Ten years at Mars: New global views plot the red planet's history

Jun 03, 2013
Operations and science highlights from ESA’s Mars Express mission, which celebrated 10 years since launch on 2 June 2013. The central image of Mars is composed from images taken by the High Resolution Stereo Camera (HRSC) images, which has mapped around 95% of the planet’s surface. The images of Phobos and Deimos were also taken by the HRSC. Credit: Images of Mars, Phobos & Deimos: ESA/DLR/FU Berlin (G. Neukum)

(Phys.org) —New global maps of Mars released on the 10th anniversary of the launch of ESA's Mars Express trace the history of water and volcanic activity on the Red Planet, and identify sites of special interest for the next generation of Mars explorers.

The unique atlas comprises a series of maps showing the distribution of minerals formed in water, by , and by weathering to create the dust that makes red. They create a global context for the dominant that sculpted the planet we see today.

The maps were built from ten years of data collected by the OMEGA mineralogical mapper on , which determines the of the by analyzing the spectrum of reflected sunlight.

"The history of Mars is encoded in its minerals," says Alvaro Giménez, ESA's Director of Science and . "These new global views, made possible thanks to the longevity of ESA's Mars Express mission, are helping us to unlock the secrets of 4.6 billion years of .

"The atlas released today will help to determine future landing sites for the next generation of Mars landers and rovers, and identify sites of special interest for future , helping to keep Europe at the forefront of ."

Each map represents a different chapter in the story of on Mars.

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This unique atlas comprises a series of maps showing the distribution and abundance of minerals formed in water, by volcanic activity, and by weathering to create the dust that makes Mars red. Together the maps provide a global context for the dominant geological processes that have defined the planet’s history. The maps were built from ten years of data collected by the OMEGA visible and infrared mineralogical mapping spectrometer on Mars Express. The animation cycles through maps showing: individual sites where a range of minerals that can only be formed in the presence of water were detected; maps of olivine and pyroxene, minerals that tell the story of volcanism and the evolution of the planet’s interior; and ferric oxide and dust. Ferric oxide is a mineral phase of iron, and is present everywhere on the planet: within the bulk crust, lava outflows and the dust oxidised by chemical reactions with the martian atmosphere, causing the surface to ‘rust’ slowly over billions of years, giving Mars its distinctive red hue. The map showing hydrated minerals includes detections made by both ESA’s Mars Express and by NASA’s Mars Reconnaissance Orbiter. Copyright Hydrated mineral map: ESA/CNES/CNRS/IAS/Université Paris-Sud, Orsay; NASA/JPL/JHUAPL; Olivine, pyroxone, ferric dust & dust maps: ESA/CNES/CNRS/IAS/Université Paris-Sud, Orsay Orsay; Video production: ESA.

Maps Showing The Distribution Of Minerals Formed In Water

The first map shows individual sites of —'phyllosilicates' and hydrated salts that form only in the presence of water. These are primarily seen in the most ancient cratered terrain dating back to over four billion years ago, suggesting that Mars sustained surface and subsurface liquid water during its first few hundred million years, potentially providing conditions favorable to early life.

Maps Showing The Distribution Of Minerals Formed By Volcanic Activity

The next two maps showing the minerals olivine and pyroxene tell the story of volcanism, with differences in the chemical composition of the solidified lavas yielding clues as to the evolution of the temperature and pressure inside the planet.

Olivine and pyroxene are the two primary minerals in basalt that form when lava solidifies. Basalt characterizes the crust of Mars as well as oceanic crust on Earth and the volcanic 'seas' on the Moon.

Some of the most pristine, magnesium-rich olivines exposed on the surface of Mars today are found around impact craters that have excavated samples of very ancient mantle from beneath the crust.

Olivine-rich surfaces are also associated with a global lava-flooding event around 3.7 billion years ago, when magma erupted onto the surface through fractures in the floors of impact craters, similar to the way in which the Moon's large impact basins were flooded with volcanic lava. Only a few traces of this global event remain today, with subsequent geological activity overprinting the signature.

