标题： 后牛顿精确的旋转型致密双星在偏心轨道中的动力学参数解：一级自旋-轨道相互作用 显示英文标题

标题： Post-Newtonian accurate parametric solution to the dynamics of spinning compact binaries in eccentric orbits: The leading order spin-orbit interaction

摘要： 我们为后牛顿（PN）精确的自旋致密双星在偏心轨道上运动的保守动力学解推导出类似开普勒的参数化方法。我们考虑的PN精确动力学包括由一阶自旋效应引起的第三后牛顿精确保守轨道动力学，即一阶自旋-轨道相互作用。表示的轨道元素以守恒的轨道能量、角动量和一个在阿诺维特、德瑟和米斯纳型坐标中表征一阶自旋-轨道相互作用的量来明确给出。我们的参数解适用于以下两种不同的情况：(i) 双星由质量相等的致密天体组成，具有两个任意自旋；(ii) 双星由任意质量的致密天体组成，其中只有一个具有任意自旋。作为我们参数化的应用，我们给出了引力波极化，其振幅限制在一阶四极矩阶次，适合描述自旋致密双星在偏心轨道上运动产生的引力辐射。目前的参数化将用于构建用于自旋致密双星在 inspiralling 偏心轨道中引力波的“即用型”参考模板。我们对自旋致密双星的后牛顿精确保守动力学的参数解清楚地表明，在所考虑的情况下，这些系统中没有混沌。最后，我们注意到，我们的参数化是推导一个完全二阶后牛顿精确“定时公式”的第一步，这可能对像J0737-3039这样的相对论性双脉冲星的射电观测有用。 显示英文摘要

摘要： We derive Keplerian-type parametrization for the solution of post-Newtonian (PN) accurate conservative dynamics of spinning compact binaries moving in eccentric orbits. The PN accurate dynamics that we consider consists of the third post-Newtonian accurate conservative orbital dynamics influenced by the leading order spin effects, namely the leading order spin-orbit interactions. The orbital elements of the representation are explicitly given in terms of the conserved orbital energy, angular momentum and a quantity that characterizes the leading order spin-orbit interactions in Arnowitt, Deser, and Misner-type coordinates. Our parametric solution is applicable in the following two distinct cases: (i) the binary consists of equal mass compact objects, having two arbitrary spins, and (ii) the binary consists of compact objects of arbitrary mass, where only one of them is spinning with an arbitrary spin. As an application of our parametrization, we present gravitational wave polarizations, whose amplitudes are restricted to the leading quadrupolar order, suitable to describe gravitational radiation from spinning compact binaries moving in eccentric orbits. The present parametrization will be required to construct `ready to use' reference templates for gravitational waves from spinning compact binaries in inspiralling eccentric orbits. Our parametric solution for the post-Newtonian accurate conservative dynamics of spinning compact binaries clearly indicates, for the cases considered, the absence of chaos in these systems. Finally, we note that our parametrization provides the first step in deriving a fully second post-Newtonian accurate `timing formula', that may be useful for the radio observations of relativistic binary pulsars like J0737-3039.