The discoveries provide valuable insights into the development of the lunar interior, with potential implications for planets like Earth or Mars.
Our understanding of the moon’s origins largely stems from the analysis of rock samples gathered by Apollo astronauts over half a century ago, along with theoretical models. These samples revealed unexpectedly high levels of titanium in basaltic lava rocks collected from the moon. Subsequent satellite observations showed that these titanium-rich volcanic rocks are mainly found on the moon’s nearside, yet the reasons behind their distribution have long puzzled scientists—until now.
Due to its rapid and hot formation, the moon likely had a global magma ocean covering its surface. As this molten rock cooled and solidified, it gave rise to the moon’s mantle and the luminous crust visible during a full moon. However, beneath the surface, the young moon was in a state of flux. Studies indicate that the remaining magma ocean solidified into dense minerals like ilmenite, a titanium and iron-containing mineral.
“Given that these dense minerals are heavier than the underlying mantle, they create a gravitational instability, causing this layer to sink deeper into the moon,” explained Weigang Liang, the lead researcher on this study conducted during his doctoral studies at LPL.
2024-04-09 07:00:03
Originally published on phys.org