Pulsar Statistics – III. Neutron Star binaries
Pulsar Statistics – III. Neutron Star binaries
复制标题
脉冲星统计 – III。
DOI：
10.1093/mnras/276.1.347
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发表时间：
1995
影响因子：
4.8
通讯作者：
D. Lorimer
中科院分区：
文献类型：
--
作者：
S. Curran;D. Lorimer
我们使用银河系脉冲星群体的详细计算机模拟来估计银河系中中子星-中子星(NS-NS)双星的数量。我们的计算是基于这一类的三个已知系统，PSR B1534+12，B1913+16和B2303+46，并使用了覆盖大片天空的灵敏脉冲星观测的最新结果。我们估计在银河系中有∼240个潜在可观测的NS-NS双星。由于B1534+12和B1913+16最终将在已知的时间尺度上由于引力辐射的发射而合并，我们可以推导出NS-NS双星的星系合并率ℛ，我们估计ℛ∼为10-7年-1。考虑到影响NS-NS系统数量的几个因素，我们得到了更现实的标称值ℛ∼3╳10-6年-1。因此，我们必须将目光投向远离银河系的GPC范围，才能看到每年几次NS-NS恒星合并。下一代引力波探测器的灵敏度预计将接近探测到如此远的距离所需的灵敏度。
We use a detailed computer simulation of the galactic pulsar population to estimate the number of neutron star–neutron star (NS–NS) binaries in the Galaxy. Our calculations are based on the three known systems of this class, PSRs B1534+12, B1913+16 and B2303+46, and use the latest results from sensitive pulsar surveys covering a large area of sky. We estimate that there are ∼240potentially observableNS–NS binaries in the Galaxy. As B1534+12 and B1913+16 will eventually merge due to the emission of gravitational radiation in a known time-scale, we can deduce the galactic merging rate ℛ of NS–NS binaries; we estimate ℛ ∼10–7yr–1. Taking account of several factors which affect the number of NS–NS systems that can be detected, we arrive at a more realistic nominal value ofℛ ∼ 3 ╳ 10–6yr–1. Thus we have to look far beyond the Galaxy to the Gpc range in order to witness several NS–NS star mergings per year. The next generation of gravitational wave detectors are expected to have sensitivities approaching that required to probe to such distances.