Oxford University scientists have proposed a new explanation for the longstanding conundrum: what happened to the water on Mars?
Although today the Martian surface is barren, frozen and inhabitable, evidence points to a once warmer, wetter planet, where water flowed freely. New research published in Nature suggests that this water is locked in the Martian rocks.
Conducted by scientists at Oxford’s Department of Earth Sciences, the research suggests that the planet’s surface reacted with the water and then absorbed it, oxidising the surface rocks in the process.
Previous research has suggested that the majority of the water on Mars was lost to space as a result of the collapse of the planet’s magnetic field, when it was either swept away by high intensity solar winds or locked up as sub-surface ice. However, these theories do not explain where all of the water has gone.
Convinced that the planet’s mineralogy held the answer to this puzzling question, a team led by Dr Jon Wade, NERC Research Fellow in Oxford’s Department of Earth Sciences, applied modelling methods used to understand the composition of Earth rocks, to calculate how much water could be removed from the Martian surface, through reactions with rock. The team assessed the role that rock temperature, sub-surface pressure and general Martian make-up, have on the planetary surfaces.
The results revealed that the basalts on Mars can hold approximately 25 per cent more water than those on Earth, and as a result drew the water from the Martian surface into its interior (mantle).
Dr Wade said: ‘People have thought about this question for a long time, but never tested the theory of the water being absorbed as a result of simple rock reactions. There are pockets of evidence that together, leads us to believe that a different reaction is needed to oxidise the Martian mantle. For instance, Martian meteorites are chemically reduced compared to the surface rocks, and compositionally look very different. One reason for this, and why Mars lost all of its water, could be in its mineralogy.
‘The Earth’s current system of plate tectonics prevents drastic changes in surface water levels, with wet rocks efficiently dehydrating before they enter the Earth’s relatively dry mantle. But neither early Earth nor Mars had this system of recycling water. On Mars, water reacting with the freshly erupted lavas that form its basaltic crust, resulted in a sponge-like effect where the planet’s water reacted with the rocks forming a variety of water bearing minerals. This water-rock reaction changed the rock mineralogy and caused the planetary surface to dry and become inhospitable to life.’
As to the question of why Earth has never experienced these changes, he said: ‘Mars is much smaller than Earth, with a different temperature profile and higher iron content of its silicate mantle. These are only subtle distinctions but they cause significant effects that, over time, add up. They made the surface of Mars more prone to reaction with surface water and able to form minerals that contain water. Because of these factors the planet’s geological chemistry naturally drags water down into the mantle, whereas on early Earth hydrated rocks tended to float until they dehydrate.’
The overarching message of Dr Wade’s paper, that planetary composition sets the tone for future habitability, is echoed in new research also published in Nature, examining the Earth’s salt levels. Co-written by Professor Chris Ballentine of Oxford’s Department of Earth Sciences, the research reveals that for life to form and be sustainable, the Earth’s halogen levels (Chlorine, Bromine and Iodine) have to be just right. Too much or too little could cause a sterile environment. Previous studies have suggested that halogen levels in the early Earth were much higher, based on samples taken from meteorites. Ballentine et al were able to prove that those original estimates were simply too high.
The two studies combined support a case for further investigation. Dr Wade said ‘Broadly speaking the inner planets in the solar system have similar composition, but subtle differences can cause dramatic differences – for example, rock chemistry. The biggest difference being, that Mars has more iron in its mantle rocks, as the planet formed under marginally more oxidising conditions.’
When searching for life, what sustains it, one clue may be to look for a water source that has ideally been on the surface for a long time. The Earth is 4.5 billion years old and has apparently had surface water for almost the entire time. Without water, the planet would become barren and no life would survive. We know that Mars once had water, and the potential to sustain life, but by comparison little is known about the other planets, and the team are keen to change that.
Dr Wade said: ‘To build on this work we want to test the effects of other sensitivities across the planets – very little is known about Venus for example. Questions like: what if the Earth had more or less iron in the mantle, how would that change the environment? What if the Earth was bigger or smaller? These answers will help us to understand how much of a role rock chemistry determines a planet’s future fate.
‘When looking for life on other planets it is not just about having the right bulk chemistry, but also very subtle things like the way the planet is put together, which may have big effects on whether water stays on the surface. These effects and their implications for other planets have not really been explored.’
Paper: The divergent fates of primitive hydrospheric water on Earth and Mars was published in Nature by Jon Wade, Brendan Dyck, Richard M. Palin, James D. P. Moore & Andrew J. Smye
The supporting paper citation is Halogens in chondritic meteorites and terrestrial accretion, by Patricia L. Clay, Ray Burgess, Henner Busemann, Lorraine Ruzié-Hamilton, Bastian Joachim, James M. D. Day & Christopher J. Ballentine, published in Nature DOI:10.1038/nature24625
Image credit: James Moore and Jon Wade