Kosmogeokemia

Kosmogeokemia is the study of the chemical composition and chemical processes of matter in the universe, from interstellar gas and dust to planets, moons, comets, and meteoritic material. The term reflects the integration of cosmology, geochemistry, and planetary science, focusing on how elements and isotopes are distributed, transformed, and transported across cosmic environments. While the exact term varies by language, it is commonly treated as a specialization within cosmochemistry and planetary geochemistry.

Methods used in kosmogeokemia combine observational and laboratory approaches. Astronomical spectroscopy, including optical, infrared, and radio observations, provides elemental and isotopic abundances in stars, nebulae, and the interstellar medium. Spacecraft missions and meteorite analysis yield physical samples for laboratory study. Laboratory techniques such as mass spectrometry, electron microscopy, and X-ray spectroscopy enable precise determinations of elemental and isotopic ratios, mineralogy, and trace constituents. Modeling of chemical evolution, nucleosynthesis, and planetary differentiation supports interpretation.

Key topics include the abundance patterns of elements and isotopes and their implications for stellar nucleosynthesis, solar system formation, and the inheritance of presolar materials. Research addresses how volatiles and organics are delivered to planets, the chemical evolution of protoplanetary disks, and the differentiation of planetary bodies. Studies often focus on meteorites, lunar and planetary rocks, cometary material, and the atmospheres of exoplanets.

Kosmogeokemia contributes to understanding the origin of the solar system, the distribution of elements in the cosmos, and the chemical conditions that influence planetary habitability. It faces challenges such as contamination control, interpreting isotopic anomalies, and translating astronomical observations into precise, laboratory-scale compositions.