water on Mars
Images taken by Mars Global Surveyor (MGS) have provided some of the best evidence yet that water still occasionally flows on the Martian surface. Two gullies on the inside of craters, which were originally photographed by MGS in 1999 and 2001, and imaged again in 2004 and 2005, showed changes consistent with water flowing down the crater walls, according to a study published in December 2006.1
Other scientists challenged this explanation, arguing that the atmosphere of Mars is so thin and the temperature so cold that liquid water couldn't persist at the surface but would rapidly evaporate or freeze. Some of these scientists suggested that the gullies, and others like them discovered by MGS, might have been caused not by water but by liquid carbon dioxide, which has a lower melting point than water. However, the carbon dioxide theory does not bear close scrutiny, for the following reason. The minimum pressure under which a substance can exist as a liquid occurs at the substance's triple point. In the case of carbon dioxide, the triple point corresponds to a temperature of -56.6°C and a pressure of 5.1 atmospheres (518,000 Pa). Now, while Mars does get as cold as (or colder than) -56.6°C, the surface pressure on Mars (or on Earth, for that matter) certainly never reaches 5.1 atmospheres. Thus we can be absolutely certain that carbon dioxide cannot exist as a liquid on or anywhere near the surface on Mars. In contrast, the triple point of water occurs at a mere 611.73 Pa (6.1173 millibars), a pressure that is frequently exceeded on the surface of Mars, in craters and other low-lying areas, according to measurements by Viking and other spacecraft. This fact adds credence to the view that water could remain liquid long enough, after breaking out from an underground source, to carry debris downslope before freezing.
Water in the past on Mars
In 1969, Mariner 9 provided the first strong evidence that liquid water had flowed on the surface of Mars in the remote past. Among the thousands of images it sent back from orbit were those of flat-floored channels with eroded banks, sand bars and teardrop-shaped islands, channels with second- and third-order tributary systems, and braided channels which, had they been encountered on Earth, would unhesitatingly have been attributed to episodic flooding. Later probes have added to the evidence of water-carved channels and other features on Mars.
The fact that Mars had flowing water implies that conditions on the planet were once very different than they are today (see Mars, past conditions). Yet, curiously, there are no signs that it ever rained on the fourth planet. The water-carved systems on Mars are short and stubby, dividing little upstream, and ending abruptly as if the water had suddenly appeared at that spot rather than having fallen over a large area and become collected. The assumption is that the Martian water erupted from beneath the surface, welling up as a result of volcanic eruptions or asteroid impacts, and then flooded to form channels, and lakes, and perhaps even seas.
An ocean on Mars?
In 1989, Timothy Parker of the Jet Propulsion Laboratory and colleagues argued that there was geological evidence of a shorelines.2 The originally proposed shorelines were two discontinuous boundaries between landforms thought to have formed by wave or other water-related processes. Stephen Clifford (Lunar and Planetary Institute) and Parker later refined the outlines and hypothesized that Noachian-aged (3.8 to 3.5 billion year old) bodies of water and ice covered up to one third of the surface of Mars.3 The two most continuous supposed shorelines, called the Arabia and Deuteronilus shorelines, run roughly parallel with the southern boundary of the northern plains. The Arabia shoreline can be traced all around the planet except through the Tharsis region. But its elevation varies by several kilometers, in some places by 11 km – a large range that doesn't fit well with a shoreline interpretation. Features of the proposed shoreline that have been interpreted as formed by wave actions or other marine processes can be equally argued as being formed by mass wasting and volcanic processes. The Deuteronilus boundary is less conspicuous than the Arabia one but has a smaller range in elevations. For nearly half its length the Deuteronilus boundary marks the southern extent of the geologic unit called the Vastitas Borealis Formation. For the rest of its length it is seen only intermittently around clusters of hills or across lava flows. Thr trouble is, if Deuteronilus is an ancient shoreline, why does it lack key features, such as inward-facing cliffs or channels that end abruptly as they enter a large body of water, that would be expected at the margins of a great sea? The fact is, the shoreline evidence for a northern ocean is not all that convincing.
Evidence from the rovers
Where did all the water go?If there was once a lot of water on the surface of Mars, where did it all go? One possibility is that some of it evaporated, became water vapor in the atmosphere, and was then lost into space because the gravity pull of the planet couldn't hold on to it. Another possibility is that much of still exists on Mars, as ice. Both the poles of Mars contain water ice. And in 2002, scientists analyzing data from the Mars Observer spacecraft announced that they had found vast quantities of water ice in great swathes of the planet just below the surface.
Related categories MARS TOPICS
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