$\mathcal{O}(G^{2} S^{\infty})$的经典引力自旋-无自旋散射
Classical gravitational spinning-spinless scattering at $\mathcal{O}(G^{2} S^{\infty})$
摘要：
利用最近导出的全自旋反螺旋度康普顿振幅，计算了自旋和无自旋物体在$\mathcal{O}(G^{2})$和自旋各阶的经典引力散射振幅。通过构造，这个振幅展示了描述克尔黑洞的自旋结构。这种自旋结构本身不足以通过接触项来修正康普顿振幅的所有变形，但是当与超相对论极限的考虑相结合时，我们可以唯一地为自旋偶数扇区中剩余的参数赋值。一旦这些参数被确定，振幅的自旋依赖性的大部分归为超几何函数。最后，我们推导出了对准自旋散射的程函相位。
英文摘要：
Making use of the recently-derived, all-spin, opposite-helicity Compton amplitude, we calculate the classical gravitational scattering amplitude for one spinning and one spinless object at $\mathcal{O}(G^{2})$ and all orders in spin. By construction, this amplitude exhibits the spin structure that has been conjectured to describe Kerr black holes. This spin structure alone is not enough to fix all deformations of the Compton amplitude by contact terms, but when combined with considerations of the ultrarelativistic limit we can uniquely assign values to the parameters remaining in the even-in-spin sector. Once these parameters are determined, much of the spin dependence of the amplitude resums into hypergeometric functions. Finally, we derive the eikonal phase for aligned-spin scattering.
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