1. Key points
For the first time, the distribution of wind speeds at the altitude of the clouds on Venus (Note 1) has been measured over both the day and night, providing an understanding of the mechanism for the high-speed atmospheric circulation and the average north-south circulation (Fig. 1).
It has been a 40 year mystery how the flow patterns on the cloud tops of Venus behaved during the night. Now, it has been revealed that a north-south wind moving in the opposite direction to that in the day is generated at night (Fig. 2).
Understanding the atmospheric circulation on a slow-rotating planet engulfed in thick clouds--a very different environment from that on Earth-will lead to the elucidation of the mechanisms that create diverse environments on terrestrial planets.
Venus hosts a fast easterly wind across the entire planet known as "super-rotation" (Note 2) that is not seen on Earth. In addition to this, the movement of clouds in the daytime observed in ultraviolet light flow from the equator towards both poles. However, it has been a mystery for 40 years how much of this second poleward flow is due to Hadley circulation (Note 3) and how much is due to winds peculiar to the thermal tides (Note 4).
A research group led by Kiichi Fukuya, a master's student at the University of Tokyo's Graduate School of Science, and Professor Takeshi Imamura of the University of Tokyo's Graduate School of Frontier Science, along with researchers from the University of Tokyo, Rikkyo University, Japan Aerospace Exploration Agency (JAXA) and other institutions, succeeded in visualizing the motion of the clouds covering Venus over both the day and night by analyzing infrared images captured by JAXA's Venus Climate Orbiter, Akatsuki (Note 5) (Fig. 1). This revealed that there was a nighttime flow towards the equator that was in the opposite direction to the motion during the day, clarifying the role of thermal tides (Fig. 2). The discovery also offers insight into the mechanism that drives super-rotation and the morphology of the Hadley circulation. Understanding how the atmospheric environment on Venus is maintained is a key factor in elucidating how planets differentiate into a variety of environments, and to understand conditions on planets with super-rotating atmospheres that are thought to be numerous outside the Solar System.
3. Research description:
Venus is a planet that is a similar size to the Earth, with a dense atmosphere that is composed mainly of carbon dioxide with clouds of sulfuric acid at high altitudes. A 100 m/s global westward wind, known as super-rotation, whips around the cloud tops at an altitude of 65 km. Investigating the mechanics of an atmosphere that is very different from that on Earth allows insight into the processes that led to the creation of the different environments on each planet. In recent years, a number of planets with high altitude cloud cover, and planets whose atmospheres are thought to be super-rotating, have been discovered outside the Solar System. Venus is therefore attracting attention as a reference celestial body for researching conditions on these exoplanets.
The motion of the Venusian atmosphere has previously been estimated principally from a series of images of the clouds illuminated by the solar UV light during the day. The UV illuminates shades in the clouds corresponding to variations in chemical composition, which allows the clouds to be identified and tracked. This tracking revealed that in addition to the super-rotation, motion of the atmosphere of Venus includes a flow of about 10 m/s from the equator to both poles. At the time of its discovery about 40 years ago, this poleward flow was ascribed to Hadley circulation, a global atmospheric circulation in which atmosphere heated by sunlight at the equator rises and flows towards high latitudes. However, it has been pointed out in recent years that this motion also includes a contribution from thermal tides; a fluid wave caused by atmospheric heating by sunlight. The respective contributions from each mechanism has not been well understood.
The Hadley circulation is the mean flow of the north-south winds during both the day and the night, while the thermal tides will be the origin of the difference between those two times. Hadley circulation and thermal tides are the two main atmospheric phenomena that are caused by the clouds that cover the entirety of Venus receiving sunlight. The Hadley circulation is responsible for the circulation of energy and matter, while the thermal tides may affect the maintenance of super-rotation. Understanding the Venusian atmosphere requires the mechanics of these two phenomena to be understood and that made it necessary to observe the planet's day and night to capture the global structure.
The best way to monitor the motion of the clouds at night is to look at the infrared emitted by the clouds and track differences in cloud top temperature between locations. But the entirety of Venus has never previously been continuously photographed in the infrared, and a clear pattern in the infrared could not be seen. This research used cloud image data acquired approximately every hour for two years with the LIR thermal imaging camera onboard Japan's Venus Climate Orbiter, Akatsuki. In order to distinguish between temperature variations and noise, the noise was reduced by superimposing and averaging multiple images shifted to account for the movement of clouds due to the super-rotation of the atmosphere (Fig. 3). With this step, small temperature fluctuations in the cloud top of about 0.3℃ could be seen, allowing the movement of the atmosphere to be visualized (animations 1 & 2).
The resultant analysis revealed a flow in the nighttime cloud tops from both poles to the equator, contrary to that in the daytime. The motion occurred at the same speed as the daytime's reverse flow, resulting in almost no net north-south circulation when averaged over the day and night (Fig. 1 & 2). The equatorward flow at night was found to occur mainly from sunset to midnight. The velocity structure of the thermal tide was clarified for the first time based on the difference in the wind velocities with time. The thermal tide contains a large contribution from a periodic wave that includes two cycles in the east-west direction (semidiurnal tide) and transmits a force in the altitude direction (transporting the east-west momentum in the altitude direction), suggesting that this helps to maintain super-rotation. (Fig. 4).
