玛射线脉冲星）和正常脉冲星磁场集中于1012Gs；某些年轻的高能脉冲星与超新星遗迹关联．另外结合脉冲星形成演化模型，对这些分布特点进行了一定的说明．

英文摘要：

The period distribution and surface magnetic field strength distribution of pulsars as well as the spatial distribution of pulsars are analyzed statistically. The spatial distribution of millisecond pulsars is more dispersive than that of normal radio pulsars. And the spatial distribution of low-mass X-ray binary pulsars is also more dispersive than that of high-inass X-ray binary pulsars. The peak values of the rotation period distributions of isolated millisecond pulsars, normal radio pulsars and millisecond pulsars in binaries are 4.7 ms, 0.6 s and 3.5 ms, respectively. The surface magnetic field strengthes of FERMI pulsars （gamma-ray pulsars observed by Large Area Telescope/Fermi Gamma-ray Space Telescope） and normal pulsars all concentrate in 1012 Gs. Combined with the model of the formation and evolution of pulsars, we discuss some characteristics of these distributions. The results show that some young pulsars in the high-energy radiation stage are associated with supernova remnants. This is the direct reflection of the theory that pulsars are formed by supernovae. The results also show that the surface magnetic field strengthes of pulsars change a little in the transformation period from the high-energy 7-ray pulsar stage to the normal radio pulsar stage.