Gas density in the orbital midplane, showing the hydrodynamic winds generated by a model exoplanet interacting with the stellar wind emanating from the central star. We assume that the observer is located in the direction -x. The white square marks the region around the planet shown in the following figures. The top figure illustrates a planetary wind with isotropic boundary conditions (A_100%), while the bottom figure incorporates day-night anisotropy (A_10%). In the anisotropic scenario, the decreased pressure on the night side leads to a reduction in the mass-loss rate of the planet. As a result, the outflow becomes less extended compared to the isotropic case.