Boyle Latham, Kesden Michael, Nissanke Samaya
Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, 60 St. George Street, Toronto, Ontario, Canada.
Phys Rev Lett. 2008 Apr 18;100(15):151101. doi: 10.1103/PhysRevLett.100.151101. Epub 2008 Apr 17.
We regard binary-black-hole (BBH) merger as a map from a simple initial state (two Kerr black holes, with dimensionless spins a and b) to a simple final state (a Kerr black hole with mass m, dimensionless spin s, and kick velocity k). By expanding this map around a=b=0 and applying symmetry constraints, we obtain a simple formalism that is remarkably successful at explaining existing BBH simulations. It also makes detailed predictions and suggests a more efficient way of mapping the parameter space of binary black-hole merger. Since we rely on symmetry rather than dynamics, our expansion complements previous analytical techniques.
我们将双黑洞（BBH）合并视为一种从简单初始状态（两个克尔黑洞，无量纲自旋分别为a和b）到简单最终状态（一个质量为m、无量纲自旋为s且具有反冲速度k的克尔黑洞）的映射。通过在a = b = 0附近展开此映射并应用对称性约束，我们得到了一种简单的形式体系，它在解释现有的双黑洞模拟方面非常成功。它还做出了详细的预测，并提出了一种更有效的方法来映射双黑洞合并的参数空间。由于我们依赖对称性而非动力学，我们的展开补充了先前的分析技术。
