AI 中文总结
研究白矮星-致密天体双星末期阶段，开发新型积分器，探讨引力波参数趋势，指出银河系外双星难被现有探测器测量，此类双星末期阶段是未来十分之一赫兹探测器重要来源，其最高频率无法模拟相关信号。
AI 中文摘要
我们通过开发一种实现质量转移和2.5阶后牛顿运动学的新型积分器，研究了圆形白矮星-致密天体双星的末期阶段。白矮星-致密天体双星经历两个阶段：一个缓慢的螺旋进动阶段，期间双星演化由弱引力辐射反应主导，以及一个由质量转移主导的更快的“螺旋出”阶段。这些系统具有独特的引力波波形，有几个特征，包括在螺旋进和螺旋出过渡设定的最大截止频率附近信号的积累。我们研究了基于组成质量的引力波参数趋势。特别是，最大截止频率强烈依赖于白矮星质量和致密性。银河系外双星不太可能被LISA或当前或未来的地面探测器测量。然而，白矮星-致密天体双星末期阶段将是未来如DECIGO和LGWA等十分之一赫兹探测器的重要来源：LGWA每年将探测到数十个白矮星-中子星双星的最终螺旋进，DECIGO将探测到数百万个螺旋进以及数千个螺旋出。这些双星的最终命运多种多样，取决于角动量损失的复杂性。特别是，我们表明，与质量足够低/高的伴星的白矮星可以在共同包层/合并中结束生命，而白矮星与中等质量的伴星不会接触。我们测试中白矮星-致密天体双星产生的最高频率为10-20Hz，无法在地面探测器中模拟亚太阳质量致密天体信号或解释类似S251112cm的信号。
英文摘要
We investigate the end stages of circular white-dwarf--compact-object binaries by developing a novel integrator implementing mass transfer and 2.5-order Post-Newtonian kinematics. White-dwarf--compact-object binaries are subject to two phases: a slow inspiral during which binary evolution is dominated by weak-gravity radiation reaction and a quicker ``outspiral" dominated by mass transfer. These systems have unique gravitational waveforms with several characteristic features including an accumulation of signal near the maximum cutoff frequency set by the transition between in- and outspiral. We investigate trends in gravitational wave parameters based on component masses. In particular, maximum cutoff frequency depends strongly on white dwarf mass and compactness. It is unlikely that extragalactic binaries will be measured by LISA or current or future terrestrial detectors. However, white-dwarf--compact-object binary end stages will be an important source for future decihertz detectors such as DECIGO and LGWA: The final inspiral of tens of white-dwarf--neutron-star binaries will be detected annually by LGWA, and millions of inspirals along with thousands of outspirals will be detected by DECIGO. The ultimate fates of these binaries are diverse and dependent upon the intricacies of angular momentum loss. In particular, we show that white dwarfs with partners of sufficiently low/high mass can end their lives in common envelopes/mergers, while white dwarfs do not enter contact with partners of intermediate mass. The highest frequencies produced by white-dwarf--compact-object binaries in our tests are 10--20 Hz---incapable of mimicking sub-solar-mass compact object signals in terrestrial detectors or explaining S251112cm-like signals.
Comments19 pages, 9 figures
