Understanding the Martian Atmosphere-Geosphere Interactions Using Oxygen Isotopic Forensics

Recent missions to Mars have shown that the planet might have hosted liquid water based on the morphological characteristics of its lithosphere. Information about the evolution of Martian surface and atmosphere is obtained via the study of Martian meteorites. Unlike Earth, Martian geosphere does not appear to be well mixed and bulk silicates show a range of oxygen isotope anomalies from 0.3 to 0.6 0/00. In order to understand this anomaly an experiment was designed with Mars simulant, liquid water and ozone to reproduce the unique $\Delta^{17}$O isotopic value uniquely characteristic of Martian meteorites. This quantity is used as a tracer of the reaction pathways occurring on the surface of Mars. We believe that only in the presence of these three ingredients can the specific value be achieved. By simulating the chemical processes occurring on the surface of Mars, we seek to understand the interactions of Martian hydrosphere, atmosphere and geosphere. This study is unique for the advancement of cutting edge research in the evolution of planetary atmosphere and surfaces, and the search for liquid water. The oxygen triple isotopic analysis is a tool that provides us with clues for discovering the geochemical history of the red planet.