The interaction of the solar wind with a planetary body results in the creation of a bow shock, where the super-magnetosonic wind is decelerated, compressed and heated. The magnetoplasma then flows around the planet in the magnetosheath, a region highly dynamical, with enough energy to originate various plasma wave modes and structures. Some of these wave modes find their origin in the upstream solar wind, e.g., through upstream ion pick-up (mass-loading). The energisation of the mass-loaded plasma, when it crosses the quasi-perpendicular bow shock (where the interplanetary magnetic field direction is near-perpendicular to the bow shock normal), can lead to the creation of mirror modes in the magnetosheath, whose behaviour is a source of information about energy conversion and plasma wave diffusion from the solar wind to the magnetosphere. In the case of the quasi-parallel bow shock (where the angle between the IMF and the shock normal is less than 45 degrees), downstream localized dynamic pressure enhancements, known as magnetosheath jets, can be formed. These jets can again be the source of other plasma waves in the magnetosheath and have an impact on the magnetopause and magnetosphere. Interestingly, these two structures sometimes seen simultaneously, begging the question if and how they are related.