High-accuracy gravitational waveforms for binary black hole mergers with nearly extremal spins
High-accuracy gravitational waveforms for binary black hole mergers with nearly extremal spins
复制标题
具有近极值自旋的双黑洞合并的高精度引力波形
DOI：
10.1088/0264-9381/29/4/045003
复制
发表时间：
2011
影响因子：
3.5
通讯作者：
B. Szilágyi
中科院分区：
文献类型：
--
作者：
G. Lovelace;M. Boyle;M. Scheel;B. Szilágyi
其动机是观察合并黑洞的引力波的可能性，这些黑洞的自旋接近极值（即无量纲单位为1），我们给出了迄今为止模拟的最高自旋黑洞合并的数值波形：（1）25.5轨道的螺旋形，两个质量相等、自旋为0.97的黑洞合并和衰荡与轨道角动量对齐;和（2）先前报道的12.5轨道螺旋，合并和衰荡的两个洞具有相同的质量和0.95级的自旋与轨道角动量反对齐。首先，我们考虑新的对齐自旋模拟的视界质量和自旋演化。在螺旋过程中，视界面积和自旋的演化与阿尔维的分析预测非常接近，而残余黑洞的最终自旋与几个分析预测相当吻合。我们还发现，一个真实的天体物理系统发射的总能量与这些参数-几乎所有的辐射包括在这个模拟的时间-将是10.952%的初始质量在无限的分离。其次，我们考虑两种模拟的重力波形。在估计其不确定性后，我们比较了几个后牛顿近似的波形，发现重大分歧以及合并前，虽然泰勒T4近似的相位恰好同意非常好的数值预测对齐自旋的情况下。我们发现，后牛顿波形有足够的不确定性，杂交波形将需要更长的数值模拟（在没有改进后牛顿波形）的低质量二元系统的精确参数估计。
Motivated by the possibility of observing gravitational waves from merging black holes whose spins are nearly extremal (i.e. 1 in dimensionless units), we present numerical waveforms from simulations of merging black holes with the highest spins simulated to date: (1) a 25.5-orbit inspiral, merger and ringdown of two holes with equal masses and spins of magnitude 0.97 aligned with the orbital angular momentum; and (2) a previously reported 12.5-orbit inspiral, merger and ringdown of two holes with equal masses and spins of magnitude 0.95 anti-aligned with the orbital angular momentum. First, we consider the horizon mass and spin evolution of the new aligned-spin simulation. During the inspiral, the horizon area and spin evolve in remarkably close agreement with Alvi's analytic predictions, and the remnant hole's final spin agrees reasonably well with several analytic predictions. We also find that the total energy emitted by a real astrophysical system with these parameters—almost all of which is radiated during the time included in this simulation—would be 10.952% of the initial mass at infinite separation. Second, we consider the gravitational waveforms for both simulations. After estimating their uncertainties, we compare the waveforms to several post-Newtonian approximants, finding significant disagreement well before merger, although the phase of the TaylorT4 approximant happens to agree remarkably well with the numerical prediction in the aligned-spin case. We find that the post-Newtonian waveforms have sufficient uncertainty that hybridized waveforms will require far longer numerical simulations (in the absence of improved post-Newtonian waveforms) for accurate parameter estimation of low-mass binary systems.
非进动黑洞双星的混合后牛顿/数值相对论波形的 NINJA-2 目录
影响因子：
3.5
作者：
Ajith P
通讯作者：
Ajith P