2D slices of the rms normalized vorticity, ﹩\omega /{\langle {\omega }^{2}\rangle }^{1/2}﹩ (ω = ∣∇ × u∣; left in each panel), and baroclinicity (∇ρ × ∇P/ρ²; right in each panel), for 48 randomly selected SNRs extracted from SN-driven turbulence simulations in J. R. Beattie et al. (2025c). The most intense ω regions, which are signatures of incompressible turbulence, correspond to the strongest ∇ρ × ∇P/ρ² structures. The ∇ρ × ∇P/ρ² structures closely trace the corrugated layer between the warm and hot plasma. J. R. Beattie et al. (2025c) find that this layer generates ω values three orders of magnitude larger than any other vorticity source in an SN-driven galactic disk environment. In this study, I show that these layers drive incompressible turbulence with a velocity spectrum ∝k^−3/2, the same spectrum as is found in global SN-driven turbulence simulations of a galactic disk (I. Connor et al. 2026). An animation of this panel with a slider for the vertical bar between the vorticity and baroclinicity can be found at astrojames.github.io/movies/.