Deep, Dynamic Currents Revealed by Venus Express and Akatsuki
Venus’ appearance is deceptive. The history of scientific research about Venus is full of mistaken assumptions that are sooner or later refuted by new observations. Ancient civilizations wrongly interpreted the morning and evening stars as 2 stars. Giovanni Cassini claimed to have observed moons. More recently, scientists assumed that Venus’ reflective clouds prevented solar energy from reaching its surface, leaving it cold. Its surface is actually hotter than Mercury’s surface. Even today, sophisticated numerical models that work to predict the behavior of atmospheres on other planets are unable to reproduce even basic properties of the atmosphere of Venus.
Consider one particular mystery. Why, when Venus is the slowest-rotating planet in the solar system, does its atmosphere whirl around it at 300 kilometers (200 miles) per hour, 60 times faster than the planet’s spin? Understanding this atmospheric superrotation has become a more urgent goal in recent decades because it also happens on Titan and even in exoplanetary atmospheres, especially those tidally locked to their stars.
Akatsuki Views Venus
Seen in natural color, Venus is as featureless as a cue ball. In ultraviolet wavelengths, a mysterious atmospheric component absorbs sunlight, outlining patterns in Venus’ clouds. Like a weather satellite, Japan’s Akatsuki orbiter swings far from Venus on each 10-day orbit and watches the clouds move through cameras that see in ultraviolet, visible, and infrared wavelengths.
More than 20 space missions visited Venus from 1962 to 1999, but there was a long gap in orbital missions after NASA’s Magellan entered the atmosphere in 1994. Finally, in 2006, European Space Agency’s Venus Express arrived, initiating 2 decades of breakthroughs in Venus science. Venus Express carried 5 instruments that could measure the temperature of the atmosphere from 40 to 170 kilometers (25 to 106 miles) above the surface. Two of them, the Venus Monitoring Camera (VMC) and the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS), were able to take images of Venus at different wavelengths and thus observe the atmosphere at different vertical levels from the surface up to about 120 kilometers (75 miles). The mission operated for 9 years until contact was lost in November 2014.
Japan Space Exploration Agency’s Akatsuki launched in 2010 to join Venus Express at Venus, targeting an equatorial orbit in 2010 to complement Venus Express’ polar one. Unfortunately, an obstruction in a valve caused Akatsuki’s main engine to break during its orbital insertion attempt. The spacecraft continued in a solar orbit. There followed an epic recovery effort using the spacecraft’s maneuvering thrusters, and Akatsuki successfully entered orbit on 7 December 2015 and is still operating. While Venus Express’ scientific goals were wide ranging, Akatsuki’s goals focus primarily on the conundrum of superrotation. Therefore, Akatsuki’s payload is mainly composed of cameras (the ultraviolet camera UVI and the infrared cameras IR1 and IR2) whose different filters observe the morphology and dynamics of clouds at multiple levels.
Emily Lakdawalla and Loren A. Roberts for The Planetary Society
Probing Venus' atmosphere
Venus Express orbited Venus from 11 April 2006 to 18 January 2015. Its Venus Monitoring Camera (VMC) had 4 ultraviolet to infrared filters that enabled it to probe from the surface to an altitude of 70 kilometers (43 miles), above the clouds. Its Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) had hundreds of channels and saw all levels of Venus’ atmosphere, from 0 to 120 kilometers (0 to 75 miles). Akatsuki arrived on 7 December 2015, bringing an ultraviolet imager (UVI), a pair of near-infrared cameras (IR1 and IR2), and one longwave infrared camera (LIR). UVI sees the daytime upper clouds in reflected sunlight. LIR sees the upper clouds’ radiant heat at a wavelength where there is little incoming solar energy. IR1 sees sunlight reflecting from the middle clouds on the dayside–and heat emanating from the surface on the nightside. IR2 sees the opacity of the lower clouds as they are silhouetted against heat emanating from the surface and deep atmosphere.
Clouds Upon Clouds
Although NASA’s Pioneer Venus was the first to try to study different cloud levels, the Galileo Jupiter mission achieved the first images showing different cloud structures at different altitudes on dayside and nightside during its flyby on 10 February 1990. Venus’ clouds float in its troposphere between altitudes of 47 and 70 kilometers (29 and 43 miles) and are divided into lower, middle, and upper cloud layers. The upper clouds of Venus are of major interest for several reasons: first, because most of Venus’ absorption of solar energy occurs in these clouds; second, because the superrotation reaches its fastest speeds precisely at the top of the upper clouds; and third, because the upper clouds possess high concentrations of a mysterious absorber–an unknown atmospheric constituent chemical responsible for more than half of the solar energy absorbed by Venus.
