论文标题
可能的潮汐消散
Possible tidal dissipation in millisecond pulsar binaries
论文作者
论文摘要
从脉冲星时间定时推论的凯伯利亚后（PK）参数为测试爱因斯坦的一般相对论提供了方便的方法。但是，在获得由重力波辐射引起的纯轨道衰减$ \ dot {p} _b $（这是PK参数之一）之前，需要仔细考虑许多因素。潮汐耗散对$ \ dot {p} _b $的影响被认为可以忽略不计。在这里，我们研究了数据，以了解潮汐耗散对$ \ dot {p} _b $的可能影响。详细研究了潮汐耗散作为$ \ dot {p} _b $的贡献者的可能性。我们用测量的$ \ dot {p} _b $收集了大量的脉冲星二进制文件样本。所有系统都是毫秒的脉冲星。这些系统的残留$ \ dot {p}^{res} _b $是通过减去三种正常效应而获得的，即shklovskii的效果，视线范围的加速度和重力辐射。假设潮汐耗散负责这种残留的$ \ dot {p}^{res} _b $，则可以计算这些系统的潮汐参数，并与潮汐模型进行比较。残留的$ \ dot {p}^{res} _b $分布在一半的正值和一半负数。动力学潮汐模型可以解释毫秒脉冲白dwarf二进制文件的残留$ \ dot {p} _b $。 \ object {psr j1227-4853}的主要序列伴侣的爱情数字可以作为合理的值$ k_2 = 0.177^{+0.098} _ { - 0.058} $，并使用平衡潮汐模型。这些结果与潮汐消散的情况兼容。此外，揭示了潮汐参数和轨道周期之间的弱相关性，这可能起源于回收阶段的潮汐过程，值得进一步研究。
The post-Keplerian(PK) parameters inferred from pulsar timing provide a convenient way to test Einstein's general theory of relativity. However, before obtaining a pure orbital decay $\dot{P}_b$ induced by gravitational wave radiation, which is one of the PK parameters, a number of factors need to be accounted for carefully. The effect of tidal dissipation on $\dot{P}_b$ has been thought of as negligible. Here, we investigate the data for possible effects of tidal dissipation on $\dot{P}_b$. The possibility of the tidal dissipation as a contributor to $\dot{P}_b$ in a large sample of millisecond pulsar binaries is investigated in detail. We collected a large sample of pulsar binaries with measured $\dot{P}_b$. All of the systems are millisecond pulsars. The residual $\dot{P}^{Res}_b$ of these systems was obtained by subtracting the three normal effects, that is to say the effect of Shklovskii, line-of-sight acceleration, and gravitational radiation. Assuming that tidal dissipation is responsible for such a residual $\dot{P}^{Res}_b$, the tidal parameters of these systems can be calculated and compared with the tidal models. The residual $\dot{P}^{Res}_b$ is distributed over the half positive and half negative. The dynamical tidal model can explain the residual $\dot{P}_b$ of millisecond pulsar-white dwarf binaries. And the Love number of the main-sequence companion of \object{PSR J1227-4853} can be derived as a reasonable value $k_2=0.177^{+0.098}_{-0.058}$ with the equilibrium tidal model. Those results are compatible with the scenario of tidal dissipation. Additionally, a weak correlation between the tidal parameter and orbital period is revealed, likely originating in the tidal process of the recycled stage which is worthy of further investigation.
