  We investigate the dynamical evolution of an intermediate mass black hole
(IMBH) in a nuclear star cluster hosting a supermassive black hole (SMBH) and
both a spherical and a flattened disk-like distribution of stellar-mass
objects. We use a direct N-body ($\varphi$GPU) and an orbit-averaged (N-ring)
numerical integrator to simulate the orbital evolution of stars and the IMBH.
We find that the IMBH's orbit gradually aligns with the stellar disk if their
mutual initial inclination is less than 90 degrees. If it is larger than 90
degrees, i.e. counterrotating, the IMBH does not align. Initially, the rate of
orbital reorientation increases linearly with the mass of the IMBH and it is
orders of magnitude faster than ordinary (i.e. Chandrasekhar) dynamical
friction. The semimajor axes of the IMBH and the stars are approximately
conserved. This suggests that the alignment is predominantly driven by
orbit-averaged gravitational torques of the stars, a process which may be
called resonant dynamical friction. The stellar disk is warped by the IMBH, and
ultimately increases its thickness. This process may offer a test for the
viability of IMBH candidates in the Galactic Center. Resonant dynamical
friction is not limited to IMBHs; any object much more massive than disk
particles may ultimately align with the disk. This may have implications for
the formation and evolution of black hole disks in dense stellar systems and
gravitational wave source populations for LIGO, VIRGO, KAGRA, and LISA.
