银河系孤立老中子星的空间和速度分布
Space and velocity distributions of Galactic isolated old Neutron stars
摘要：
本文介绍了银河系中子星的Monte-Carlo轨道模拟结果。模拟考虑到最新观察到的NS空间和速度分布在出生时，并考虑其形成率。我模拟了两个NS群体。在过去的12 Gyr中，第一批天体以恒定的速度在银河系圆盘中诞生。那些在第二个人口同时形成12 Gyr前在银河系的隆起。我假设出生在银河系圆盘的NS占总NS人口的40%。由于NS的初始速度分布并不为人所知，我运行了两组模拟，每组包含3x10^6个模拟NS。一组采用双峰初速度分布，另一组采用单峰初速度分布，这两种分布都是基于卫星观测而提出的。根据最近的观测结果，本文讨论了银河系结构的动力加热对NS空间和速度分布的影响，并指出它是可以忽略的。我呈现了当前纪元模拟NS空间和速度矢量的目录，以及模拟NS相对于太阳的位置、距离和自行的目录。假设银河系中有10^9个NS，我发现在太阳附近NS的密度约为2- 4x 10 ^-4 pc^-3，它们的标度高度约为0.3-0.6 kpc（取决于所采用的初速度分布）。这些星表可以用来检验某些射电瞬变与这些天体有关的假设。
英文摘要：
I present the results of Monte-Carlo orbital simulations of Galactic Neutron Stars (NSs). The simulations take into account the up-to-date observed NS space and velocity distributions at birth, and account for their formation rate. I simulate two populations of NSs. Objects in the first population were born in the Galactic disk at a constant rate, in the past 12 Gyr. Those in the second population were formed simultaneously 12 Gyr ago in the Galactic bulge. I assume that the NSs born in the Galactic disk comprise 40% of the total NS population. Since the initial velocity distribution of NSs is not well known, I run two sets of simulations, each containing 3x10^6 simulated NSs. One set utilizes a bimodal initial velocity distribution and the other a unimodal initial velocity distribution, both are advocated based on pulsars observations. In light of recent observational results, I discuss the effect of dynamical heating by Galactic structure on NS space and velocity distributions and show it can be neglected. I present catalogue of simulated NS space and velocity vectors in the current epoch, and catalogue of positions, distances and proper motions of simulated NSs, relative to the Sun. Assuming there are 10^9 NSs in the Galaxy, I find that in the solar neighborhood the density of NSs is about 2-4x10^-4 pc^-3 and their scale height is about 0.3-0.6 kpc (depending on the adopted initial velocity distribution). These catalogue can be used to test the hypothesis that some radio transients are related to these objects.
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