New Insights into Martian Interior
A team from the University of Oxford has presented evidence that Mars historically possessed extensive magmatic systems beneath its crust. These structures resemble those formed on Earth through plate tectonics, even though Mars is generally considered tectonically inactive.
The study, published in Nature Astronomy on June 26, relies on geophysical measurements and modeling derived from data collected by various Mars missions. Findings indicate that large volumes of molten rock existed deep underground and may have remained active for prolonged periods.
Key support comes from seismic analyses that reveal subsurface density and temperature variations, as well as chemical signatures in volcanic deposits pointing to sustained magmatic activity.
This revelation prompts renewed discussion about early Martian climate and habitability. Magmatic processes can release heat and volatiles essential for atmospheric development and the presence of liquid water.
While the exact mechanisms enabling such systems without plate tectonics remain under investigation, the research opens new avenues for understanding the geological evolution of terrestrial planets.