Atmospheric tidal waves maintain Venus’s super-rotation

Images from the Akatsuki spacecraft unveil why Venus’s atmosphere rotates much faster than its surface.

This story is featured in the Asia Research News 2021 magazine. Read in ISSUU (above) or full text and images below

Venus rotates very slowly, taking 243 Earth days to rotate once around its axis. Its thick atmosphere, however, rotates 60 times faster, taking only 96 hours to whip around the entire planet.

“The super-rotation of Venus’s atmosphere was discovered in the 1960s, but the mechanism behind its formation and maintenance has been a long-standing mystery,” says atmospheric scientist Takeshi Horinouchi of Hokkaido University.

Horinouchi and his colleagues from Japan’s Institute of Space and Astronautical Science and other institutes have solved a key part of the puzzle.

Venus’s cloud layer is the fastest moving section of its atmosphere, racing around the equator at 360 kilometres/ hour (224 miles/hr). To move so much faster than the planet, the atmosphere needs to generate enough angular momentum to overcome friction caused by the planet’s surface, even at the top of the cloud layer 70km (42mi) above the surface.

Others have theorized that turbulence and waves within the atmosphere provide the needed angular momentum. Horinouchi and his colleagues found that they do play important roles, but the most critical factor for maintaining super-rotation has to do with heat.

Since the planet rotates so slowly, Venus’s dayside faces the sun for months (in Earth time), getting very hot. At the equator, the heat warms and pushes the atmosphere towards the planet’s much cooler nightside, creating a powerful thermal tide. This tidal wave provides the necessary force to keep the atmosphere moving so fast.

North and south of the equator, another circulation pattern pushes warm air towards the poles, distributing both heat and angular momentum. The interaction between the two circulations helps reinforce the thermal tide, propelling it in a westward direction, even despite turbulence and other waves working against it. Besides providing the angular momentum needed for super-rotation, the dual circulation system also helps even out temperatures across the planet.

The findings, reported in the journal Science, are thanks to the Akatsuki spacecraft, which began its orbit of Venus in December 2015. Using images provided by Akatuski’s ultraviolet and infrared cameras, the researchers were able to develop a new, highly precise method to track clouds and derive wind velocities. This allowed them to estimate the contributions of atmospheric waves and turbulence to super-rotation.

“Our study could help us better understand atmospheric systems on tidally-locked exoplanets with one side always facing a central star, which is similar to Venus’s very long solar day,” Horinouchi says.

The proposed system that maintains the super-rotation (yellow) of Venus’s atmosphere. The atmosphere is controlled by a dual circulation system: a vertical circulation (white) that slowly transports heat towards the poles and the super-rotation that rapidly transports heat towards the planet’s nightside. The thermal tide (red) on either side of the equator forces the super-rotation in a westward direction.

Did you know?:

  • Venus is one of two planets in our solar system that rotate ‘backwards’, from east to west. Uranus is the other. The atmosphere on Venus moves in the same direction, but 60 times faster than the planet. 
  • Venus has the longest day of any planet in our solar system. One day is longer than its entire year!
  • With an axil tilt of only three degrees, Venus spins nearly upright and so does not experience noticeable seasons.

Further information

Professor Takeshi Horinouchi
[email protected]
Faculty of Environmental and Earth Science
Hokkaido University

Published: 14 May 2021


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News topics: 

Horinouchi, T., Hayashi, Y-Y., Watanabe, S., Yamada, M., Yamazaki, A. et al. How waves and turbulence maintain the super-rotation of Venus’ atmosphere. Science