Table 5: Best parameters of the RT models, shown in Figs. 18-22. The dust shell was confined to end at a radius of $10^4~R_{\rm i}$.

T*a		 $T_{\rm dust}$b Comp. $\tau_{8.0, 9.8, 13.~\mu {\rm m}}$ $R_{\rm i}$c $L_{*,~{\rm bol}}$d
[kK] [kK]     [AU/mas/Ri/*] $[ L_\odot ]$

3		 1.2 amCe 0.8, 0.6, 0.4 35/5/10 $5\times 10^4$
3 1.2 Silf 1, 6, 1.7 40/5/10 $5\times 10^4$
25 1.2 amCe 0.8, 0.6, 0.4 60/8/1000 $5\times 10^4$
25 1.2 Silf 0.8, 4.9, 1.3 115/15/2000 $5\times 10^4$
a T* denotes the stellar effective temperature. b  $T_{\rm dust}$ is the dust temperature at the sublimation zone, visible as ring of radius $R_{\rm i}$ in Fig. 22. c  $R_{\rm i/*}$ is the size ratio of the stellar and dust sublimation radius $R_{\rm i}$. d  $L_{*,~{\rm bol}}$ labels the bolometric luminosity of the embedded star. e 100% amorphous Carbon grains (Hanner 1988). f 100% warm amorphous silicate grains (Ossenkopf et al. 1992).


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