Martian Hydrology
Due to the low
atmospheric pressure on Mars' surface, liquid water can only exist at the
lowest elevations for short periods of time. Water appears to make up the
majority of the two polar ice caps. If the water ice in the south polar ice cap
were to melt, it would cover the entire planet's surface to a depth of 11 meters.
The permafrost mantle reaches from the pole to around 60 ° latitude.
Large amounts of water
ice are believed to be trapped within Mars' thick cryosphere. Radar images from
Mars Express and the Mars Reconnaissance Orbiter reveal huge amounts of water
ice at both the poles and mid-latitudes from July 2005 to November 2008. On July
31, 2008, the Phoenix lander took a direct sample of water ice in shallow
Martian soil.
Thousands of features
similar to terrestrial gullies can be found along crater and canyon walls. The
gullies are found in the southern hemisphere's highlands, facing the Equator,
and are all poleward of 30 degrees latitude. Several scientists have indicated
that their development process requires liquid water, most likely from melting
ice, while others have proposed formation mechanisms utilizing carbon dioxide
frost or dry dust movement. Weathering has left no partially degraded gullies
and no overlaid impact craters, indicating that these are relatively young
structures, potentially even active today.
Other geological
features, such as deltas and alluvial fans preserved in craters, also strongly
suggest that Mars was warmer and wetter at some point in its history. Such
circumstances necessitate the widespread presence of crater lakes across a
considerable percentage of the surface, which is supported by independent
mineralogical, sedimentological, and geomorphological evidence. Some authors
have even claimed that during the planet's history, much of the planet's low
northern plains were covered by a genuine ocean hundreds of meters deep,
however, this is still debatable.
The discovery of
specific minerals such as hematite and goethite, both of which develop in the
presence of water, adds to the evidence that liquid water once existed on Mars'
surface. Higher resolution analyses by the Mars Reconnaissance Orbiter have
refuted some of the data previously thought to imply ancient water basins and
flows. The mineral jarosite was discovered by Opportunity in 2004. This only
occurs in the presence of acidic water, indicating that there was once water on
Mars. More recent evidence for liquid water comes from NASA's Mars rover
Opportunity's discovery of the mineral gypsum on the surface in December 2011. Furthermore,
according to study leader Francis McCubbin, a planetary scientist at the
University of New Mexico in Albuquerque who studied hydroxals in crystalline
minerals from Mars, the amount of water in Mars' upper mantle is equal to or
greater than that of Earth, with 50–300 parts per million of water, enough to
cover the entire planet to a depth of 200–1000 meters.
On March 18, 2013, NASA reported evidence of mineral hydration, most likely hydrated calcium sulphate, in several rock samples, including broken fragments of "Tintina" rock and "Sutton Inlier" rock, as well as veins and nodules in other rocks such as "Knorr" rock and "Wernicke" rock, from instruments on the Curiosity rover. In the rover's traverse from the Bradbury Landing site to the Yellowknife Bay area in the Glenelg terrain, analysis using the rover's DAN instrument revealed evidence of subsurface water with as much as 4% water content down to a depth of 60 cm (2.0 ft).
Comments
Post a Comment