  The coherent torques between stars on orbits near massive black holes (MBHs)
lead to resonant angular momentum relaxation. Due to the fact that orbits are
Keplerian to good approximation, the torques efficiently change the magnitude
of the angular momenta and rotate the orbital inclinations. As a result the
stars are rapidly randomized. The galactic MBH is a good system for the
observational study of resonant relaxation. The age of the young B-stars at a
distance of $\sim0.01 pc$ from the MBH is comparable to the resonant relaxation
time, implying that resonant relaxation may have played an important role in
their dynamical structure. In contrast, the O-stars in the stellar disks at
$\sim0.1 pc$ are younger than the resonant relaxation time, as required by
their dynamical coherence. Resonant relaxation dynamics dominates the event
rate of gravitational wave (GW) emission from inspiraling stars into MBHs of
masses comparable to the Galactic MBH. Resonant relaxation leads to rates
$\lesssim 10$ times higher than those predicted by 2-body relaxation, which
would improve the prospects of detecting these events by future GW detectors,
such as LISA.
