PASADENA, Calif. – Data collected during several recent flybys of Titan by NASA’s Cassini spacecraft have put another arrow in the quiver of scientists who think the Saturnian moon contains active cryovolcanoes spewing a super-chilled liquid into its atmosphere. The information was released today during a meeting of the American Geophysical Union in San Francisco, Calif.
“Cryovolcanoes are some of the most intriguing features in the solar system,” said Rosaly Lopes, a Cassini radar team investigation scientist from NASA’s Jet Propulsion Laboratory in Pasadena, Calif. “To put them in perspective — if Mount Vesuvius had been a cryovolcano, its lava would have frozen the residents of Pompeii.”
Rather than erupting molten rock, it is theorized that the cryovolcanoes of Titan would erupt volatiles such as water, ammonia and methane. Scientists have suspected cryovolcanoes might inhabit Titan, and the Cassini mission has collected data on several previous passes of the moon that suggest their existence. Imagery of the moon has included a suspect haze hovering over flow-like surface formations. Scientists point to these as signs of cryovolcanism there.
Active Cryovolcanic Features on Titan?
“Cassini data have raised the possibility that Titan’s surface is active,” said Jonathan Lunine, a Cassini interdisciplinary scientist from the Lunar and Planetary Laboratory, University of Arizona, Tucson. “This is based on evidence that changes have occurred on the surface of Titan, between flybys of Cassini, in regions where radar images suggest a kind of volcanism has taken place.”
What led some Cassini scientists to believe that things are happening now were changes in brightness and reflectance detected at two separate and distinct regions of Titan. Reflectance is the ratio of light that radiates onto a surface to the amount reflected back. These changes were documented by Visible and Infrared Mapping Spectrometer data collected on Titan flybys from July 2004 to March 2006. In one of the two regions, the reflectance of the surface surged upward and remained higher than expected. In the other region, the reflectance shot up but then trended downward. There is also evidence that ammonia frost is present at one of the two changing sites. The ammonia was evident only at times when the region was inferred to be active.
“Ammonia is widely believed to be present only beneath the surface of Titan,” said Robert M. Nelson of JPL, a scientist for Cassini’s Visual and Infrared Mapping Spectrometer team. “The fact that we found it appearing at times when the surface brightened strongly suggests that material was being transported from Titan’s interior to its surface.”
Some Cassini scientists indicate that such volcanism could release methane from Titan’s interior, which explains Titan’s seemingly continuous supply of fresh methane. Without replenishment, scientists say, Titan’s original atmospheric methane should have been exhausted long ago.
But other scientists familiar with the spectrometer data argue that the ammonia identification is not certain, and that the purported brightness changes might not be associated with changes on Titan’s surface. Instead they might result from the transient appearances of ground “fogs” of ethane droplets very near Titan’s surface, driven by atmospheric rather than geophysical processes. Nelson has considered the ground fog option, stating, “There remains the possibility that the effect is caused by a local fog, but if so, we would expect it to change in size over time due to wind activity, which is not what we see.”
The chilly volcanoes of Titan are not a fait accompli. An alternative hypothesis to an active Titan suggests the Saturnian moon could be taking its landform evolution cues from a moon of Jupiter.
“Like Callisto, Titan may have formed as a relatively cold body, and may have never undergone enough tidal heating for volcanism to occur,” said Jeffrey Moore, a planetary geologist at the NASA Ames Research Center, Moffett Field, Calif. “The flow-like features we see on the surface may just be icy debris that has been lubricated by methane rain and transported downslope into sinuous piles like mudflows.” More revelations may be forthcoming. Scientists are still analyzing the data from Cassini’s most recent flyby on Dec. 5. Cassini’s next Titan flyby is scheduled in 11 days, when the spacecraft will come within 970 kilometers (603 miles) of its cloud-shrouded surface.
For more information about the Cassini-Huygens mission, visit: http://saturn.jpl.nasa.gov and http://www.nasa.gov/cassini .
The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. JPL, a division of the California Institute of Technology in Pasadena, manages the mission for NASA’s Science Mission Directorate in Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radar instrument was built by JPL and the Italian Space Agency, working with team members from the United States and several European countries. The Visual and Infrared Mapping Spectrometer team is based at the University of Arizona.
Infrared Map of Titan’s Active Regions December 15, 2008 Full-Res: PIA11701
This infrared projection map of Titan was composed from images taken by NASA’s Cassini spacecraft, visual and infrared mapping spectrometer. The location of two regions that changed in brightness are labeled. These regions are hypothesized by some to be areas of cryovolcanic activity on Titan.
Rather than erupting molten rock, it is theorized that the cryovolcanoes of Titan would erupt volatiles such as water, ammonia and methane. Scientists have suspected cryovolcanoes might be on Titan, and the Cassini mission has collected data on several previous passes of the moon that suggest their existence. Imagery of the moon has included a suspect haze hovering over flow-like surface formations, which are plausibly the result of icy volcanism.
Some Cassini scientists indicate that such volcanism could release methane from the interior, which explains Titan’s seemingly continuous supply of fresh methane. Without replenishment, scientists say, Titan’s original atmospheric methane should have been exhausted long ago.
This image is an overlay of all the high-resolution images from the first 45 flybys, up through last February 2007. The map was created using what 2.1 micron wavelength. Image scale is about 25 kilometers (16 miles) per pixel or 1.8 pixels per degree.
For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm. The visual and infrared mapping spectrometer team homepage is at http://wwwvims.lpl.arizona.edu. Credit: NASA/JPL/University of Arizona
Active Cryovolcanic Features on Titan?
The Cassini Radar Mapper imaged Titan on Feb. 22, 2008 (as shown on the left) and April 30, 2006 (as shown on the right).
These radar images show the outlines of regions “1”d “2” identified by Cassini’s visual and infrared mapping spectrometer and inferred to be variable (see VIMS flat map, PIA11701), and which have been hypothesized to be due to cryovolcanic activity. The lobate, flow-like features in region 1 are consistent with this interpretation.
Region 1 is just north of the feature named Hotei Arcus and is centered on 28 degrees south latitude by 78 degrees west longitude. The region is about 400 kilometers (249 miles) across. Region 2 is on the western part of Xanadu and is centered on 7 degrees south latitude by 135 degrees west longitude. This region is about 900 kilometers (560 miles) across. In both cases, north is up, and features as small as 300-500 meters can be resolved.
