Here we have a binary black hole system (BHBH) in a quasi-equilibrium circular orbit. This is puncture BHBH initial data, evolved with the BSSN formulation. The primary black hole has a spin that is aligned with its angular momentum axis, and the secondary black hole has a spin that is anti-aligned with respect to this axis. $S_1$ and $S_2$ are defined as $S_1/{M_1}^2 = a_1/M_1$ and $S_2/{M_2}^2 = a_2/M_2$. The mass of the primary black hole is $M_1 = 36 M_{\odot}$ and the mass of the secondary black hole is $M_2 = 29 M_{\odot}$, which gives a mass ratio of $M_{1}/M_{2} = 1.24$. We define M to be the ADM mass at the initial time which is $M = M_{ADM}(0) = 65 M_{\odot}$. Similarly, we define $J = J_{ADM}(0)$, where $J/M^{2} = 0.949$.
Fig. 1-1: Initial Configuration |
Fig. 1-2: Initial Masses |
Fig. 1-3: Initial Spins |
The initial and final spins are indicated by the green arrows, and are normalized to their dimensionless values. The binary makes approximately six orbits prior to merging after $t \approx 280 \; ms$. As the binary merges, we see the formation of a common horizon, which oscillates until settling down at $t \approx 300 \; ms$. The simulation continues until $t = 366 \; ms$ to demonstrate the stability of the resulting Kerr black hole. The arrow at the end of the visualization indicates the direction of the final angular momentum, and is scaled to the dimensionless angular momentum, $J_{BH}/{M_{BH}}^2$.
Fig. 1-2: Binary Black Holes at time t = 0 ms |
Fig. 1-2: Binary Black Holes at time t = 265 ms |
Fig. 1-2: Binary Black Holes at time t = 366 ms |
Quantity | Dimensionless Value |
$M_{BH}/M$ | 0.95 |
$J_{BH}/M^2$ | 0.686 |
$\Delta E_{GW}/M$ | 0.040 |
$\Delta J_{GW}/M^2$ | 0.399 |
$\delta E \equiv (M-M_{BH}- \Delta E_{GW})/M$ | $4.37 \times 10^{-4}$ |
$\delta J \equiv (J-J_{BH}- \Delta J_{GW})/J$ | $-8.13 \times 10^{-2}$ |
Our simulation maintains good conservation of energy and momentum, since $\delta E$ and $\delta J$ are on the order of $10^{-4}$ and $10^{-2}$, respectively.