The study, published as the inaugural article in the journal Space and Planetary Resources, was conducted by Kevin M. Cannon of Ethos Space Corp. and the Colorado School of Mines. Drawing on decades of laboratory analyses of nearly 400 martian meteorites and on in-situ measurements from the Spirit, Opportunity, Curiosity, Perseverance and Zhurong rovers, Cannon compiled the highest reported concentrations of 83 naturally occurring elements on Mars and compared them with the grades of ore deposits mined on Earth. The work arrives, he argues, at an inflection point between what may be the last large robotic science missions to Mars and the first serious steps toward commercialization and human landings.

A central theme of the analysis is that past discussions of planetary resources have often stumbled into logical errors that the terrestrial mining industry abandoned long ago. The most common is the presence-versus-absence fallacy: asking whether an element exists on Mars at all, when modern mass spectrometers can detect parts per trillion in virtually any material. What matters, Cannon stresses, is concentration, or grade, in a specific raw material at a specific location, because the energy and cost of extraction rise exponentially as grade falls. A gold mining company does not care how much gold is in Earth’s crust; it cares about the grade of a particular deposit. Similarly, the speciation of an element into separable ore minerals, such as zircon or monazite, versus lattice-bound substitutions in silicates, can make the difference between a practical resource and an impractical one.

The comparison baseline matters too. Average crustal composition is the wrong yardstick; martian concentrations must be measured against actual terrestrial ore bodies, which are enriched many orders of magnitude above bulk crust. When that comparison is made, the results span more than five orders of magnitude, with a median ratio of 27, meaning terrestrial ores are on average 27 times richer than the best-known martian materials. Six elements, including oxygen, sulfur, germanium, rubidium, argon and xenon, match or exceed the concentrations of the materials they are extracted from on Earth. Volatile elements such as sulfur, chlorine and bromine sit close to terrestrial ore grades, consistent with Mars having accreted from more volatile-rich building blocks. By contrast, the light metals lithium, beryllium and boron, the platinum group elements, the light rare earths, and the nuclear fuels thorium and uranium are orders of magnitude depleted in known martian samples.

Perhaps the most striking conclusions concern specific deposit types that rovers may have already brushed against. In Gale crater, ChemCam on the Curiosity rover detected copper enrichments throughout the stratigraphy of Mount Sharp, with the highest values in the Kimberley Formation. Detailed analysis suggests the copper occurs both in detrital grains of the potassic sandstones and adsorbed on manganese oxide coatings, pointing toward a porphyry copper or impact-hydrothermal deposit somewhere in the sediment source region. That would be a remarkable finding, because earlier theoretical work had specifically predicted that porphyry copper deposits should not exist on Mars, a prediction made before the discovery of evolved, potassic igneous lithologies and the full extent of ancient water-rock interaction on the planet.

At Jezero crater, the Perseverance rover has found strongly correlated nickel and copper enrichments in highly altered, aluminum-rich float rocks, with ore-grade values that support the long-standing prediction of Ni-Cu-PGE sulfide deposits associated with ultramafic volcanism. The region’s extensive olivine-rich unit, mapped from orbit and confirmed on the ground by an olivine cumulate outcrop on the crater floor, fits the terrestrial analog of large igneous provinces where such sulfide ores segregate from lava flows. Perseverance’s PIXL instrument has also detected lamellar bands of zirconium, titanium, chromium and phosphorus-bearing dense grains in deltaic sediments, evidence for heavy mineral lag deposits of the kind mined on Earth for ilmenite and zircon. Cannon notes that in all three cases the enriched materials were transported by water away from their sources, leaving only shadows of the original ore bodies, much as the California gold rush began in creek beds before prospectors traced the gold back to hard rock.

The quantitative picture is sharpened by extrapolation from element-element correlations in the meteorite collection. A single SuperCam point at Jezero reporting up to 2000 parts per million copper, if taken at face value, would predict roughly 2.2 parts per million ruthenium based on the meteorite correlation, exceeding typical terrestrial platinum-group ore grades even though the value falls below rover detection limits. Similarly, a PIXL spot measuring 1.4 weight percent zirconium, attributed to zircon or baddeleyite, implies about 362 parts per million hafnium, slightly above terrestrial ore values. These calculations suggest that ore-quality enrichments may already have been encountered on rover traverses, hidden below the sensitivity of onboard instruments, and that only a tiny fraction of the martian surface has been examined at all.

