准椭圆轨道上的第三类后牛顿angular momentum通量和吸气紧双星轨道根数的长期演化
Third post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact binaries in quasi-elliptical orbits
摘要：
利用多极后闵可夫斯基波生成方法计算了在准椭圆轨道上运动的紧凑天体的螺旋双星系统的角动量通量。3PN角动量通量包括瞬时、尾和尾中尾对3PN能通量的贡献，此外还有非线性记忆的贡献。我们平均的角动量通量的二进制的轨道使用3PN准开普勒表示的椭圆轨道。平均角动量通量提供了在准椭圆轨道上运动的双星的引力波定相所需的最终输入。在准椭圆情形下，得到了3PN引力辐射反应下轨道根数的演化。对于小的偏心率，我们给出了简单的限制表达式有关逐步阶$e^2$。这项工作是很重要的准偏心双星的模板建设，并为后牛顿的结果与数值相对论模拟的暴跌和合并的偏心双星的比较。
英文摘要：
The angular momentum flux from an inspiralling binary system of compact objects moving in quasi-elliptical orbits is computed at the third post-Newtonian (3PN) order using the multipolar post-Minkowskian wave generation formalism. The 3PN angular momentum flux involves the instantaneous, tail, and tail-of-tails contributions as for the 3PN energy flux, and in addition a contribution due to non-linear memory. We average the angular momentum flux over the binary's orbit using the 3PN quasi-Keplerian representation of elliptical orbits. The averaged angular momentum flux provides the final input needed for gravitational wave phasing of binaries moving in quasi-elliptical orbits. We obtain the evolution of orbital elements under 3PN gravitational radiation reaction in the quasi-elliptic case. For small eccentricities, we give simpler limiting expressions relevant for phasing up to order $e^2$. This work is important for the construction of templates for quasi-eccentric binaries, and for the comparison of post-Newtonian results with the numerical relativity simulations of the plunge and merger of eccentric binaries.
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