The upper layers in the atmospheres of gas giants - Saturn, Jupiter, Uranus and Neptune - are hot, just like Earth's. But unlike Earth, the Sun is too far from these outer planets to account for the high temperatures. Their heat source has been one of the great mysteries of planetary science.
To learn more about Saturn, zoom in and give the planet a spin. Use the search function at bottom to learn more about its moons - or just about anything else in the solar system. Credit: NASA/JPL-Caltech
New analysis of data from NASA's Cassini spacecraft finds a viable explanation for what's keeping the upper layers of Saturn, and possibly the other gas giants, so hot: auroras at the planet's north and south poles. Electric currents, triggered by interactions between solar winds and charged particles from Saturn's moons, spark the auroras and heat the upper atmosphere. (As with Earth's northern lights, studying auroras tells scientists what's going on in the planet's atmosphere.)
The work, published April 6 in Nature Astronomy, is the most complete mapping yet of both temperature and density of a gas giant's upper atmosphere - a region that has, in general, been poorly understood.
The aurora at Saturn's southern pole is visible in this false-color image. Blue represents the aurora; red-orange is reflected sunlight. The image was gathered by Cassini's ultraviolet imaging spectrograph (UVIS) on June 21, 2005. Credit: NASA/JPL/University of Colorado
Full image and caption
By building a complete picture of how heat circulates in the atmosphere, scientists are better able to understand how auroral electric currents heat the upper layers of Saturn's atmosphere and drive winds. The global wind system can distribute this energy, which is initially deposited near the poles toward the equatorial regions, heating them to twice the temperatures expected from the Sun's heating alone.
"The results are vital to our general understanding of planetary upper atmospheres and are an important part of Cassini's legacy," said author Tommi Koskinen, a member of Cassini's Ultraviolet Imaging Spectograph (UVIS) team. "They help address the question of why the uppermost part of the atmosphere is so hot while the rest of the atmosphere - due to the large distance from the Sun - is cold."
Managed by NASA's Jet Propulsion Laboratory in Southern California, Cassini was an orbiter that observed Saturn for more than 13 years before exhausting its fuel supply. The mission plunged it into the planet's atmosphere in September 2017, in part to protect its moon Enceladus, which Cassini discovered might hold conditions suitable for life. But before its plunge, Cassini performed 22 ultra-close orbits of Saturn, a final tour called the Grand Finale.
It was during the Grand Finale that the key data was collected for the new temperature map of Saturn's atmosphere. For six weeks, Cassini targeted several bright stars in the constellations of Orion and Canis Major as they passed behind Saturn. As the spacecraft observed the stars rise and set behind the giant planet, scientists analyzed how the starlight changed as it passed through the atmosphere.
Measuring the density of the atmosphere gave scientists the information they needed to find the temperatures. (Density decreases with altitude, and the rate of decrease depends on temperature.) They found that temperatures peak near the auroras, indicating that auroral electric currents heat the upper atmosphere.
And both density and temperature measurements together helped scientists figure out wind speeds. Understanding Saturn's upper atmosphere, where planet meets space, is key to understanding space weather, and its impact on other planets in our solar system and exoplanets around other stars.
The Cassini-Huygens
mission is a cooperative project of NASA, ESA (the European Space Agency) and the
Italian Space Agency. JPL, a division of Caltech in Pasadena, manages the
mission for NASA's Science Mission Directorate in Washington. JPL designed,
developed and assembled the Cassini orbiter.
More information about Cassini can be found here: