Gravito-turbulent bi-fluid protoplanetary discs - I. An analytical perspective to stratification

Open Access

Fig. 4

Comparison between the numerical solution of Eq. (19) and our approximated solution (Eq. (22)) for different Toomre parameters of gas $($ Q_{g}^{3 D} $)$ $(\$ Q_g^{3D}\$ )$ , dust $($ Q_{d}^{3 D} $)$ $(\$ Q_d^{3D}\$ )$ , and relative effective gas-to-dust temperature $(\tilde{ξ})$ ${\rm{(}}\widetilde \xi {\rm{)}}$ . Top: Vertical profile of gas density. Bottom: L2 norm error map in log₁₀ scale.

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