Saturn surprises greet Cassini

The spacecraft discovers a radiation belt, listens to lightning, and examines a hazy, glowing moon.
By | Published: August 12, 2004
August 12, 2004
Cassini bagged its first major discovery just one month into the start of the spacecraft’s 4-year-long exploration of Saturn and its moons. NASA scientists announced last week that Saturn’s radiation belts extend much closer to the planet than previously thought, a revelation that Cassini imaging team member Donald Mitchell of Johns Hopkins University called a “huge surprise.”
Saturn's south pole in the infrared
A prominent dark spot marks Saturn’s South Pole. The Cassini spacecraft took this contrast-enhanced image on July 13, 2004, through a filter sensitive to infrared wavelengths. Cassini was 3.1 million miles (5 million kilometers) from Saturn at the time.
NASA / JPL / Space Science Institute
Radiation belts are regions where energetic electrons and ions have become trapped in a planet’s magnetic field. Gas clouds located inward of Saturn’s innermost, or D, ring emit fast, electrically neutral atoms when bombarded by the new belt’s magnetically trapped ions. Cassini’s magnetospheric imaging instrument detected the neutral atoms, allowing scientists to map the new belt. It extends from just above Saturn’s cloud tops all the way to the inner edge of the D ring.

“This new radiation belt had eluded detection by any of the spacecraft that previously visited Saturn,” said Mitchell. “With its discovery, we have seen something that we did not expect, that radiation belt particles can ‘hop’ over obstructions like Saturn’s rings without being absorbed by the rings in the process.”

Detail of Saturn's southern clouds
Irregular boundaries visible in Saturn’s southern polar region highlight the often turbulent nature of the planet’s cloud bands. Cassini snapped this infrared image on July 13, 2004.
NASA / JPL / Space Science Institute
Meanwhile, another Cassini instrument picked up bursts of radio waves created by lightning in Saturn’s stormy atmosphere. “We are detecting the same crackle and pop one hears when listening to an AM radio broadcast during a thunderstorm,” said Bill Kurth from the University of Iowa.

Twenty years ago, Voyager detected lightning, too. But it came from a single extended storm system growling in Saturn’s low latitudes. The storm lasted for months, regularly sparking lightning in a pattern that changed little from day to day. For Cassini, lightning is much more intermittent and, scientists think, may stem from storms of shorter duration occurring at the planet’s middle and high latitudes.

Why the difference in storm characteristics? When Voyager passed Saturn, the rings cast a shadow near Saturn’s equator, creating a cool band that cut through the planet’s warmest zone. The proximity of hot and cool air masses may have prompted large, long-lived storms to form in Saturn’s equatorial region. In contrast, Cassini has arrived during Saturn’s southern hemisphere summer. Now, the shadow of the rings drapes over much of the northern hemisphere, diffusing any sharp temperature contrasts.

Titan haze layers
This image of Titan reveals layers high in the moon’s atmosphere where photochemical reactions create distinct layers of haze. The detached layer, a separate purple band arcing above the pale moon’s limb in this false-color view, is about 75 miles (120 km) thick.
NASA / JPL / Space Science Institute
Titan, Saturn’s largest moon, remains Cassini’s most intriguing target. “Titan glows throughout the near-infrared spectrum,” said Kevin Baines, a member of Cassini’s science team at the Jet Propulsion Laboratory in Pasadena, California. Day and night, fluorescing methane and carbon monoxide gases give the moon an infrared glow.

Late last month, Cassini revealed a view of Titan from another end of the spectrum. Imaging in the ultraviolet, the spacecraft found two distinct layers of haze, providing scientists with another puzzle. Titan’s dense atmosphere — which is mostly nitrogen with a few percent methane — forms haze particles in the presence of ultraviolet light. Scientists believe the process begins in the high atmosphere, at altitudes above 250 miles (400 kilometers), where ultraviolet light breaks down methane and nitrogen molecules. The byproducts probably react to form complex organic molecules that combine into the small haze particles.

Why two haze layers have formed, say scientists, is a mystery they hope Cassini will help them solve.