Akatsuki’s UVI is uniquely capable of studying the topmost clouds, with one filter that is more sensitive to the distribution of the mysterious absorber, making its presence known as dark streaks on ultraviolet images. Examining both missions’ data, Yeon Joo Lee (Technische Universität Berlin) discovered that the reflectivity of the upper clouds of Venus varies over time. The variation might result from changes in the abundance of the unknown absorber and affects the capacity of the atmosphere to absorb solar energy. This could be the first detection of climate change at another planet.
Venus' Upper Clouds
Just after it entered orbit, Akatsuki’s LIR camera spotted an enormous stationary wave running completely across the globe from north to south on Venus. The camera sees heat emanating from Venus’ uppermost clouds, day or night.
Months before Akatsuki’s arrival, Toru Kouyama (of IAST, Japan) and I discovered (independently, Kouyama using NASA’s Infrared Telescope Facility and myself using Venus Express’ VIRTIS) that some cloud patterns on Venus kept still despite the strong winds at high altitudes. We interpreted the cloud patterns to be stationary waves in the atmosphere called Lee waves, which happen where winds encounter obstacles like high mountains. Our findings were confirmed right after the orbit insertion of Akatsuki, when the very first image acquired by its longwave infrared (LIR) instrument contained the largest stationary wave ever spotted in the solar system.
Why are stationary waves in high clouds important? Their presence suggests that momentum and energy can be transported from Venus’ surface, 70 kilometers (43 miles) below, to the superrotating atmosphere. However, this discovery creates more puzzles than it solves. The Soviet Venera landers measured only very slow winds of 2 to 3 kilometers (1 to 2 miles) per hour at the surface. How can that connect to such high speeds at high altitudes? Even more puzzling is that VIRTIS sees stationary waves in the upper clouds but does not see them in simultaneous observations of the lower clouds.
Venus' Middle Clouds
Akatsuki’s IR1 camera is specially designed to penetrate beneath the upper clouds and image the middle cloud deck, whose patterns are intriguingly variable. Akatsuki’s images have revealed patterns that vary with time and from one side of Venus to the other and has seen the superrotating winds change speed by as much as 20 meters per second (about 25 percent) from year to year.
These middle clouds, located at a height of 50 to 56 kilometers (31 to 35 miles), have contained other surprises for us. They appeared featureless to Galileo in 1990 but have shown intriguing patterns to Akatsuki’s IR1. Their surprisingly varied brightness suggests there is some other atmospheric absorber in the middle clouds, a hypothesis supported by measurements from infrared instruments on Venus Express and NASA’s MESSENGER, which studied Venus during a flyby in June 2007. We have a lot to learn about Venus’ atmospheric chemistry and how it varies with altitude.
Venus' Lower Clouds
Akatsuki’s IR2 camera relies on heat emanating from the lower atmosphere of Venus to image the nightside lower clouds. The infrared radiation originating beneath the clouds silhouettes the lowermost cloud deck, so areas of thicker cloud appear darker in this photo. At lower left, the camera’s detector is overwhelmed by the brilliance of sunlight reflecting off the daylit crescent.
Both Venus Express and Akatsuki imaged the lower clouds (from 47 to 50 kilometers or 29 to 31 miles) on Venus’ nightside and found patterns that are strikingly different from the upper clouds. The clouds are more opaque near the equator, giving Venus a dark band in Akatsuki IR2 images, and more transparent (lighter) toward the poles. Impressive phenomena lie along the border between the equatorial band and the midlatitude bands, where shear makes billows and vortices, patterns like those seen on Jupiter. At Jupiter, these vortices are caused by the Coriolis effect. Venus rotates so slowly that its vortices can’t have the same cause.
Venus Express’ polar, elliptical orbit gave it brief, very close views of intricate cloud patterns at the north pole and distant views taking in the entire southern hemisphere. On each orbit, VIRTIS stared for hours at a vortex that whirls over Venus’ south pole. We discovered that its shape changes rapidly from a dipole to a tripole to a circle in a matter of days. Itziar Garate-Lopez (UPV/EHU, Spain) used VIRTIS to map the vertical structure of the south polar vortex and found it to be both tall and deep: it extends up to an altitude of 80 kilometers (50 miles), while its base lies at 55 kilometers (34 miles) or perhaps deeper. Intriguingly, the vortex’s location in the upper and lower clouds can be different, so its 3-dimensional structure might be helix-shaped.
ESA/VIRTIS/INAF-IASF/Obs. de Paris-LESIA
Storm at the South Pole
Venus Express’ VIRTIS revealed a maelstrom at the south pole—a whirling storm that punches a deep hole into the upper clouds.
The unknown absorber in Venus’ clouds helps us measure the speed of its winds through the tracking of cloud features seen in multiple ultraviolet images. We can also measure instantaneous wind speeds with spacecraft or ground-based spectrometers by examining how features in atmospheric spectra are Doppler-shifted by the fast motion of the atmosphere. Venus Express and Akatsuki’s monitoring have together produced more than 4 million cloud-tracking measurements.
