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Galactic winds play a crucial role in the ejection of the interstellar medium(ISM) into intergalactic space. This study presents a model that classifiespossible transonic solutions of galactic winds in the gravitational potentialof the dark matter halo and stellar component under spherically symmetric andsteady assumptions. Our model includes injections of mass and energy resultingfrom supernovae feedback along a flow line. The mass flux in galactic winds isa critical factor in determining the acceleration process of the flow andrevealing the impact of galactic winds on galaxy evolution. We apply thetransonic galactic wind model to the observed outflow velocities ofstar-forming galaxies to estimate the mass flux. Dividing the mass flux by thestar formation rate (SFR) yields the mass loading rate (and mass loadingfactor), which indicates the entrainment effect of the ISM by the hot gas flow.Our results demonstrate that the mass loading rate is inversely correlated withgalaxy mass and SFR. In less massive galaxies (stellar mass $\sim 10^{7-8}M_\odot$), the mass loading rate exceeds unity, indicating effective ejectionof the ISM into intergalactic space. However, in massive galaxies (stellar mass$\sim 10^{10-11} M_\odot$), the mass loading rate falls below unity, meaningthat the mass flux cannot exceed the injected mass by supernovae, thusresulting in the ineffective ejection of the ISM.

Transonic galactic wind model including stellar feedbacks and application to outflows in high/low-$z$ galaxies