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The vertical shear instability (VSI) is a promising mechanism to driveturbulence in protoplanetary disks. Numerical simulations in literaturedemonstrate that the VSI non-linear saturation is predominated by the linearcorrugation modes. These modes possess vertical wavelengths significantlylonger than radial wavelengths. This paper aims to investigate the naturalradial wavelengths of corrugation modes upon saturation, by a series ofnumerical simulations conducted in Athena++ at different grid resolutions, diskaspect ratios, and viscosity. We find a continuous reduction of radialwavelengths with grid resolution and a sign of convergence at 64 cells perscale height for fiducial models. Synthetic ALMA molecular line observations of$^{12}$CO(2-1) are performed to inspect the observability of corrugation modesfeature, where it is washed out at above 32 cells per scale height. Flared andviscous disks that exhibit longer saturation wavelengths may mitigate theobservation difficulty.

A resolution study on corrugation mode wavelengths of vertical shear instability