09/10/2024
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ESA’s Mars Categorical has captured an astonishing array of landforms rising from a thick winter blanket of frost as spring arrives within the south polar area of Mars. A few of these options are surprisingly darkish in contrast with their icy environment, incomes their nickname of ‘cryptic terrain’.
The seasonal polar caps of Mars are primarily composed of carbon dioxide ice with some water ice. The ice partially sublimates (turns immediately from strong ice into vapour) in spring, releasing massive quantities of gasoline into Mars’ skinny environment. In autumn, the vapour condenses once more, and the polar caps develop. By late winter they could even attain so far as 55 levels latitude – roughly the equal of Scotland and Denmark’s southern reaches if translated to the northern hemisphere of Earth.
This freeze-thaw cycle provides rise to quite a lot of curious floor options, lots of that are captured in these photos of the Australe Scopuli area near the south pole of Mars. The photographs had been taken by the Excessive Decision Stereo Digicam (HRSC) onboard Mars Categorical on 2 April 2024 throughout southern hemisphere spring.
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The left facet of the principle picture is dominated by a thick stack of uncovered layered deposits, fashioned as layers of ice freeze with various quantities of mud trapped inside. The appropriate facet of the principle picture exhibits the graceful floor of those polar layered deposits.
Darkish-toned terrain dominates the centre of the scene. Initially nicknamed cryptic terrain as a result of it was unclear why these rising options are a lot darker than the remainder of the ice cap, researchers now have a greater thought as to the processes at play on this dynamic area.
Periglacial patterns
Zooming into the darkish area within the main image reveals that the surface is covered with a pattern of polygon shapes at a range of scales. Each polygon is bounded by troughs or ridges, and sometimes the troughs trap bright frost.
For a closer look at polygonal terrain we can turn to higher resolution imagery provided by ESA’s Trace Gas Orbiter. Although the example shown here (above) is from a different area in Mars’ southern latitudes, it beautifully illustrates the occurrence of lingering ice at the polygon edges in and around an impact crater, on a cold springtime morning.
On Earth, this pattern is a common periglacial feature in arctic and antarctic regions that usually indicates the presence of water ice in the ground. ‘Periglacial’ refers to regions and processes where cold climate contributes to the evolution of landforms and landscapes. The polygons form from freeze-thaw cycles of ground ice over the course of several years, or even centuries. Studying these kinds of patterns on Mars can help researchers decipher the climate history of the planet.
Jets and fans
In many locations throughout the image, bright and dark fan-shaped deposits can be seen. They range from tens of metres to several hundreds of metres and are oriented in the direction of prevailing winds.
When sunlight penetrates through the translucent carbon dioxide ice layer in early spring it warms up the underlying surface. The ice at the bottom of the layer begins to sublimate, creating pockets of trapped gas. The pressure builds up and the overlying ice suddenly cracks. Jets of gas burst through the surface, carrying dark dust from below. The dust falls back to the surface in a pattern shaped by the direction of the prevailing wind.
The process is similar to that which creates the ‘spider’ features presented in another recent Mars Express image release.
After the dark material has settled on top of the ice, a second phase kicks in as the ice and new layer of dust interact.
The dark material absorbs more sunlight than the brighter, reflective ice and so it warms up the ice it fell on top of and the dark grains gradually sink through the ice. At the same time, this accelerates the process of sublimation, creating a hole. Either fresh ice is revealed underneath, or new frost may then condense on top of the sinking dark grains, resulting in a bright fan at the place of the initially dark fan.
This process is only observed in spring. Once the seasonal translucent ice layer has completely sublimated, the fans become indistinguishable from the underlying surface.
Exploring Mars
It is thanks to the longevity of missions like Mars Express, which arrived in orbit around the Red Planet in 2003, that seasonal changes can be observed over many years and once-cryptic features can be better understood.
As well as studying the ice caps of the planet the HRSC has shown us the full range of Mars’ geological features, from wind-sculpted ridges and grooves to sinkholes on the flanks of colossal volcanoes to impact craters, tectonic faults, river channels and ancient lava pools.
With its suite of eight instruments Mars Express also maps the planet’s minerals, explores the composition and circulation of its atmosphere, probes beneath its crust, and studies the martian environment.
The mission has been immensely productive over its lifetime, creating a far fuller and more accurate understanding of our planetary neighbour than ever before.
The Mars Express High Resolution Stereo Camera (HRSC) was developed and is operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR).
