Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays
A. Sesana, A. Vecchio, M. Volonteri
备注：
12 pages, 10 figures, accepted for publication in MNRAS. Results revised (differences within a factor of two) after a bug in the code for generating the timing residuals has been fixed
Massive black holes are key components of the assembly and evolution of cosmic structures and a number of surveys are currently on-going or planned to probe the demographics of these objects and to gain insight into the relevant physical processes. Pulsar Timing Arrays (PTAs) currently provide the only means to observe gravitational radiation from massive black hole binary systems with masses >10^7 solar masses. The whole cosmic population produces a stochastic background that could be detectable with upcoming Pulsar Timing Arrays. Sources sufficiently close and/or massive generate gravitational radiation that significantly exceeds the level of the background and could be individually resolved. We consider a wide range of massive black hole binary assembly scenarios, we investigate the distribution of the main physical parameters of the sources, such as masses and redshift, and explore the consequences for Pulsar Timing Arrays observations. Depending on the specific massive black hole population model, we estimate that on average at least one resolvable source produces timing residuals in the range ~5-50 ns. Pulsar Timing Arrays, and in particular the future Square Kilometre Array (SKA), can plausibly detect these unique systems, although the events are likely to be rare. These observations would naturally complement on the high-mass end of the massive black hole distribution function future surveys carried out by the Laser Interferometer Space Antenna (LISA)
Millisecond and Binary Pulsars as Nature's Frequency Standards. III. Fourier Analysis and Spectral Sensitivity of Timing Observations to Low-Frequency Noise
Tempo2, a new pulsar timing package. II: The timing model and precision estimates
Tempo 2是一个新的脉冲星脉冲到达时间分析软件包。在本文中，我们详细描述了tempo 2使用的计时模型，并讨论了可达到的精度的限制。除了脉冲星的内在减速行为外，tempo 2还考虑了双星轨道运动、脉冲星或双星系统的长期运动、星际、太阳系和电离层色散、天文台运动（包括地球自转、岁差、章动、极移和轨道运动）、对流层传播延迟以及双星伴星和太阳系天体的引力时间膨胀的影响。我们相信，定时模型是准确的，在其描述的可预测的系统的定时效果优于一纳秒，除了在相对论性的二元系统的情况下，需要进一步的理论发展。潜在误差的最大来源是测量误差、星际散射、太阳系星历误差、原子钟不稳定性和引力波。
Do magnetars glitch? : Timing irregularities in anomalous X-ray pulsars
我们研究了几个反常X射线双星（AXP）的时间历史，发现它们表现出与射电双星相似的自旋不规则性。我们认为这些不规则性只是射电双星的毛刺，并将毛刺自旋降速解拟合到1 E ~2259+586，1 E ~1048.1-5937和4U~0142+61的数据中。推断的大小的毛刺（$ΔΩ$）是可比的，在无线电脉冲星毛刺。这些结果，我们认为，我们研究的三个AXP是孤立的中子星自旋磁偶极子辐射和冷却，磁场衰变和磁层粒子轰击的组合提供动力。
Millisecond and Binary Pulsars as Nature's Frequency Standards. III. Fourier Analysis and Spectral Sensitivity of Timing Observations to Low-Frequency Noise
