Where angular momentum goes in a precessing black hole binary
  We evolve a set of 32 equal-mass black-hole binaries with collinear spins
(with intrinsic spin magnitudes $|\vec{S}_{1,2}/m^2_{1,2}|=0.8$) to study the
effects of precession in the highly nonlinear plunge and merger regimes. We
compare the direction of the instantaneous radiated angular momentum,
$\hat{\delta J}_{\rm rad}(t)$, to the directions of the total angular momentum,
$\hat{J}(t)$, and the orbital angular momentum, $\hat{L}(t)$. We find that
$\hat{\delta J}_{\rm rad}(t)$ approximately follows $\hat{L}$ throughout the
evolution. During the orbital evolution and merger, we observe that the angle
between $\vec{L}$ and total spin $\vec{S}$ is approximately conserved to within
$1^\circ$, which allows us to propose and test models for the merger remnant's
mass and spin. For instance, we verify that the \hangup effect is the dominant
effect and largely explains the observed total energy and angular momentum
radiated by these precessing systems. We also verify that the total angular
momentum, which significantly decreases in magnitude during the inspiral,
varies in direction by less than $\sim 5^\circ$. The maximum variation in the
direction of $\vec J$ occurs when the spins are nearly antialigned with the
orbital angular momentum. Based on our results, we conjecture that transitional
precession, which would lead to large variations in the direction of $\vec J$,
is not possible for similar-mass binaries and would require a mass ratio
$m_1/m_2\lesssim1/4$.
