Atmospheric waves are a ubiquitous feature on planets with atmospheres in hydrostatic equilibrium. Their spatial scales can range from large Rossby waves of over a thousand Km to small scale ripples with hundreds of meters in length. Many of these features have been studied extensively on Earth which brought a wealth of knowledge into the inner workings of the atmospheric displays. With the advent of space missions capable of taking detailed images and temperature profiles on other planets of the Solar System, it became clear how widespread wave activity is throughout the cosmos. A wave type of particular interest to atmospheric science are internal gravity waves, oscillations in which buoyancy acts as the restoring force in a stably stratified fluid. Although these waves do not seem to have a major impact on the general circulation of the atmosphere, they can be an important driver to many processes that contribute to the momentum budget of atmosphere dynamics. That is because these waves are capable of transporting energy and momentum not only on their specific atmospheric layers (at similar altitudes) but vertically across the atmosphere. On Earth these waves are usually generated by flow over mountains and are a major source of clear air turbulence, driving several processes in the middle atmosphere. Emergent research on these types of features on other planets is now at the forefront of planetary science, particularly for Mars and Venus. However, their characteristics, forcing mechanisms and role in the atmosphere dynamics of their respective planets are still clouded in uncertainty. In this talk, my goal is to present this type of wave activity across the Solar System, with a focus on Venus observations, with an observational analysis of wave activity throughout the thick cloud deck. A thorough categorization of these structures might provide clues to fully understand major dynamical motions of Venus’ atmosphere, such as its superrotation.