Mapping the indicators globally reveals a crucial geographic pattern. Olivine detections, potassium- and thorium-rich alkali terrains, aluminum clay exposures and fan-shaped sedimentary landforms, the best orbital proxies for sulfide, porphyry-like, leached and placer deposits respectively, cluster largely in equatorial regions such as Nili Fossae, Mawrth Vallis and eastern Valles Marineris. The mid-latitudes, where shallow ground ice is abundant, show a notable absence of these indicators, partly because younger lava flows, plains deposits and ice-dust mantles bury the ancient Noachian units where ores are most likely. This creates a potential tradeoff for settlement planning: if water is mined from ground ice, prospecting for metals may be pushed to marginal zones, but if water comes from hydrated minerals or other equatorial sources, the richest known mineral provinces become accessible. Atmospheric carbon dioxide and iron, available everywhere from regolith and iron meteorites, impose no such constraint.

Volumetrics remain a major uncertainty. The hematite-bearing unit at Meridiani Planum covers some 150,000 square kilometers, though its thickness is poorly known, while a native sulfur deposit recently discovered by Curiosity in Gediz Vallis has an estimated volume of 28,000 to 50,000 cubic meters. For the copper and nickel-copper signals at Gale and Jezero, the source deposits, if intact, likely exceed the transported materials in which they were detected, but elements like copper and nickel cannot yet be mapped from orbit. Cannon also flags unexplored geologic settings as prime targets for human fieldwork: evolved dacite terrains in Syrtis Major and the Eridania basin, impact-induced and magma-ice hydrothermal systems, speculative ancient seafloor deposits, and deeply leached aluminum clay stratigraphies like those at Mawrth Vallis, where extreme alteration hinted at by Jezero’s float rocks may have concentrated additional elements.

The bottom line is a sober but encouraging assessment. Mars falls between the Moon and Earth in its ore grades, as expected for a planet with intermediate geologic activity and water-rock interaction. Basic structural and industrial metals, including iron, aluminum, manganese, chromium, copper, zinc and titanium, show promising enrichments detectable with current orbital and geomorphologic data and should be prioritized for an initial settlement, while elements like lead, uranium and antimony are so depleted that substitution or import will likely remain necessary. As robotic exploration winds down and human missions approach, the study argues that the periodic table, not just the water cycle, must become the framework for choosing where on Mars to go and what to build when we get there.

Subject of Research: Assessment of non-volatile mineral and ore resources on Mars using meteorite and rover sample data

Article Title: Mineral resources of Mars based on decades of sample analysis

Article References: Cannon, K. M. (2025). Mineral resources of Mars based on decades of sample analysis. Space and Planetary Resources, 1(1), Article 1. https://doi.org/10.1007/s44461-025-00001-8

Image Credits: AI Generated

DOI: 10.1007/s44461-025-00001-8

Keywords: Mars, mineral resources, ore deposits, in-situ resource utilization, martian meteorites, Gale crater, Jezero crater, porphyry copper, Ni-Cu-PGE sulfides, heavy mineral sands, Perseverance rover, Curiosity rover

Shergottites, among the most studied Martian meteorites, date back to roughly 4.4 billion years. They originated from volcanic activity on Mars, making them invaluable for scientists aiming to decode the planet’s magmatic processes. The unique geochemical signatures within these rocks suggest that various geological environments contributed to their formation, signifying that Mars has undergone significant volcanic activity over a prolonged period. The study hypothesizes that the interaction between the Martian mantle and its crust has led to these varying magmatic types, thus offering substantial implications for our understanding of planetary evolution.

The researchers employed advanced analytical techniques, including isotopic analysis and geochemical modeling, to unravel the complexities of magmatic processes on Mars. By using high-resolution spectrometry and mass spectrometry, they were able to investigate the elemental compositions within the shergottites in considerable detail. Their findings indicate that Mars experienced multiple episodes of magmatism with distinct origins and melting processes, contradicting earlier theories that posited a more homogenous volcanic activity across the planet.

