Accretion disks around kicked black holes: Post-kick Dynamics
  Numerical calculations of merging black hole binaries indicate that
asymmetric emission of gravitational radiation can kick the merged black hole
at up to thousands of km/s, and a number of systems have been observed recently
whose properties are consistent with an active galactic nucleus containing a
supermassive black hole moving with substantial velocity with respect to its
broader accretion disk. We study here the effect of an impulsive kick delivered
to a black hole on the dynamical evolution of its accretion disk using a
smoothed particle hydrodynamics code, focusing attention on the role played by
the kick angle with respect to the orbital angular momentum vector of the
pre-kicked disk. We find that for more vertical kicks, for which the angle
between the kick and the normal vector to the disk $\theta\lesssim 30^\circ$, a
gap remains present in the inner disk, in accordance with the prediction from
an analytic collisionless Keplerian disk model, while for more oblique kicks
with $\theta\gtrsim 45^\circ$, matter rapidly accretes toward the black hole.
There is a systematic trend for higher potential luminosities for more oblique
kick angles for a given black hole mass, disk mass and kick velocity, and we
find large amplitude oscillations in time in the case of a kick oriented
$60^\circ$ from the vertical.
