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Venus’s Turbulent Atmosphere

International research team sheds light on the Earth’s ‘twin planet’

The atmospheric superrotation at the upper clouds of Venus. While the superrotation is present in both day and night sides of Venus, it seems more uniform in the day (AKATSUKI-UVI image at 360 nm, right side), while in the night this seems to become more irregular and unpredictable (composite of Venus Express/VIRTIS images ar 3.8 µm, left). CREDITS: JAXA, ESA, J. Peralta (JAXA) and R. Hueso (UPV/EHU).

Examples of new types of cloud morphology discovered on the night side of Venus thanks to Venus Express (ESA) and the infrared telescope IRTF (NASA): stationary waves (Venus Express, up-left corner), “net” patterns (IRTF, up-right), mysterious filaments (Venus Express, down-left) and dynamical instabilities (Venus Express, down-right). CREDITS: ESA, NASA, J. Peralta (JAXA) and R. Hueso (UPV/EHU).

The mysterious fast filaments as seen on the nightside upper clouds of Venus with the instrument VIRTIS onboard Venus Express. CREDITS: ESA, S. Naito (Acamon), R. Hueso (UPV/EHU) and J. Peralta (JAXA).

A research paper published today by Nature Astronomy sheds light on the so far unexplored nightside circulation at the upper cloud level of Venus. Researchers from the Rhenish Institute for Environmental Research at the University of Cologne are part of an international research project which has now presented its preliminary findings. They discovered unexpected patterns of slow motion and abundant stationary waves in Venus’s nighttime sky. 

Venus is often referred to as Earth's twin because both planets share a similar size and surface composition. Also, they both have atmospheres with complex weather systems. But that is about where the similarities end: Venus is one the most hostile places in our solar system. Its atmosphere consists of 96.5 percent carbon dioxide, with surface temperatures of constantly about 500 degrees Celsius. Venus is a slowly rotating planet – it needs about 243 terrestrial days to complete one rotation. We would expect its atmosphere to rotate with the same rhythm, but in fact it takes only four days. This phenomenon is called superrotation, and it causes substantial turbulences in the planet’s atmosphere. The scientists do not yet fully understand its origin and motor, but are working on an answer to this puzzle. The many waves in the planet's atmosphere may play an important role.

The preliminary research results were generated by an international collaboration headed by the Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA). Experts in space and astronautical science and astrophysics from universities and institutions in Japan, Spain, Italy, and Germany are cooperating in the project. From Germany, the Rhenish Institute for Environmental Research at the University of Cologne and the Center for Astronomy and Astrophysics at the Technical University of Berlin are involved.

The research team analysed data generated by the spacecraft Venus Express to investigate components of Venus’s complex atmosphere, including thermal measurements with regard to horizontal and vertical wave patterns. The data also included first global measurements from the tracking of individual features in thermal emission images at 3.8 and 5.0 µm (micrometer) during 2006–2008 and 2015.

Vertical information in unison with horizontal data help to understand the nature of the observed wave patterns. The vertical information from the VeRa instrument (an atmosphere experiment in Venus Express emits radio waves which the scientists then interpret) could help to identify the observed waves as buoyancy waves. This, in turn, is crucial for the analysis of atmospheric processes. 

Dr. Silvia Tellmann is Vice-Director of the Department of Planetary Research at the Rhenish Institute for Environmental Research at the University of Cologne. She is an expert on the structure, dynamics, and circulation of planetary atmospheres and a co-author of the study. ‘We were able to relate the stationary gravity waves found at higher altitudes with the surface elevations of Venus’, she says. ‘Hence, the waves can be explained with wind currents caused by topographical obstacles. We assume that these stationary waves are substantial for the continuity of the superrotation in the atmosphere of Venus.’

Original Publication:
J. Peralta, R. Hueso, A. Sánchez-Lavega, Y. J. Lee, A. García Muñoz, T. Kouyama, H. Sagawa, T. M. Sato, G. Piccioni, S. Tellmann, T. Imamura & T. Satoh: ‘Stationary waves and slowly moving features in the night upper clouds of Venus.’ Nature Astronomy 1, Article number: 0187 (2017), published online: 24 July 2017, doi: 10.1038/s41550-017-0187

URL: https://www.nature.com/articles/s41550-017-0187

Media Enquiries:
Dr. Silvia Tellmann
Rhenish Institute for Environmental Research, University of Cologne
+49 221 277 8181 3
stellmann(at)uni-koeln.de

Press and Communication Team:
Jürgen Rees
+49 221 470-3107
j.rees(at)uni-koeln.de