  Stars embedded in active galactic nucleus (AGN) disks or captured by them may
scatter onto the supermassive black hole (SMBH), leading to a tidal disruption
event (TDE). Using the moving-mesh hydrodynamics simulations with {\small
AREPO}, we investigate the dependence of debris properties in in-plane TDEs in
AGN disks on the disk density and the orientation of stellar orbits relative to
the disk gas (pro- and retro-grade). Key findings are: 1) Debris experiences
continuous perturbations from the disk gas, which can result in significant and
continuous changes in debris energy and angular momentum compared to `naked'
TDEs. 2) Above a critical density of a disk around a SMBH with mass
$M_{\bullet}$ ($\rho_{\rm crit} \sim 10^{-8}{\rm
g~cm^{-3}}(M_{\bullet}/10^{6}{\rm M}_{\odot})^{-2.5}$) for retrograde stars,
both bound and unbound debris is fully mixed into the disk. The density
threshold for no bound debris return, inhibiting the accretion component of
TDEs, is $\rho_{\rm crit,bound} \sim 10^{-9}{\rm
g~cm^{-3}}(M_{\bullet}/10^{6}{\rm M}_{\odot})^{-2.5}$. 3) Observationally,
AGN-TDEs transition from resembling naked TDEs in the limit of $\rho_{\rm
disk}\lesssim 10^{-2}\rho_{\rm crit,bound}$ to fully muffled TDEs with
associated inner disk state changes at $\rho_{\rm disk}\gtrsim\rho_{\rm
crit,bound}$, with a superposition of AGN+TDE in between. Stellar or remnant
passages themselves can significantly perturb the inner disk. This can lead to
an immediate X-ray signature and optically detectable inner disk state changes,
potentially contributing to the changing-look AGN phenomenon. 4) Debris mixing
can enriches the average disk metallicity over time if the star's metallicity
exceeds that of the disk gas.
