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For interstitial velocity $u=6U\xi (1-\xi )$, $\xi =z/h$, reflecting transverse walls and molecular diffusion $D$, solve $D{\chi }^{\prime \prime }=u-U$ with zero mean and zero normal derivative. One solution is $\chi =(U{h}^2/D)({\xi }^3-{\xi }^4/2-{\xi }^2/2+1/60)$. Averaging the advection-diffusion equation gives enhancement $-\overline{(u-U)\chi }=D\overline{({\chi }^{\prime }{)}^2}=U^2{h}^2/(210D)$. The approximation requires transverse equilibration and slowly varying longitudinal concentration.

In a steady Keplerian accretion disk with $\Sigma ={\Sigma }_0{R}^{-2}$, $\nu ={\nu }_0{R}^2$, and tracer diffusivity $k=\zeta \nu$, the trace passive scalar concentration obeys the displayed constant-coefficient advection-diffusion equation in logarithmic radius. Contaminant mass is proportional to $CdY$, because $2\pi R\sigma dR=2\pi {\Sigma }_{0}CdY$. A radial impulse $C_0\delta (R-R_0)$ therefore has logarithmic amplitude $C_0/R_0$ and evolves by the Gaussian heat kernel centered at $\ln R_0-vt$. The full-line solution idealizes radii far from the disk boundaries.

For a stationary planar advected magnetic flux potential, average its advection-diffusion equation horizontally and split it into mean and fluctuation. The mean transport is $\overline{w{a}^{\prime }}=\eta {\bar{a}}_z+C$, with $C=⟨w{a}^{\prime }⟩$. Multiplying the fluctuation equation by $a^{\prime }$ and applying integration by parts gives $⟨\overline{w{a}^{\prime }}{\bar{a}}_z⟩+B_{0}C=-\eta ⟨|\nabla a^{\prime }{|}^2⟩$. A vanishing mean derivative removes the constant term in the first correlation, yielding the displayed dissipative identity. The boundary assumptions must eliminate surface terms; a periodic layer replaces, rather than accompanies, decay at vertical infinity.