We perform magnetohydrodynamic simulations of accreting, equal-mass binary black holes in full general relativity focusing on the impact of black hole spin on the dynamical formation and evolution of minidisks. We find that during the late inspiral the sizes of minidisks are primarily determined by the interplay between the tidal field and the effective innermost stable orbit around each black hole. Our calculations support that a minidisk forms when the Hill sphere around each black hole is significantly larger than the black hole’s effective innermost stable orbit. As the binary inspirals, the radius of the Hill sphere decreases, and minidisks consequently shrink in size. As a result, electromagnetic signatures associated with minidisks may be expected to gradually disappear prior to merger when there are no more stable orbits within the Hill sphere. In particular, a gradual disappearance of a hard electromagnetic component in the spectrum of such systems could provide a characteristic signature of merging black hole binaries. For a binary of given total mass, the timescale to minidisk “evaporation” should therefore depend on the black hole spins and the mass ratio. We also demonstrate that accreting binary black holes with spin have a higher efficiency for converting accretion power to jet luminosity. These results could provide new ways to estimate black hole spins in the future.

我们在完全广义相对论中对吸积等质量双黑洞进行磁流体动力学模拟，重点关注黑洞自旋对微型盘的动力学形成和演化的影响。我们发现，在晚期吸气期间，迷你盘的大小主要取决于潮汐场和每个黑洞周围有效的最内部稳定轨道之间的相互作用。我们的计算表明，当每个黑洞周围的希尔球明显大于黑洞有效的最内部稳定轨道时，就会形成一个迷你盘。随着二元螺旋运动，希尔球的半径减小，小圆盘的尺寸也随之缩小。因此，当希尔球内没有更稳定的轨道时，与迷你盘相关的电磁特征可能会在合并之前逐渐消失。特别是，此类系统频谱中硬电磁成分的逐渐消失可以提供合并黑洞双星的特征签名。因此，对于给定总质量的二进制文件，迷你盘“蒸发”的时间尺度应取决于黑洞自旋和质量比。我们还证明，自旋吸积二元黑洞在将吸积功率转换为喷射光度方面具有更高的效率。这些结果可以为未来估计黑洞自旋提供新的方法。此类系统频谱中硬电磁成分的逐渐消失可以提供合并黑洞双星的特征特征。因此，对于给定总质量的二进制文件，迷你盘“蒸发”的时间尺度应取决于黑洞自旋和质量比。我们还证明，自旋吸积二元黑洞在将吸积功率转换为喷射光度方面具有更高的效率。这些结果可以为未来估计黑洞自旋提供新的方法。此类系统频谱中硬电磁成分的逐渐消失可以提供合并黑洞双星的特征特征。因此，对于给定总质量的二进制文件，迷你盘“蒸发”的时间尺度应取决于黑洞自旋和质量比。我们还证明，自旋吸积二元黑洞在将吸积功率转换为喷射光度方面具有更高的效率。这些结果可以为未来估计黑洞自旋提供新的方法。