Tonight's Sky
Sun
Sun
Moon
Moon
Mercury
Mercury
Venus
Venus
Mars
Mars
Jupiter
Jupiter
Saturn
Saturn

Tonight's Sky — Change location

OR

Searching...

Tonight's Sky — Select location

Tonight's Sky — Enter coordinates

° '
° '

New maps of seasonal polar caps will refine martian climate models

The spectroscopy data allowed scientists to accurately determine the thickness of the martian ice caps over time.
Provided by the Planetary Science Institute, Tucson, Arizona
Mars polar cap
Springtime on Mars: The images of Mars' north polar cap (left) were taken by NASA's Hubble Space Telescope (HST), while the maps at right were created from neutron spectroscopy data gathered by the Mars Odyssey spacecraft. The images and maps show the recession of the seasonal polar cap from early to late spring. The maps reveal the thickness of surface carbon dioxide ice (dry ice), which decreases as the northern hemisphere is exposed to sunlight during the spring and summer. The images and maps extend from the pole to 50° north latitude.
September 16, 2009
Scientists from the Tucson-based Planetary Science Institute have created the first detailed maps that show the amount of dry ice (solid carbon dioxide) deposited in the polar regions of Mars. The maps reveal how the ice thickness varies with the seasons.

"The maps were created from measurements taken by the Mars Odyssey neutron spectrometer," said Thomas Prettyman, Planetary Science Institute senior scientist.

The spectroscopy data, gathered during 2 martian years, allowed Prettyman and his colleagues to accurately determine the thickness of the martian ice caps over time.

The amount of carbon dioxide ice at the poles varies in response to seasonal changes in sunlight, and about 25 percent of the atmosphere is cycled through the seasonal caps, Prettyman said.

"We need a detailed understanding of the present atmosphere on Mars in order to answer fundamental questions about the planet's climate history, including whether conditions on Mars could have been suitable for life in the distant past," he said.

The local thickness of the polar caps depends on several factors such as the amount of solar energy absorbed by the surface and atmosphere and the flow of warm air from lower latitudes that accompanies carbon dioxide condensation at the poles, Prettyman said.

In the northern polar region, carbon dioxide deposition is skewed toward an area known as Acidalia. Thicker carbon dioxide ice in that region may be caused by frigid winds coming from Chasma Boreale, a large canyon near the martian north pole.

In the southern hemisphere, carbon dioxide ice accumulates more rapidly in a region known as the south polar residual cap, which is offset from the pole and contains perennial carbon dioxide ice deposits.

Prettyman and his colleagues concluded that the asymmetry in the south polar seasonal cap is caused primarily by variations in surface composition.

"The regions outside the residual cap consist of water ice mixed with rocks and soil that are warmed during summer," he said. "This delays the onset of carbon dioxide ice accumulation in the fall. In addition, heat stored in water-rich regions is gradually released during fall and winter, further limiting ice accumulation."

Prettyman and his colleagues also used neutron spectroscopy to determine how much non-condensable gas (argon and nitrogen) remains in the atmosphere at high latitudes as carbon dioxide condenses.

"We observed strong enrichment of non-condensable gas at the south pole during fall and winter," Prettyman said. "The observed time variation of the concentration of nitrogen and argon provides information about local circulation patterns. This includes the timing and strength of the polar winter vortex, a large-scale, cyclonic flow that inhibits mixing of nitrogen and argon with air from lower latitudes."

Accurate data on the thickness of carbon dioxide ice and its distribution, as well as data on seasonal concentrations of non-condensable gases, will allow scientists to refine martian general circulation models. This will give them a deeper understanding of atmospheric dynamics and the planet's climate change over time.

Neutron spectroscopy is key to determining carbon dioxide ice thickness during the long polar nights. "Unlike optical techniques, neutron spectroscopy does not require sunlight and can peer into the darkness, revealing details of the seasonal caps that have never been observed before," he said.
0

JOIN THE DISCUSSION

Read and share your comments on this article
Comment on this article
Want to leave a comment?
Only registered members of Astronomy.com are allowed to comment on this article. Registration is FREE and only takes a couple minutes.

Login or Register now.
0 comments
ADVERTISEMENT

FREE EMAIL NEWSLETTER

Receive news, sky-event information, observing tips, and more from Astronomy's weekly email newsletter.

ADVERTISEMENT
ADVERTISEMENT
BoxProductcovernov

Click here to receive a FREE e-Guide exclusively from Astronomy magazine.

Find us on Facebook

Loading...