Buried water ice at Mars's equator?
Windswept piles of dust, or layers of ice? ESA’s Mars Express has revisited one of Mars’s most mysterious features to clarify its composition. Its findings suggest layers of water ice stretching several kilometres below ground – the most water ever found in this part of the planet.
Over 15 years ago, Mars Express studied the Medusae Fossae Formation (MFF), revealing massive deposits up to 2.5 km deep. From these early observations, it was unclear what the deposits were made of – but new research now has an answer.
“We’ve explored the MFF again using newer data from Mars Express’s MARSIS radar, and found the deposits to be even thicker than we thought: up to 3.7 km thick,” says Thomas Watters of the Smithsonian Institution, USA, lead author of both the new research and the initial 2007 study. “Excitingly, the radar signals match what we’d expect to see from layered ice, and are similar to the signals we see from Mars’s polar caps, which we know to be very ice rich.”
If melted, the ice locked up in the MFF would cover the entire planet in a layer of water 1.5 to 2.7 m deep: the most water ever found in this part of Mars, and enough to fill Earth’s Red Sea.
Alternating layers of ice
The MFF consists of several wind-sculpted features measuring hundreds of kilometres across and several kilometres high. Found at the boundary between Mars’s highlands and lowlands, the features are possibly the biggest single source of dust on Mars, and one of the most extensive deposits on the planet.
Initial observations from Mars Express showed the MFF to be relatively transparent to radar and low in density, both characteristics we’d see from icy deposits. However, scientists couldn’t rule out a drier possibility: that the features are actually giant accumulations of windblown dust, volcanic ash or sediment.
“Here’s where the new radar data comes in! Given how deep it is, if the MFF was simply a giant pile of dust, we’d expect it to become compacted under its own weight,” says co-author Andrea Cicchetti of the National Institute for Astrophysics, Italy. “This would create something far denser than what we actually see with MARSIS. And when we modelled how different ice-free materials would behave, nothing reproduced the properties of the MFF – we need ice.”
The new results instead suggest layers of dust and ice, all topped by a protective layer of dry dust or ash several hundred metres thick.
Future exploration and collaboration
Although Mars now appears to be an arid world, the planet’s surface is full of signs that water was once abundant, including dried-up river channels, ancient ocean and lake beds, and water-carved valleys. We’ve also found significant stores of water ice on Mars, such as the enormous polar caps, buried glaciers nearer the equator, and near-surface ice laced through martian soil.
Massive stores of ice near the equator – such as those suspected to lurk below the dry surface of the MFF – couldn’t have formed in the planet’s present climate. They must have formed in a previous climate epoch.
“This latest analysis challenges our understanding of the Medusae Fossae Formation, and raises as many questions as answers,” says Colin Wilson, ESA project scientist for Mars Express and the ESA ExoMars Trace Gas Orbiter (TGO). “How long ago did these ice deposits form, and what was Mars like at that time? If confirmed to be water ice, these massive deposits would change our understanding of Mars climate history. Any reservoir of ancient water would be a fascinating target for human or robotic exploration.”
The extent and location of these icy MFF deposits would also make them potentially very valuable for our future exploration of Mars. Missions to Mars will need to land near the planet’s equator, far from the ice-rich polar caps or high-latitude glaciers. And they’ll need water as a resource – so finding ice in this region is almost a necessity for human missions to the planet.
“Unfortunately, these MFF deposits are covered by hundreds of metres of dust, making them inaccessible for at least the next few decades. However, every bit of ice we find helps us build a better picture of where Mars’s water has flowed before, and where it can be found today.”
While Mars Express maps water ice to a depth of a few kilometres, a view of near-surface water is provided by Mars orbiter TGO. This orbiter is carrying the FREND instrument, which is mapping hydrogen – an indicator of water ice – in the topmost metre of martian soil. FREND spotted a hydrogen-rich area the size of the Netherlands within Mars’s Valles Marineris in 2021, and is currently mapping how shallow water deposits are distributed across the Red Planet.
“Together, our Mars explorers are revealing more and more about our planetary neighbour,” adds Colin.
Notes for editors
The paper, ‘Evidence of Ice-Rich Layered Deposits in the Medusae Fossae Formation of Mars’ by T. R. Watters et al., is published in the journal Geophysical Research Letters.
MARSIS is Mars Express’s Radar for Sub-surface and Ionospheric Sounding. More information on MARSIS and the orbiter’s other instruments can be found via ESA’s Mars Express pages:
esa.int/Science_Exploration/Space_Science/Mars_Express/Mars_Express_orbiter_instruments
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