Modeling the outflow of planetary atmospheres is important for understanding the evolution of exoplanet systems and for interpreting their observations. Modern theoretical models of exoplanet atmospheres become increasingly detailed and multicomponent, and this makes difficulties for engaging new researchers in the scope. Here, for the first time, we present the results of testing the gas-dynamic method incorporated in our aeronomic model, which has been proposed earlier. Undertaken tests support the correctness of the method and validate its applicability. For modeling the planetary wind, we propose a new hydrodynamic model equipped with a phenomenological function of heating by stellar UV radiation. The general flow in this model well agrees with results obtained in more detailed aeronomic models. The proposed model can be used for both methodical purposes and testing the gas-dynamic modules of self-consistent chemical-dynamic models of the planetary wind.
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