Pyroxenes are particularly widespread in the cratered highlands, pointing to some of the most ancient portions of the planet's crust. In the smooth northern plains, the pyroxenes reflect the eruption of more evolved lavas compared to the pristine olivines.

Maps Showing The Distribution Of Dust Created By Weathering

Dust obscures much of the underlying rock on Mars, but it is very closely related to ferric oxide, a mineral phase of iron found all over the planet, with greatest abundances in the northern lowlands and the volcanic province of Tharsis.

The Red Planet's dust is thought primarily to result from chemical reactions with the atmosphere, causing the iron-rich rocks to 'rust' slowly over billions of years, giving Mars its distinctive hue.

Weathering and erosion from past glacial activity and impact events, as well as dust storms, winds and freezing and thawing cycles today, contribute to the continued production of fine-grained dust.

"Collectively, these mineral maps provide unique records of the planet's evolution through time. They exhibit the role water and volcanic processes played over the entire planet, spanning geological aeons," says Jean-Pierre Bibring, Principal Investigator for OMEGA.

Maps Providing Hints For Future In-Situ Exploration

The maps also highlight areas of particular scientific interest that may warrant further in-situ exploration, such as the abundance of hydrated mineral exposures clustered along the boundary between the low northern plains and the ancient cratered highlands.

"Against the flanks of these cliffs, thick ice deposits may have preserved ancient water-altered sites for a longer period of time than in more exposed locations," says Professor Bibring.

In some places, the maps show an overlap between volcanic outcrops and hydrated minerals: here, minerals may have become altered via heating during volcano-ice interactions.

One such location, known as Nili Fossae, is identifiable by the obvious bright red/yellow spot in the olivine map, a mineral easily weathered into clay in the presence of water. If rocks here were altered by hydrothermal activity, then conditions may have once existed there to support life.

"These are very special sites—possibly unique within the entire solar system—with well preserved records of the environment during the few hundreds of millions of years following planet formation, during which life might have emerged on Earth and possibly at Mars," adds Professor Bibring.

Ten Years Of Discovery

In addition to the tantalizing tale of the history of water and volcanism on the surface, Mars Express has also been conducting a wide range of studies of the Red Planet, from the subsurface all the way up to the upper atmosphere and beyond to Mars' two tiny moons, Phobos and Deimos, providing an in depth analysis of all aspects of the Martian environment.

Over 95% of the surface has been imaged by the mission's high-resolution camera, with two thirds mapped at a resolution of 20 m per pixel or better, and much of it in stereo, yielding stunning 3D images.

Ground-penetrating radar has added a third dimension to the planet by determining the vertical extent of the polar ice caps. At the south pole, there is enough water locked up in ice to cover the entire planet with a layer of water 11 m deep if melted.

Meanwhile the detection of traces of methane in the atmosphere has led to an intense debate in the scientific community: does it have a volcanic origin, or could it be the result of active biology, as it is on Earth?

Mars Express has also provided the most detailed atlas of its innermost moon Phobos, and in December this year will make its closest pass yet, just 58 km from the center of the tiny moon.

"The decade-long observations by Mars Express of all aspects of the Martian environment are providing us with a truly global perspective on the history of the Red Planet, paving the way for the next generation of Mars exploration missions," says Olivier Witasse, ESA's Mars Express Project Scientist.

"But we still have a lot to look forward to and are planning a number of unique observations with Mars Express, such as coordinating measurements of the atmosphere with NASA's MAVEN spacecraft, watching the very close pass of Comet C/2013 Siding Spring by Mars in October 2014, and monitoring the arrival of ESA's ExoMars Entry, Descent, and Landing Demonstrator module in October 2016."

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More information: Related Papers

"Global maps of anhydrous minerals at the surface of Mars from OMEGA/MEx," by A. Ody et al., is published in the Journal of Geophysical Research 117, (2012).

"Global investigation of olivine on Mars: Insights into crust and mantle compositions," by A. Ody et al., is published in the Journal of Geophysical Research, 118 (2013).

"Hydrous minerals on Mars as seen by the CRISM and OMEGA imaging spectrometers: Updated global view," by J. Carter et al., is published in the Journal of Geophysical Research 118 (2013).

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