New images yield clues to seasons of Uranus

Scientists seized their chance in 2007 to capture the first detailed images of the planet's features.Provided by the Division for Planetary Sciences
By | Published: October 13, 2008 | Last updated on May 18, 2023
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Uranus seasons
Near-infrared images from the Keck II telescope show the planet Uranus in 2005 (left), with the rings at an angle of 8 degrees, and at equinox in 2007 (right pair), with the planet’s ring system edge-on. In all images, the south pole is at the left and the equator is directly below the rings.
Courtesy of University of Wisconsin-Madison
With an 84-year orbit around the Sun, it isn’t often that planetary scientists have an opportunity to observe the change of seasons on Uranus, a planet some 19 times farther from the Sun than Earth.

But in 2007, the planet reached equinox, the point in time where the Sun is directly over the planet’s equator and what little sunlight the planet gets is distributed evenly over its northern and southern hemispheres. This situation gave scientists their best opportunity to probe the seasonal dynamics of the ringed planet.

Speaking at the American Astronomical Society’s Division for Planetary Sciences meeting, a team led by University of Wisconsin-Madison researcher Lawrence Sromovsky shared crisp new Keck II Telescope images of Uranus as it changed seasons.

“The last time this happened, there were no instruments that could resolve any features on the planet,” said Sromovsky, who led the study in collaboration with scientists from the Space Science Institute, the University of California at Berkeley, the SETI Institute and the Keck Observatory on the summit of Hawaii’s 14,000-foot Mauna Kea. “Now we can see what’s going on.”

Improvements in imaging technology and optics, as well as a new generation of large ground-based telescopes like Keck II, Sromovsky explains, provide researchers a chance to probe in detail the atmospheres of distant planets like Uranus. As a result, they’re gaining intriguing insight into the seasonal changes that drive astonishing and mysterious weather features.

The seventh planet from the Sun and the first planet to be discovered with the aid of a telescope, Uranus is characterized by a ring system and a blue-green atmosphere composed of hydrogen, helium, and methane. It has neatly zoned bands of clouds and some of the strangest discrete cloud features in the outer solar system.

The new study, based on a set of Keck II observations, was intended to take advantage of the change of seasons on Uranus to better understand how the Sun influences the planet’s weather. In addition to Sromovsky and Pat Fry and William Ahue of UW-Madison, the study was conducted by Heidi B. Hammel of the Space Science Institute, Imke de Pater of UC-Berkeley, Kathy Rages and Mark Showalter of the SETI Institute, and Marcos van Dam of the Keck Observatory.

Sromovsky and his colleagues were especially interested in seeing how the change of seasons influenced the planet’s weather. The study is challenging, says Sromovsky, because the progress of the seasons is so slow on Uranus and the planet is so far away, but it is intriguing because the planet’s equator is tilted at an unusually large 98° from its orbit plane, as if it had been tipped on its side.

“This tilt gives it the largest seasonal forcing of any planet in the solar system,” Sromovsky notes. “On an annual average basis, the poles get more sunlight than the equator.”

Seasonal forcing is the change in the solar heating distribution caused by a planet’s tilt on its axis. On Earth, the seasons change in relation to a hemisphere’s orientation to the Sun as determined by the 23.5° tilt of the planet’s axis of rotation.

“If the latitudinal distribution of solar energy input varies over the planet’s orbit, that forces changes in the weather,” Sromovsky said.

But for Uranus, weather changes due to seasonal forcing seem to lag behind the forcing: “Although both hemispheres were symmetrically heated by sunlight at equinox, the atmosphere itself was not symmetric, implying that it was responding to past sunlight instead if current sunlight, a result of Uranus’ cold atmosphere and long response time,” Sromovsky explained.

Uranus is cold because it receives very little energy, Sromovsky notes of a planet whose atmospheric temperatures at cloud tops can reach a frosty -360° Fahrenheit (-218° Celsius). The planet lacks a measurable internal heat source, and at its great distance, the Sun’s warmth is 400 times less than it is at Earth.

The most recent Keck II images show changes in the brightness of cloud bands in the planet’s northern and southern hemispheres as well as changes in two previously observed and apparently long-lived discrete cloud features. One is a massive vortex that had been oscillating in Uranus southern hemisphere, perhaps for decades, between 32° and 36° south latitude. In 2004, the feature began drifting north and may soon dissipate, according to the new report.

“For two decades, it seemed like it was behaving in a very reliable way,” Sromovsky said. “It may be that a change in the seasons has triggered it into a new dynamical state.”

The new images also gave Sromovsky’s group the opportunity to measure Uranus’ monster winds over a wider range of latitudes than was previously possible. Winds on the planet can achieve speeds of up to 560 mph (900 km/h).