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Turbulent convection models are thought to be good tools to deal with theconvective overshooting in the stellar interior. However, they are too complexto be applied in calculations of stellar structure and evolution. In order tounderstand the physical processes of the convective overshooting and tosimplify the application of turbulent convection models, a semi-analyticsolution is necessary.  We obtain the approximate solution and asymptotic solution of the turbulentconvection model in the overshooting region, and find some important propertiesof the convective overshooting:  I. The overshooting region can be partitioned into three parts: a thin regionjust outside the convective boundary with high efficiency of turbulent heattransfer, a power law dissipation region of turbulent kinetic energy in themiddle, and a thermal dissipation area with rapidly decreasing turbulentkinetic energy. The decaying indices of the turbulent correlations $k$,$\bar{u_{r}'T'}$, and $\bar{T'T'}$ are only determined by the parameters of theTCM, and there is an equilibrium value of the anisotropic degree $\omega$.  II. The overshooting length of the turbulent heat flux $\bar{u_{r}'T'}$ isabout $1H_k$($H_k=|\frac{dr}{dlnk}|$).  III. The value of the turbulent kinetic energy at the convective boundary$k_C$ can be estimated by a method called \textsl{the maximum of diffusion}.Turbulent correlations in the overshooting region can be estimated by using$k_C$ and exponentially decreasing functions with the decaying indices.

Turbulent convection model in the overshooting region: II. Theoretical analysis