Venus Express discovered that the velocity of the superrotation at the dayside upper clouds increased from 300 to about 380 kilometers (190 to 240 miles) per hour from 2006 to 2013. Akatsuki observed that wind speeds had decreased again by 2016, though not to their 2006 levels. This behavior correlates well with the changes in brightness of the upper clouds. The correspondence strongly suggests that the solar tides are a main cause of the superrotation. When there is more of the unknown absorber in the clouds, the atmosphere absorbs more incoming solar energy, powering faster winds. In contrast, the winds within the dayside middle clouds seem to keep more constant over time.
Top left: ESA; bottom left: ESA/VIRTIS/INAF-IASF/Obs. de Paris-LESIA; both right: JAXA/ISAS/DARTS
Venus' Varied Cloud Patterns
Venus’ multilayered atmosphere abounds with fascinating cloud patterns. TOP LEFT: An ultraviolet image taken by Venus Express’ VMC on 10 May 2010 shows gravity waves in Venus’ upper clouds—ripples along surfaces where atmospheric density changes with altitude. TOP RIGHT: Akatsuki's IR2 imaged well-developed vortices within Venus’ lowermost clouds just south of the equator on 13 August 2016. BOTTOM LEFT: This is the highest-resolution image of stationary waves in Venus’ nightside upper clouds, taken by Venus Express’ VIRTIS on 7 May 2008. BOTTOM RIGHT: On 1 July 2016, Akatsuki’s IR2 saw sharp, dark stripes edging the nightside lower clouds for distances of thousands of kilometers. These are some of the longest cloud patterns ever spotted on Venus.
The 2 spacecraft have produced a lesscontinuous record in the lower clouds because the longer-wavelength infrared instruments capable of observing at this altitude (the infrared channel of VIRTIS on Venus Express and the IR2 camera on Akatsuki) both failed after fulfilling their expected lifetimes. VIRTIS studied the clouds from 2006 to 2008, finding that the wind speeds did not vary with latitude during that time period (although they did vary with time). However, when Akatsuki observed the lower clouds in 2016, Takeshi Horinouchi of Hokkaido University discovered that a jet with much faster wind speeds is sometimes present at the equator. This recurrent jet might explain the billows and vortices observed in the lower clouds. We combined Venus Express and Akatsuki data with low-cloud data from Galileo, NASA’s Pioneer Venus entry probes, Soviet VEGA balloons, and numerous groundbased observations to reconstruct the equatorial wind speeds from 1978 to 2017 and found that their speed has varied by more than 100 kilometers (60 miles) per hour in that time.
To get a more complete picture of the 3-dimensional circulation of Venus’ winds through all levels of the nightside and dayside of Venus, we had help from the worldwide campaign of observations organized for the second Venus flyby of MESSENGER in June 2007. We performed feature tracking on images from Venus Express, MESSENGER, and amateur observations with small telescopes. We obtained Doppler wind speeds from spectra taken at large, ground-based telescopes, and we predicted wind speeds using temperature measurements from orbit and ground. We learned that the atmospheric circulation on the nightside of Venus is surprisingly different from the dayside.
With VIRTIS, we were able to image the upper-level clouds on the nightside with high resolution for the very first time. Our measurements revealed that superrotation on the nightside, rather than being homogeneous like on the dayside, sometimes becomes chaotic, with wind speeds as slow as 70 kilometers (43 miles) per hour in some places. VIRTIS was also able to observe a particular emission from oxygen molecules that occurs at an altitude of about 100 kilometers (60 miles) on the nightside well above the clouds, where superrotation is supposed to vanish. Ricardo Hueso (UPV/EHU, Spain) and Dmitry Gorinov (Space Research Institute, Russia) performed enormously challenging tracking of these fast airglow emissions and confirmed that at this altitude, the east-to-west superrotation is replaced by another mean circulation called “solar to antisolar.” As is hypothesized to happen on hot Jupiter exoplanets tidally locked to their stars, Venus’ highest-altitude winds blow from the area where solar insolation is maximum (the subsolar point) to the antipode at the antisolar point.
In the short term, worldwide campaigns of observations are being prepared to coordinate with the Venus flybys of the ESA/JAXA Mercury mission BepiColombo in October 2020 and August 2021 and probably also NASA’s Parker Solar Probe in December of this year. However, despite all we have learned from more than 60 years of spacecraft study, there are critical gaps in our knowledge of Venus’ atmosphere.
We know almost nothing about the deep atmosphere of Venus below 40 kilometers (25 miles), which contains more than 75 percent of the total mass of the atmosphere and controls the interaction between the surface and the atmosphere. Only in situ measurements from probes and landers can provide information for this region. Descent probes and short-lived (1 hour) and long-lived (1 year) landers have been proposed; more futuristic projects consider low-altitude balloons or surface rovers. New missions capable of making in situ measurements after a gap of more than 30 years will likely change our view of the planet all over again. After all, Venus’ appearances are deceptive.