About this Research Topic
Secondary minerals are formed by processes such as weathering and crystallization after the primary formation of rocks. These minerals shape the evolution toward the planetary equilibrium and provide essential insights into geological history, environmental conditions, and habitability. The geological significance of secondary minerals in studying planetary evolution is multi-fold: clays, sulfates, and carbonates indicate past or present aqueous environments, providing critical evidence for the planet's climate history. These water-related minerals assist in mapping the distribution of ancient water bodies through information obtained by orbital explorers and field rovers. When combined with the information derived from laboratory analogs and geochemical models, it is possible to understand crystallization mechanisms and compare them with known processes on Earth. Some secondary minerals can preserve organic molecules, acting as a time capsule and offering opportunities for studying organic chemistry and investigating the possibility of past or present life on a planetary body.
While fundamental chemical and thermodynamic principles apply universally to mineral formation, the specific processes involved in the formation of secondary minerals in the solar system can differ significantly from those on Earth due to variations in environmental conditions and energy sources. The direct applicability of the so-called "actualism principle" to extreme conditions or unique geological histories of other celestial bodies might be challenging in certain situations that we cannot extrapolate to Earth. Although thermodynamics favors mineral weathering, the most suitable reactions remain poorly explored in a planetary context. Modeling approaches and laboratory experiments indicate that conversions of primary minerals to carbonates and clays are the most likely pathways for interacting gaseous atmospheres with surface minerals. However, silicates' conversion to secondary phases can be inhibited without aqueous phases or modified by kinetic constraints. This issue discusses the formation of sulfides, sulfates, carbonates, or clays in contexts like Enceladus, Europa, Titan, Venus, or Mars, where the crystallization processes may significantly differ from Earth.
We acknowledge contributions dealing with the study of secondary minerals across various celestial bodies, enabling scientists to compare and contrast the geological processes and histories of these objects. This comparative approach may contribute to a broader understanding of planetary evolution within the solar system. We encourage submissions based on the following:
• Spectral data from orbital probes and field data collected by rovers;
• Terrestrial analogs;
• Geochemical modeling (specifically those based on kinetic approaches);
• Laboratory experiments performed using specially developed devices.
• Novel analyses of the experimental data provided by the rovers, with a particular focus on the cases of Curiosity and Perseverance on Mars.
While fundamental chemical and thermodynamic principles apply universally to mineral formation, the specific processes involved in the formation of secondary minerals in the solar system can differ significantly from those on Earth due to variations in environmental conditions and energy sources. The direct applicability of the so-called "actualism principle" to extreme conditions or unique geological histories of other celestial bodies might be challenging in certain situations that we cannot extrapolate to Earth. Although thermodynamics favors mineral weathering, the most suitable reactions remain poorly explored in a planetary context. Modeling approaches and laboratory experiments indicate that conversions of primary minerals to carbonates and clays are the most likely pathways for interacting gaseous atmospheres with surface minerals. However, silicates' conversion to secondary phases can be inhibited without aqueous phases or modified by kinetic constraints. This issue discusses the formation of sulfides, sulfates, carbonates, or clays in contexts like Enceladus, Europa, Titan, Venus, or Mars, where the crystallization processes may significantly differ from Earth.
We acknowledge contributions dealing with the study of secondary minerals across various celestial bodies, enabling scientists to compare and contrast the geological processes and histories of these objects. This comparative approach may contribute to a broader understanding of planetary evolution within the solar system. We encourage submissions based on the following:
• Spectral data from orbital probes and field data collected by rovers;
• Terrestrial analogs;
• Geochemical modeling (specifically those based on kinetic approaches);
• Laboratory experiments performed using specially developed devices.
• Novel analyses of the experimental data provided by the rovers, with a particular focus on the cases of Curiosity and Perseverance on Mars.
Keywords: urey reaction, mars weathering, clays, sulfides, oxides, clathrates, europa, titan, enceladus, Actualism in geology, carbonates on Mars
Important Note: All contributions to this Research Topic must be within the scope of the section and journal to which they are submitted, as defined in their mission statements. Frontiers reserves the right to guide an out-of-scope manuscript to a more suitable section or journal at any stage of peer review.
