  We present a new method for replacing the outermost layers of stellar models
with interpolated atmospheres based on results from 3D simulations, in order to
correct for structural inadequacies of these layers. This replacement is known
as patching. Tests, based on 3D atmospheres from three different codes and
interior models with different input physics, are performed. Using solar
models, we investigate how different patching criteria affect the
eigenfrequencies. These criteria include the depth, at which the replacement is
performed, the quantity, on which the replacement is based, and the mismatch in
$T_\mathrm{eff}$ and $\log g$ between the un-patched model and patched 3D
atmosphere. We find the eigenfrequencies to be unaltered by the patching depth
deep within the adiabatic region, while changing the patching quantity or the
employed atmosphere grid leads to frequency shifts that may exceed
$1\,\mu\mathrm{Hz}$. Likewise, the eigenfrequencies are sensitive to mismatches
in $T_\mathrm{eff}$ or $\log g$. A thorough investigation of the accuracy of a
new scheme, for interpolating mean 3D stratifications within the atmosphere
grids, is furthermore performed. Throughout large parts of the atmosphere
grids, our interpolation scheme yields sufficiently accurate results for the
purpose of asteroseismology. We apply our procedure in asteroseismic analyses
of four \textit{Kepler} stars and draw the same conclusions as in the solar
case: Correcting for structural deficiencies lowers the eigenfrequencies, this
correction is slightly sensitive to the patching criteria, and the remaining
frequency discrepancy between models and observations is less
frequency-dependent. Our work shows the applicability and relevance of patching
in asteroseismology.