Open-system magmatism on Mars, in particular, appeared to be fueled by a continuous supply of fresh magma from the mantle. This process allows for the incorporation of crustal materials into the magma chamber, subsequently altering its composition before eruption. Such interaction emphasizes a dynamic recycling process within the planetary crust and mantle, contributing to the diversified composition noted in shergottites. Moreover, the continued release of gases during the melting processes provides a potential explanation for the atmospheric conditions during Mars’s early history, highlighting possible links to habitability.

Conversely, the closed-system magmatism suggests that some magma remained isolated from the crust, allowing it to evolve in a more controlled environment, unaltered by external influences. This process indicates that certain volcanic eruptions were influenced chiefly by the primary mantle compositions without significant crustal contamination. The implications of these findings suggest a more complex thermal and structural evolution of Mars than previously understood, hinting at the planet’s hotter beginnings amidst a transition toward today’s colder climate.

Furthermore, the study notes that the geochemical diversity in Martian magmatism has crucial ramifications for understanding planetary models beyond Mars. By revealing the interplay between open and closed systems, these findings encourage scientists to rethink the geological frameworks that govern not only Mars but potentially other terrestrial planets and exoplanets. The implications extend to astrobiology, where understanding the evolution of planetary conditions can illuminate the potential for life beyond Earth.

As researchers continue to investigate the stories bottled within Martian meteorites, they emphasize the potential for future missions to Mars. These missions could provide an even more comprehensive understanding of the planet’s geological history, leading to possible on-site analysis of the magmatic systems at play. Advances in rover technology and extraterrestrial material sampling could mark a new era in planetary science, focusing on understanding planetary systems as a whole rather than isolated phenomena.

The research team’s results have ignited discussions within the scientific community about the methodology used in the study of Martian meteorites. As they dive deeper into the parameters affecting magmatism, there is a call for enhanced collaborative efforts across disciplines, engaging geologists, planetary scientists, and astrobiologists alike in a quest to unravel the mysteries of the Red Planet. The exploration of shergottites promises to yield further insights that are not just historic but potentially life-altering in our ongoing quest to find life beyond Earth.

Beyond the specific nuances of Mars’s geology, this research presents an opportunity to reflect on the significance of studying planetary materials as windows into not only the solar system’s formation but also the conditions that led to the emergence of life on Earth. This study serves as a powerful reminder of how much we still have to learn about our neighboring planet and the quest to comprehend the origins and evolution of life in our universe.

With the increasing availability of advanced technologies and better scientific tools, the future looks bright for ongoing and new explorations of Mars’s geology. Scientists are optimistic that future findings—enriched by these new understandings—will unravel even more about the dynamics of planetary formation and the rules governing volcanic activity across various celestial bodies. Partners in the academic community continue to monitor the developments arising from this research closely, anticipating the exciting prospects that may arise from it.

The multifaceted nature of Martian magmatism uncovered in this study signifies an evolving landscape of planetary science, where new theories can profoundly shift our understanding of geology, atmospheres, and the potential for life. With each new discovery, we are one step closer to forming a coherent picture of Mars’s past—one that may hold the keys to unearthing the broader overarching principles of planetary science for Earth and beyond.

The revelations surrounding Martian magmatism through the lens of shergottites lay the groundwork for future inquiries into other planetary phenomena. This study epitomizes the significance of meteorite research as a critical field in understanding not only Mars but also our place in the cosmos. We live in a transformative era of space exploration, where interplanetary research is shedding light on profound cosmic questions, bridging gaps between geology, astronomy, and astrobiology.

As we look to the future, the ongoing investigations of Martian meteorites carry the promise of exciting discoveries that will continue to evolve our understanding of the solar system. Each analysis of the geological intricacies within these materials brings us closer to unmasking the Red Planet’s enigmatic past, inviting researchers and enthusiasts alike to engage in the remarkable quest to learn more about our stellar neighborhood.

Subject of Research: Martian Magmatism

Article Title: Open- versus closed-system magmatism on Mars revealed by shergottites

Article References:

Peel, C.J., Howarth, G.H., Costin, G. et al. Open- versus closed-system magmatism on Mars revealed by shergottites.
Commun Earth Environ (2025). https://doi.org/10.1038/s43247-025-03026-1

Image Credits: AI Generated

DOI: 10.1038/s43247-025-03026-1

Keywords: Magmatism, Mars, Shergottites, Volcanology, Planetary Geology