Volcanic eruptions that look like single events are often the visible outcome of slow, complicated activity taking place deep underground. Beneath the surface, magma shifts position, changes chemically, and can sit for long stretches before finally erupting. To piece together what is happening below, scientists examine lava flows, rock textures, and minerals left behind at the surface. These clues help reveal the hidden magma systems that drive volcanic activity.
A recent study published in Geology shows that this same complexity exists on Mars. High resolution images of the landscape and mineral measurements collected from orbit indicate that some of the planet’s youngest volcanic regions have a much more detailed history than previously assumed. Instead of forming during brief, one time eruptions, these volcanoes were built by magma systems that remained active and changed over extended periods beneath the martian surface.
Study Focuses on Volcanic System Near Pavonis Mons
An international team of researchers from Adam Mickiewicz University in Poznań, the School of Earth, Environment and Sustainability (SEES) at the University of Iowa, and the Lancaster Environment Centre examined a long lasting volcanic system located south of Pavonis Mons, one of the largest volcanoes on Mars. By pairing careful surface mapping with mineral data gathered from orbiting spacecraft, the scientists reconstructed how the volcano and its underlying magma system developed over time with remarkable precision.
“Our results show that even during Mars’ most recent volcanic period, magma systems beneath the surface remained active and complex,” says Bartosz Pieterek of Adam Mickiewicz University. “The volcano did not erupt just once — it evolved over time as conditions in the subsurface changed.”
Multiple Eruptive Phases Traced by Mineral Signatures
The analysis revealed that the volcanic system progressed through several stages. Early activity involved lava spreading out from fissures in the ground, while later eruptions came from more focused vents that built cone shaped features. Although these lava deposits look different today, they were all fed by the same underlying magma reservoir. Each phase left behind a unique mineral fingerprint, allowing researchers to track how the magma’s composition shifted over time.
“These mineral differences tell us that the magma itself was evolving,” Pieterek explains. “This likely reflects changes in how deep the magma originated and how long it was stored beneath the surface before erupting.”
Orbital Data Offers Rare Insight Into Mars Interior
Since scientists cannot yet collect rock samples directly from Martian volcanoes, studies like this offer valuable information about the planet’s interior. The findings demonstrate how powerful orbital observations can be for uncovering the hidden structure and long term evolution of volcanic systems, both on Mars and on other rocky worlds.
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