gunung api di Mars

The Martian landscape, long perceived as a geologically quiet world, is revealing hidden complexities beneath its surface. New research focusing on Pavonis Mons, one of the largest volcanoes on Mars, suggests its volcanic history is far more intricate and prolonged than previously understood. This discovery challenges conventional thinking about volcanic activity on the Red Planet and offers fresh insights into the planet’s internal dynamics.

For years, volcanic eruptions were often visualized as singular events – magma rising, erupting and then subsiding. However, a recent study published January 29, 2026, in the journal Geology, demonstrates that Martian volcanoes, at least in the case of Pavonis Mons, experienced extended periods of activity, evolving over time and gradually reshaping the surrounding terrain. This research provides a new lens through which to view the formation and evolution of not only Pavonis Mons but potentially other volcanic regions on Mars.

The study, led by Bartosz Pieterek of Adam Mickiewicz University, combined detailed surface mapping with orbital mineral data to reconstruct the volcanic and magmatic evolution of the region south of Pavonis Mons with unprecedented detail. This approach allowed researchers to trace the history of magma movement and changes within the volcano over extended periods. “Our results show that even during Mars’ most recent volcanic period, magma systems beneath the surface remained active and complex,” explained Dr. Pieterek. “The volcano did not erupt just once – it evolved over time as conditions in the subsurface changed.”

From Fissure Eruptions to Cone-Forming Vents

The research reveals that the volcanic system south of Pavonis Mons developed through multiple eruptive phases. Initially, lava flowed through long fissures, spreading widely across the surface. Over time, volcanic activity became more concentrated, focusing on single points and creating cone-forming vents. While these different lava flows appear distinct on the surface, the study confirms they were all supplied by the same underlying magma system. This suggests a dynamic interplay between magma supply, pressure, and the evolving structure of the volcano.

Crucially, each phase of eruption left behind unique “mineral fingerprints.” Variations in mineral composition provide scientists with valuable clues about how the magma itself changed over time. “These mineral differences tell us that the magma itself evolved,” Dr. Pieterek stated. “It likely reflects changes in the depth of the magma’s origin and how long it was stored beneath the surface before erupting.” Pavonis Mons, standing 8.7 km (5.4 mi) tall, is strategically positioned along the Martian equator, between longitudes 235°E and 259°E, as part of the Tharsis Montes chain of volcanoes.

Peering into Mars’ Interior Without Direct Samples

Unlike Earth, scientists currently lack the ability to directly sample the interior of Martian volcanoes. Orbital observations are the primary means of understanding the processes occurring beneath the surface. This makes studies like Pieterek’s particularly valuable, offering a rare glimpse into the structure and evolution of the planet’s interior. The Tharsis Montes volcanoes, including Pavonis Mons, lie along the crest of a northeast-trending rise known as the Tharsis bulge, which extends more than 3,000 km across the western equatorial region of Mars.

“Because direct sampling of Martian volcanoes is currently impossible, studies like this provide a rare insight into the structure and evolution of the planet’s interior,” Pieterek explained. The findings underscore the importance of continued orbital exploration and the development of advanced analytical techniques to unravel the mysteries hidden within the Martian landscape.

Further research will focus on refining the timeline of volcanic activity at Pavonis Mons and exploring the potential connections between subsurface magma dynamics and broader geological features on Mars. Understanding the complex history of Martian volcanism is crucial for reconstructing the planet’s past climate and assessing its potential for past or present habitability.

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