  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.
