论文标题
绝热顺序的赤道平面上的极高质量比灵感
Extreme mass ratio inspirals on the equatorial plane in the adiabatic order
论文作者
论文摘要
我们从巨大旋转黑洞（BH）的赤道平面上的灵感恒星质量紧凑物体计算重力波。我们的灵感轨道是通过考虑重力辐射在质量比的最低顺序上的绝热变化来计算的。我们采用一种插值方法来计算预先计算出的轨道参数空间区域内的任意点的绝热变化。使用获得的灵感轨道和相关的引力波，我们计算重力波和信噪比（SNR）的功率光谱（SNR），用于BH旋转的几个值，二进制的质量以及在最终plunge之前假设的三元丽莎观察过程中的初始轨道偏心。我们发现（i）SNR随着BH的旋转和BH质量$ M \ agt 10^6m_ \ odot $的增加而增加，（ii）SNR的最大值为$ m \ 10^6m_ \ odot $，而（iii）SNR随着$ m = 10^6m = 10^6m = 10^6m = 10^6m_的初始偏心增加而增加。我们还表明，结合较高的重力波模式的贡献对于提高检测率至关重要。
We compute gravitational waves from inspiraling stellar-mass compact objects on the equatorial plane of a massive spinning black hole (BH). Our inspiral orbits are computed by taking into account the adiabatic change of orbital parameters due to gravitational radiation in the lowest order in mass ratio. We employ an interpolation method to compute the adiabatic change at arbitrary points inside the region of orbital parameter space computed in advance. Using the obtained inspiral orbits and associated gravitational waves, we compute power spectra of gravitational waves and the signal-to-noise ratio (SNR) for several values of the BH spin, the masses of the binary, and the initial orbital eccentricity during a hypothetical three-yrs LISA observation before final plunge. We find that (i) the SNR increases as the BH spin and the mass of the compact object increase for the BH mass $M \agt 10^6M_\odot$, (ii) the SNR has a maximum for $M \approx 10^6M_\odot$, and (iii) the SNR increases as the initial eccentricity increases for $M=10^6M_\odot$. We also show that incorporating the contribution from the higher multipole modes of gravitational waves is crucial for enhancing the detection rate.
