To understand the dynamical structures of stellar wind bubble, one and two-dimensional calculations has been performed. Using FCT Code with cooling effects and assuming constant mass loss rate and ambient medium density, we could divide stellar winds into the regime of slow and fast winds. The slow wind driven bubble shows initially radiative and becomes partially radiative bubble in which shocked stellar wind zone is still adiabatic. In contrast., the fast wind driven bubble shows initially fully adiabatic and becomes adiabatic bubbles with radiative outer shell. We also determine analytically the onset of thin-shell formation time in case of fast wind driven bubble with power-law energy injection and ambient density structure. We solve the line transfer problem with numerical results in order to calculate line profile of [OIII] forbidden line.

The proposed evaporation disk model is improved to figure out two flow system ~n the observed bipolar molecular outflow and stellar optical jet. Using the improved model, we can interpret the dymanical interactions of the two flows as well as obtain the physical parameter distributions along the flows Numerical & analytical adiabatic hydrodynamic calculations of the stellar jet inside show that the jet Mach number increases with an inversely proportional to the jet radius and M₁∼35, V₁∼150㎞/sec, Z₁∼0.1 pc, R₁∼0.05pc, T₁∼10³K, ρ₁-4.3×10^(-3)g/㎤(n₁∼25/㎤) at the end of the flow. By the way, in the case of the molecular flow. which is developed from the evaporated disk wind, the same calculations show that the flow Mach number increases with an inversely proportional to the mass flux distribution and M_d∼15, V₁∼15㎞/sec, Z_d∼1pc, R_d∼025pc, T_d∼10²K, ρ_d∼4.0×10^(-3)g/㎤(n_d∼25/㎤) at the flow end Most of the calculated physical parameters in the two flows consistent with the observational ones very well. The theoretically calculated flows develope the supersonic flows to make the shocked regions at the ends of flows. These regions are gravitationally unstable to produced the fragmentations whose masses are∼2 M- in the stellar let case and 0.3 M_⊙ in the bipolar flow case. This mass distribution supports that both the origins of Herbig-Haro objects and the birth of low mass stars are attributed to the instabilities of the shocked regions in the stellar jets and the bipolar molecular flows respectively.