1. LESIA, Observatoire de Paris, Université Pierre et Marie Curie, CNRS, Paris 7, Meudon F-92195, France
2. Departments of Earth and Planetary Sciences & Physics and Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA
3. NASA/Goddard Space Flight Center, Code 693, Greenbelt, Maryland 20771, USA

Correspondence to: T. Fouchet¹ Correspondence and requests for materials should be addressed to T.F. (Email: thierry.fouchet@obspm.fr).

The middle atmospheres of planets are driven by a combination of radiative heating and cooling, mean meridional motions, and vertically propagating waves (which originate in the deep troposphere). It is very difficult to model these effects and, therefore, observations are essential to advancing our understanding of atmospheres. The equatorial stratospheres of Earth and Jupiter oscillate quasi-periodically on timescales of about two and four years, respectively, driven by wave-induced momentum transport^{1, 2, 3, 4, 5}. On Venus and Titan, waves originating from surface–atmosphere interaction and inertial instability are thought to drive the atmosphere to rotate more rapidly than the surface (superrotation). However, the relevant wave modes have not yet been precisely identified. Here we report infrared observations showing that Saturn has an equatorial oscillation like those found on Earth and Jupiter, as well as a mid-latitude subsidence that may be associated with the equatorial motion. The latitudinal extent of Saturn's oscillation shows that it obeys the same basic physics as do those on Earth and Jupiter. Future highly resolved observations of the temperature profile together with modelling of these three different atmospheres will allow us determine the wave mode, the wavelength and the wave amplitude that lead to middle atmosphere oscillation.

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