Multimessenger observations of double neutron stars in the Galactic disk with gravitational and radio waves
Multimessenger observations of double neutron stars in the Galactic disk with gravitational and radio waves
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DOI：
10.1103/physrevd.107.103035
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发表时间：
2023-05
影响因子：
5
通讯作者：
Wen-Fan Feng;Jie-Wen Chen;Yan Wang;S. Mohanty;Y. Shao
中科院分区：
文献类型：
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作者：
Wen-Fan Feng;Jie-Wen Chen;Yan Wang;S. Mohanty;Y. Shao
我们评估了对银盘中双中子星（DNS）进行无线电跟踪的前景，这些双中子星可以通过未来的星载引力波（GW）探测器进行探测。我们首先根据最近 LIGO 结果的合并率模拟星载引力波探测器可访问的银盘中的 DNS 群体。使用偏心双星的吸气波形，天琴（TQ）、LISA和TQ+LISA可检测到的DNS的平均数量分别为217、368和429。对于TQ+LISA的联合GW检测，基于Fisher信息矩阵，可检测源的参数估计预测精度可以达到$\Delta P_{\mathrm b}/P_{\mathrm b} \lesssim 10^{-6}$、$\Delta \Omega \lesssim 100~{\mathrm {deg}}^2$、$\Delta e/e \lesssim 0.3$的水平，和 $\Delta \dot{P}_{\mathrm b} / \dot{P}_{\mathrm b} \lesssim 0.02$。这些估计精度以信噪比的幂律函数的形式拟合。接下来，我们根据脉冲星束几何形状以及自旋周期和光度的经验分布来模拟这些 DNS 中可能的脉冲星的射电脉冲发射。对于TQ+LISA可检测到的DNS，后续使用Parkes、FAST、SKA1和SKA的脉冲星搜索可检测到的DNS的平均数量分别为8、10、43和87。根据射电望远镜的不同，这些 GW 可探测到的脉冲星双星的平均距离从 1 到 7 kpc 不等。考虑到主要的辐射计噪声和相位抖动噪声，这些引力波可探测脉冲星的定时精度可能低至 70 ${\rm ns}$，而最可能的值约为 100 $\mu {\rm s}$。
We evaluate the prospects for radio follow-up of the double neutron stars (DNSs) in the Galactic disk that could be detected through future space-borne gravitational wave (GW) detectors. We first simulate the DNS population in the Galactic disk that is accessible to space-borne GW detectors according to the merger rate from recent LIGO results. Using the inspiraling waveform for the eccentric binary, the average number of the DNSs detectable by TianQin (TQ), LISA, and TQ+LISA are 217, 368, and 429, respectively. For the joint GW detection of TQ+LISA, the forecasted parameter estimation accuracies, based on the Fisher information matrix, for the detectable sources can reach the levels of $\Delta P_{\mathrm b}/P_{\mathrm b} \lesssim 10^{-6}$, $\Delta \Omega \lesssim 100~{\mathrm {deg}}^2$, $\Delta e/e \lesssim 0.3$, and $\Delta \dot{P}_{\mathrm b} / \dot{P}_{\mathrm b} \lesssim 0.02$. These estimation accuracies are fitted in the form of power-law function of signal-to-noise ratio. Next, we simulate the radio pulse emission from the possible pulsars in these DNSs according to pulsar beam geometry and the empirical distributions of spin period and luminosity. For the DNSs detectable by TQ+LISA, the average number of DNSs detectable by the follow-up pulsar searches using the Parkes, FAST, SKA1, and SKA are 8, 10, 43, and 87, respectively. Depending on the radio telescope, the average distances of these GW-detectable pulsar binaries vary from 1 to 7 kpc. Considering the dominant radiometer noise and phase jitter noise, the timing accuracy of these GW-detectable pulsars can be as low as 70 ${\rm ns}$ while the most probable value is about 100 $\mu {\rm s}$.