钟比法在脉冲星定时观测中的应用
Applying clock comparison methods to pulsar timing observations
摘要：
频率计量在精度（$10^{-16}$中的部分）和小波动（$<10^{-17}$）方面优于任何其他计量分支。反过来，在天体中，毫秒双星（MSP）的旋转速度是迄今为止最稳定的（$<10^{-18}$）。因此，脉冲星信号到达时间（TOA）的精确测量有望揭示宇宙学现象的信息，并扩大我们的天体物理知识。与此相关的是，脉冲星定时阵列（PTA）项目已经开发和运行了几十年。脉冲星的到达时间会受到局部辐射和环境效应的影响，在通过星际介质的传播方向上，或者普遍受到超大质量黑洞双星的引力波的影响。这些效应（信号）可以表现为随时间的低频波动，在现象上类似于红噪声。而其余的脉冲星固有和仪器背景（噪声）是白色的。本文主要讨论频率计量问题。从我们的观点来看，脉冲星是一个精确的时钟，可以用几个望远镜同时测量，以排除不相关的白噪声。我们应用现代统计方法的时间和频率计量的模拟脉冲星数据，我们显示的相关红噪声信号的望远镜之间的检测极限。
英文摘要：
Frequency metrology outperforms any other branch of metrology in accuracy (parts in $10^{-16}$) and small fluctuations ($<10^{-17}$). In turn, among celestial bodies, the rotation speed of millisecond pulsars (MSP) is by far the most stable ($<10^{-18}$). Therefore, the precise measurement of the time of arrival (TOA) of pulsar signals is expected to disclose information about cosmological phenomena, and to enlarge our astrophysical knowledge. Related to this topic, Pulsar Timing Array (PTA) projects have been developed and operated for the last decades. The TOAs from a pulsar can be affected by local emission and environmental effects, in the direction of the propagation through the interstellar medium or universally by gravitational waves from super massive black hole binaries. These effects (signals) can manifest as a low-frequency fluctuation over time, phenomenologically similar to a red noise. While the remaining pulsar intrinsic and instrumental background (noise) are white. This article focuses on the frequency metrology of pulsars. From our standpoint, the pulsar is an accurate clock, to be measured simultaneously with several telescopes in order to reject the uncorrelated white noise. We apply the modern statistical methods of time-and-frequency metrology to simulated pulsar data, and we show the detection limit of the correlated red noise signal between telescopes.
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