Using radar measurements gathered by NASA’s Cassini spacecraft, Stanford geophysicist Howard Zebker and his team have concluded that the surface of Ligeia Mare, Titan’s second largest sea, has a mirror-like smoothness, possibly due to a lack of winds. As the only other solar system body with an Earth-like weather system, Titan could serve as a model for studying our own planet’s early history.
New radar measurements of an enormous sea on Titan offer insights into the weather patterns and landscape composition of the Saturnian moon. The measurements, made in 2013 by NASA’s Cassini spacecraft, reveal that the surface of Ligeia Mare, Titan’s second largest sea, possesses a mirror-like smoothness, possibly due to a lack of winds.
“If you could look out on this sea, it would be really still. It would just be a totally glassy surface,” said Howard Zebker, professor of geophysics and of electrical engineering at Stanford who is the lead author of a new study detailing the research.
The findings, recently published online in Geophysical Research Letters, also indicate that the solid terrain surrounding the sea is likely made of solid organic materials and not frozen water.
Saturn’s largest moon, Titan has a dense, planet-like atmosphere and large seas made of methane and ethane. Measuring roughly 260 miles (420 km) by 217 miles (350 km), Ligeia Mare is larger than Lake Superior on Earth. “Titan is the best analog that we have in the solar system to a body like the Earth because it is the only other body that we know of that has a complex cycle of solid, liquid, and gas constituents,” Zebker said.
Titan’s thick cloud cover makes it difficult for Cassini to obtain clear optical images of its surface, so scientists must rely on radar, which can see through the clouds, instead of a camera.
To paint a radar picture of Ligeia Mare, Cassini bounced radio waves off the sea’s surface and then analyzed the echo. The strength of the reflected signal indicated how much wave action was happening on the sea. To understand why, Zebker said, imagine sunlight reflecting off of a lake on Earth. “If the lake were really flat, it would act as a perfect mirror and you would have an extremely bright image of the sun,” he said. “But if you ruffle up the surface of the sea, the light gets scattered in a lot of directions, and the reflection would be much dimmer. We did the same thing with radar on Titan.”
The radar measurements suggest the surface of Ligeia Mare is eerily still. “Cassini’s radar sensitivity in this experiment is one millimeter, so that means if there are waves on Ligeia Mare, they’re smaller than one millimeter. That’s really, really smooth,” Zebker said.
One possible explanation for the sea’s calmness is that no winds happened to be blowing across that region of the moon when Cassini made its flyby. Another possibility is that a thin layer of some material is suppressing wave action. “For example, on Earth, if you put oil on top of a sea, you suppress a lot of small waves,” Zebker said.
Cassini also measured microwave radiation emitted by the materials that make up Titan’s surface. By analyzing those measurements, and accounting for factors such as temperature and pressure, Zebker’s team confirmed previous findings that the terrain around Ligeia Mare is composed of solid organic material, likely the same methane and ethane that make up the sea. “Like water on Earth, methane on Titan can exists as a solid, a liquid, and a gas all at once,” Zebker said.
Titan’s similarities to Earth make it a good model for our own planet’s early evolution, Zebker said. “Titan is different in the details from Earth, but because there is global circulation happening, the big picture is the same,” he added. “Seeing something in two very different environments could help reveal the overall guiding principles for the evolution of planetary bodies, and help explain why Earth developed life and Titan didn’t.”
Ker Than is associate director of communications for the School of Earth Sciences.
Howard Zebker, Stanford University School of Earth Sciences: 650-723-8067, email@example.com
Ker Than, Stanford University School of Earth Sciences: 646-673-4558, firstname.lastname@example.org