AI 中文总结
本研究构建长周期射电暂现源合成星表，估计LISA四年内可探测到约0.05%至6%的这类源，其频率、振幅和天区位置的测量精度满足需求，可为射电巡天及双星本质验证提供支持。
AI 中文摘要
近期发现的长周期射电暂现源代表了一类令人困惑的新型天体物理源，其中部分被认为是每轨道周期发射一次脉冲的致密双星系统。若该解释正确，轨道周期（进而引力波频率）直接编码在射电信号中，这类信号通常处于毫赫兹频段。本研究探讨这类系统能否被激光干涉空间天线（LISA）探测到。假设射电脉冲与轨道运动之间的相位锁定关系广泛存在于这类源的总体中，我们结合观测数据和相关系统（如激变变星）的理论模型构建了合成源星表。根据不同的天体物理假设，我们估计在四年观测期内，约0.05%至6%的长周期暂现源可被LISA探测到。对于可探测系统，我们发现注入频率的恢复精度可达约10^5分之一，振幅误差在约2倍以内，天区位置误差在约30平方度以内。我们的结果表明，引力波观测可为这类源的双星本质提供直接证据，且重要的是，可通过预测脉冲周期、天区位置和轨道性质来指导未来的射电巡天。我们还计算了提取的频率导数与引力波衰减所要求的频率导数之间的失配，以评估每个可探测候选体中电动力损失驱动轨道演化的可能性。
英文摘要
The recently-discovered long-period radio transients represent a puzzling new class of astrophysical sources, some of which are thought to be compact binary systems emitting a pulse once per orbit. If this interpretation is correct, the orbital period--and therefore the gravitational-wave frequency--is directly encoded in the radio signal, which typically lies in the millihertz band. In this work, we explore whether these systems can be detected by the Laser Interferometer Space Antenna (LISA). Assuming that this phase-locking between radio pulses and orbital motion applies broadly across the population, we construct synthetic source catalogues informed by both observations and theoretical models of related systems, such as cataclysmic variables. We estimate that between $\sim 0.05\%$ and $\sim 6\%$ of long-period transients will be detectable within four years of observation with LISA, depending on astrophysical assumptions. For detectable systems, we find injected frequencies are recoverable to one part in $\sim 10^{5}$, amplitudes to within a factor $\sim 2$, and the sky positions to within $\sim$30 square degrees. Our results demonstrate that gravitational-wave observations can provide direct evidence for the binary nature of these sources and, importantly, can guide future radio surveys by predicting pulse periods, sky positions, and orbital properties. The mismatch between extracted frequency derivatives and that imposed by gravitational-wave decay is also computed to show that the likelihood of electromotive losses driving orbital evolution can be assessed for each detectable candidate.
Comments16 pages, 11 figures, 2 tables. Accepted for publication in A&A