The fact that the average north-south circulation is nearly zero at the cloud top suggests that the polewards flow of the Hadley circulation is higher than the cloud top and then the returning flow towards the equator is in the cloud layer below the cloud top. In-between altitudes at the cloud top, the north-south flow appears to be weak. It was previously thought that the sulfuric acid clouds were mainly created in the equatorial region and transported polewards, but in fact most of the clouds may be carried from high latitudes by the flow returning towards the equator. Such circulation patterns also has a significant impact on the circulation of energy throughout the atmosphere and the fluid dynamics that maintain the super-rotation.
Now that the structure of the Hadley circulation and thermal tide are known, future studies using numerical simulations of Venus's atmospheric physics can target reproducing these results. Additionally, the ability to observe the distribution of Venus's wind and cloud top temperatures over both the day and night has opened the possibility of tracking temporal changes due to different atmospheric phenomena, bringing a new method to Venus meteorology. The response of the atmospheric dynamics to the solar heating of the cloud layer revealed in this work is expected to play an important role in the atmospheres of other planets, such as generating super-rotation in the atmospheres of exoplanets. Further understanding can be achieved through collaborations between meteorology in the Solar System and the exoplanet science.
Journal name: Nature
Paper Title: The nightside cloud-top circulation of the atmosphere of Venus
Authors: Kiichi Fukuya*, Takeshi Imamura*, Makoto Taguchi, Tetsuya Fukuhara, Toru Kouyama, Takeshi Horinouchi, Javier Peralta, Masahiko Futaguchi, Takeru Yamada, Takao M. Sato, Atsushi Yamazaki, Shin-ya Murakami, Takehiko Satoh, Masahiro Takagi, Masato Nakamura
(Note 1) Venus
Venus is a planet with a rocky surface (terrestrial planet) and is the Earth's neighbor towards the Sun in our Solar System. The size and density of Venus are close to that of the Earth. The planet is the brightest object in the sky after the Sun and Moon, earning it the name "morning star" or "evening star". Due to the greenhouse effect resulting from a dense atmosphere rich in carbon dioxide, the temperature on the surface of the planet reaches about 460℃. Clouds of sulfuric acid exist at altitudes of 50 ~ 70km. The planet's rotation is extremely slow, with a rotation period of 243 days. However, the atmosphere moves around Venus in just 40 days, due to the high-speed easterly wind. The rapid wind speed compared to the planet's rotation is a phenomenon known as 'super-rotation'.
(Note 2) Super-rotation
A phenomenon in which the atmosphere of the planet circulates more rapidly than the planet rotates over a wide range in latitudes that includes the equator. On Venus, such winds are found at all latitudes, with the wind speed increasing with altitude from the surface and reaching a maximum speed of 100 m/s near the cloud-top region at an altitude of 70km. This is very different from winds on Earth, and the mechanism that causes such speeds is not well understood. Similar winds can be seen on Saturn's moon, Titan, and observations have pointed to the existence of super-rotation on exoplanets.
(Note 3) Hadley circulation
Because the planet equator receives the most solar energy, the atmosphere becomes warmer near the equatorial region and is cooler at higher latitudes. In an attempt to eliminate this temperature difference, warm atmosphere rises close to the equator and flows in the upper atmosphere towards higher latitudes, before cooling and descending in the higher latitude regions to cycle back through the lower atmosphere to the equator. This kind of circulation is called the Hadley circulation and on Earth, operates between the equator and a latitude of about 30°. On Venus, the Hadley circulation is expected to occur near the cloud tops and near the planet surface which are heated by sunlight, but unlike on the Earth, the circulation can extend from the equator to high latitudes. Hadley circulation occurs simultaneously to the east-west wind (super-rotation on Venus) and in the same location, but it generally the much slower of the two.
(Note 4) Thermal tide
Planetary atmospheres are heated by sunlight at a location directly below the Sun's position, which moves relative to the atmosphere at the planet rotates and the atmosphere circulates to cause planetary-scale fluid waves. Such a wave is known as a thermal tide and is widely observed on Earth and Mars, in addition to Venus. Thermal tides propagate both in the east-west and vertical direction, transferring momentum between different altitudes and accelerating/decelerating the average east-west wind. Unlike the so-called tide, the attraction of other celestial bodies such as the Moon is irrelevant to the thermal tide.
(Note 5) Akatsuki
Japan's Venus Climate Orbiter, Akatsuki, was launched in May 2010 and entered orbit around Venus in December 2015, after a five year delay due to trouble with the propulsion system en route to Venus. The orbiter is a meteorological satellite of Venus and performs continuous imaging observations of the atmosphere using five cameras that take images at different wavelengths from orbit. Akatsuki also conducts observations of the Venusian atmosphere using communication radio waves between its antenna and the Earth. Project website: https://akatsuki.isas.jaxa.jp/en/
6. Research group
Kiichi Fukuya（At the time: Department of Earth and Planetary Science, The University of Tokyo, Current：Tokyo Software & Systems Development Laboratory, IBM Japan）
Takeshi Imamura（Department of Complexity Science and Engineering, Graduate School of Frontier Sciences/ Department of Earth and Planetary Science, University of Tokyo）
Masato Nakamura (Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency）