在Milky Way中来自孤立中子星的连续引力波的可探测性：粒子数合成方法
Detectability of continuous gravitational waves from isolated neutron stars in the Milky Way: the population synthesis approach
摘要：
目的。我们估计的数量的中子星，可检测的连续引力波源与当前和未来的引力波探测器，假设一个简单的唯象模型的旋转非轴对称的中子星。方法.我们采用了银河系中子星人口的数值模型，与孤立的银河系中子星的射电观测比较建立的属性。我们生成一个任意大的中子星的合成群体，并演化它们的周期、磁场和空间位置。我们使用一个引力波发射模型的基础上指数衰减的椭圆-一个非轴对称的恒星，没有假设的起源给定的椭圆。我们计算了一个给定的检测器的预期信号为1年的观察，并假设检测标准的信噪比为11.4 -相当于一个有针对性的连续波搜索。我们分别分析了每个探测器中可探测到的人口：高级LIGO，高级Virgo和计划中的爱因斯坦望远镜。在计算预期信号时，我们忽略了由于源自旋下降和地球相对于太阳质心的运动而引起的信号频率变化。结果对于中子星演化的保守值：每100年一次的超新星爆发率，初始椭圆率$ε_{0}$ = 1 e-5，没有椭圆率$η$ = $t_\rm{hub}$ = 1 e 4 Myr的衰减，预计探测到的中子星的数量低于1：0.15（基于对10 M恒星的模拟）。参数空间（$ε_{0}$，$η$）的更广泛的研究。根据爱因斯坦望远镜的计划灵敏度，并假设相同的弹性模型，预期的探测数量是：在一年的观测运行中，26.4个双星。
英文摘要：
Aims. We estimate the number of pulsars, detectable as continuous gravitational wave sources with the current and future gravitational-wave detectors, assuming a simple phenomenological model of evolving non-axisymmetry of the rotating neutron star. Methods. We employ a numerical model of the Galactic neutron star population, with the properties established by comparison with radio observations of isolated Galactic pulsars. We generate an arbitrarily large synthetic population of neutron stars and evolve their period, magnetic field, and position in space. We use a gravitational wave emission model based on exponentially decaying ellipticity - a non-axisymmetry of the star, with no assumption of the origin of a given ellipticity. We calculate the expected signal in a given detector for a 1 year observations and assume a detection criterion of the signal-to-noise ratio of 11.4 - comparable to a targeted continous wave search. We analyze the population detectable separately in each detector: Advanced LIGO, Advanced Virgo, and the planned Einstein Telescope. In the calculation of the expected signal we neglect signals frequency change due to the source spindown and the Earth motion with respect to the Solar barycentre. Results. With conservative values for the neutron stars evolution: supernova rate once per 100 years, initial ellipticity $ε_{0}$ = 1e-5 with no decay of the ellipticity $η$ = $t_\rm{hub}$ = 1e4 Myr, the expected number of detected neutron stars is below one: 0.15 (based on a simulation of 10 M stars) for the Advanced LIGO detector. A broader study of the parameter space ($ε_{0}$ , $η$) is presented. With the planned sensitivity for the Einstein Telescope, and assuming the same ellipiticity model, the expected detection number is: 26.4 pulsars during a 1-year long observing run.
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