Directly comparing GW150914 with numerical solutions of Einstein's equations for binary black hole coalescence
Directly comparing GW150914 with numerical solutions of Einstein's equations for binary black hole coalescence
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DOI：
10.1103/physrevd.94.064035
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发表时间：
2016-09-14
影响因子：
5
通讯作者：
Zlochower, Y.
中科院分区：
文献类型：
--
作者：
Abbott, B. P.;Abbott, R.;Zlochower, Y.
我们将GW 150914直接与完全广义相对论中的合并双黑洞模拟进行比较，其中包括专门用于重现这一事件的几个模拟。我们的计算超越了现有的半解析模型，因为对于所有的模拟，包括两个独立的，旋进的自旋源，我们进行比较，占所有的自旋加权四极模式，并分别占所有的四极和八极模式。与Abbott等人[Phys. Rev. Lett. 116，241102（2016）]（在90%的可信水平），我们发现数据与广泛的非旋进和旋进模拟兼容。后续模拟使用先前估计的二进制参数最相似的数据，即使所有的四极和八极模式。仅包括四极模的比较限制了总红移质量M-z epsilon [64 M-圆点- 82 M-圆点]、质量比1/q = m（2）/m（1）epsilon [0.6; 1]以及有效排列自旋chi（eff）epsilon [-0.3，0.2]，其中chi（eff）=（S-1/m（1）+S-2/m（2））。(L)超过上限/M。包括四极和八极模式，我们发现质量比更严格的限制。即使考虑到岁差，在任何质量下，极端质量比和有效自旋的模拟与数据都高度不一致。几个非旋进和旋进模拟具有相似的质量比和chi（eff）是一致的数据。虽然相关，但组件的自旋（幅度和方向）并不受数据的显著约束：数据与组件自旋幅度a（1，2）高达至少0.8的模拟一致，具有随机取向。需要进一步详细的后续计算来确定数据是否包含来自横向（旋进）自旋的弱印记。对于nonprecessing二进制，模拟之间的插值，我们重建后验分布与以前的结果一致。最终黑洞的红移质量在64.0 M圆点-73.5 M圆点范围内与M-f，M-z一致，最终黑洞的无量纲自旋参数与a（f）= 0.62-0.73一致。由于我们的方法调用没有中间近似广义相对论，并可以强烈拒绝二进制的辐射是不一致的数据，我们的分析提供了一个有价值的补充雅培等人。
We compare GW150914 directly to simulations of coalescing binary black holes in full general relativity, including several performed specifically to reproduce this event. Our calculations go beyond existing semianalytic models, because for all simulations-including sources with two independent, precessing spins - we perform comparisons which account for all the spin-weighted quadrupolar modes, and separately which account for all the quadrupolar and octopolar modes. Consistent with the posterior distributions reported by Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016)] (at the 90% credible level), we find the data are compatible with a wide range of nonprecessing and precessing simulations. Follow-up simulations performed using previously estimated binary parameters most resemble the data, even when all quadrupolar and octopolar modes are included. Comparisons including only the quadrupolar modes constrain the total redshifted mass M-z epsilon [64 M-circle dot - 82 M-circle dot], mass ratio 1/q = m(2)/m(1) epsilon [0.6; 1], and effective aligned spin chi(eff) epsilon [-0.3, 0.2] where chi(eff) = (S-1/m(1)+S-2/m(2)). (L) over cap /M. Including both quadrupolar and octopolar modes, we find the mass ratio is even more tightly constrained. Even accounting for precession, simulations with extreme mass ratios and effective spins are highly inconsistent with the data, at any mass. Several nonprecessing and precessing simulations with similar mass ratio and chi(eff) are consistent with the data. Though correlated, the components' spins (both in magnitude and directions) are not significantly constrained by the data: the data is consistent with simulations with component spin magnitudes a(1,2) up to at least 0.8, with random orientations. Further detailed follow-up calculations are needed to determine if the data contain a weak imprint from transverse (precessing) spins. For nonprecessing binaries, interpolating between simulations, we reconstruct a posterior distribution consistent with previous results. The final black hole's redshifted mass is consistent with M-f,M-z in the range 64.0 M-circle dot - 73.5 M-circle dot and the final black hole's dimensionless spin parameter is consistent with a(f) = 0.62-0.73. As our approach invokes no intermediate approximations to general relativity and can strongly reject binaries whose radiation is inconsistent with the data, our analysis provides a valuable complement to Abbott et al.