Some are simply lacelike patterns, but others have legs extending in all directions.
"You can see the sort of spiderlike shape," Hansen said. "They drape over the local topography. In fact, they love to sit on top of little hummocks."
Unlike rivers, which flow downhill, many of Mars's formations do the reverse.
"The channels widen and deepen as they go uphill," Hansen said. "That type of erosion is consistent with gas as the erosion agent."
The channels can get up to six feet (two meters) deep, the images show.
Using an infrared detector called the Compact Reconnaissance Imaging Spectrometer for Mars, HiRise was also able to determine the composition of bright streaks that often angle outward from the dust deposits, like slightly wider fans.
These streaks are comprised of carbon dioxide rather than dust, said Tim Titus of the U.S. Geological Survey in Flagstaff, Arizona.
The fact that the white streaks and the black fans don't perfectly align indicates that they were produced at different times of the day, Titus added.
At dawn, there isn't enough heat from the sun to melt any gas, he pointed out. Later gas flows form, but they're not fast enough to pick up any dust.
When this gas escapes into the air, it expands and cools rapidly, raining back carbon dioxide "snow" to the surface.
"Our calculation is that as much as 2 percent of the gas can get converted back into frost," Titus said. "That's plenty to form these [white] fans."
When the heat picks up strength later in the day, the stronger gas jets begin picking up dust. But by then the wind has shifted, sending the darker dust in a different direction as the frost.
In the afternoon the process slows down again, producing a new bright streak representing still another slight shift in wind direction.
Global climate models for Mars predict the normal wind speeds at various times of day.
Thus, Titus said, "the direction of the fans can tell us a lot about what time of day they were formed."
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