  Advances in time domain astronomy have produced a growing population of
flares from galactic nuclei, including both tidal disruption events (TDEs) and
flares in active galactic nuclei (AGN). Because TDEs are uncommon and AGN
variability is abundant, large-amplitude AGN flares are usually not categorized
as TDEs. While TDEs are normally channelled by the collisional process of
two-body scatterings over relaxation timescale, the quadrupole moment of a gas
disk alters the stellar orbits, allowing them to collisionlessly approach the
central massive black hole (MBH). This leads to an effectively enlarged loss
cone, the \emph{loss wedge}. Earlier studies found a moderate enhancement, up
to a factor $\sim 2-3$, of TDE rates $\dot{N}_{\rm 2b} $ for a static
axisymmetric perturbation. Here we study the loss wedge problem for an evolving
AGN disk, which can capture large number of stars into the growing loss wedge
over much shorter times. The rates $\dot{N}_{\rm cl}$ of collisionless TDEs
produced by these time-evolving disks are much higher than the collisional
rates $\dot{N}_{\rm 2b}$ in a static loss wedge. We calculate the response of a
stellar population to the axisymmetric potential of an adiabatically growing
AGN disk and find that the highest rates of collisionless TDEs are achieved for
the largest (i) MBH masses $M_{\bullet}$ and (ii) disk masses $M_{\rm d}$. For
$M_{\bullet}\sim 10^7 M_\odot$ and $M_{\rm d} \sim 0.1 M_{\bullet}$, the rate
enhancement can be up to a factor $\dot{N}_{\rm cl}/\dot{N}_{\rm 2b} \sim 10$.
The orbits of collisionless TDEs sometimes have a preferred orientation in
apses, carrying implications for observational signatures of resulting flares.
