10.05.2025

IQUID WATER WAS ABUNDANT ON MARS BEFORE ~3 BILLION YEARS AGO (LEFT) BUT VANISHED AS THE PLANET TRANSITIONED INTO THE COLD, DRY ENVIRONMENT WE SEE TODAY (RIGHT). 

This study is jointly completed by Dr. Weijia Sun (Institute of Geology and Geophysics, Chinese Academy of Sciences), Dr. Hrvoje Tkalčić (The Australian National University), Dr. Marco G. Malusà (University of Milano-Bicocca), and Dr. Yongxin Pan (Institute of Geology and Geophysics, Chinese Academy of Sciences).

Liquid water plays a crucial role in regulating the habitability of Mars. Liquid water was abundant on Mars during the Noachian and Hesperian periods (from the planet’s formation to about 3 billion years ago). However, during the Amazonian, it vanished from the surface as the planet transitioned into the cold, dry environment we see today. One of the greatest mysteries regarding water on Mars is whether liquid water exists at the present day within its crust and, if so, at what depth it is located. "The water involves profound questions about life and humanity’s future on the Red Planet," Tkalčić says.

The multidisciplinary team consisted of geophysicists and geologists. Sun, Tkalčić, Malusà, and Pan contemplated the possibility that the fine structure of the Martian crust is a potentially critical breakthrough for unravelling this scientific mystery. The team analyzed the seismic waveforms of the two largest meteorite impacts (S1000a and S1094b) and the largest marsquake (S1222a) recorded by NASA's InSight seismometer. Their results from seismic inversion reveal a significant low shear-wave velocity anomaly at a depth of 5.4–8 km, raising the possibility of liquid water at the base of the upper crust.

The team estimated a maximum water content of 520–780 meters of Global Equivalent Layer (the thickness of a water layer uniformly distributed across the entire surface of Mars), assuming the pores are entirely filled with liquid water. The research team wants to emphasize that this estimate is based solely on the geophysical inference of the local profile (variation of seismic speeds with depth) beneath the InSight lander without accounting for lateral structural variations we should expect realistically. Moreover, the hidden water’s volume estimate does not account for potentially primordial liquid water within the Martian crust. This finding can be validated by future missions equipped with seismometers on Mars.

The study provides seismic evidence for the presence of substantial liquid water in the upper Martian crust (5.4–8 km). These findings offer critical insights into the Martian water cycle and the evolution of its habitable environments and lay a crucial foundation for future research on the exploration of Martian life.

Quelle: AAAS