of $F_{\rm rad}$ for IMS model ($2\times F_{\rm rad}$ of Case I3). The dashed line is the fake stable layer introduced to prevent the dramatic effects near the upper boundary. The abscissa is the height from bottom $z=(r-r_{\rm b})/d$ for $r\in [r_{\rm b}, r_{\rm b}+d]$, where $d$ is height of the computed zone and $r_{\rm b}$ is the location of the bottom.[]{data-label="init"}](./figures/ini-flx.eps "fig:"){width="8.0cm"}\
![Initial distributions of radiative flux and superadiabatic gradient for intermediate mass star (IMS) model (solid lines) and massive star (MS) model (dotted lines). The MS model is taken from 1D stellar model and the IMS model is constructed according to the 1D stellar model. Case I1, I2 and I3 listed in Table [\[runs\]]{} has the same initial $\Delta\nabla$ and different initial $F_{\rm rad}$. The solid line in upper panel is an example of initial distribution of $F_{\rm rad}$ for IMS model ($2\times F_{\rm rad}$ of Case I3). The dashed line is the fake stable layer introduced to prevent the dramatic effects near the upper boundary. The abscissa is the height from bottom $z=(r-r_{\rm b})/d$ for $r\in [r_{\rm b}, r_{\rm b}+d]$, where $d$ is height of the computed zone and $r_{\rm b}$ is the location of the bottom.[]{data-label="init"}](./figures/ini-sgt.eps 