  Linear damping rates of radial oscillation modes in selected $Kepler$ stars
are estimated with the help of a nonadiabatic stability analysis. The
convective fluxes are obtained from a nonlocal, time-dependent convection
model. The mixing-length parameter is calibrated to the surface-convection-zone
depth of a stellar model obtained from fitting adiabatic frequencies to the
LEGACY observations, and two of the three nonlocal convection parameters are
calibrated to the corresponding LEGACY linewidth measurements. The atmospheric
structure in the 1D stability analysis adopts a temperature-optical-depth
relation derived from 3D hydrodynamical simulations. Results from 3D
simulations are also used to calibrate the turbulent pressure and to guide the
functional form of the depth-dependence of the anisotropy of the turbulent
velocity field in the 1D stability computations.
