Thematic Articles

Sanbagawa Subduction: What Went in, How Deep, and How Hot did it Get?

The Sanbagawa belt is a “coherent” oceanic subduction-type metamorphic region representing a rock package predominantly derived from oceanic crust and accreted at depths of 20–80 km (300–700 °C). The thermal structure and lithological layers are complexly deformed but semi- continuous, in contrast to more commonly reported subduction-related domains dominated by mélange. The coeval Shimanto accretionary complex records accretion at depths <15 km and the rocks are primarily terrigenous sediments. The Sanbagawa belt has a greater proportion of mafic rocks than the Shimanto complex, implying progressive peeling-off of oceanic plate stratigraphy with more basaltic oceanic crust slices accreted at deeper levels. Tectonic exhumation can be explained by three separate phases dominated by buoyancy-driven upflow, ductile thinning, and normal faulting.

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Paired Metamorphism of SW Japan and Implications for Tectonics of Convergent Margins

The Sanbagawa-Ryoke pair of geological units in southwest Japan is the classic example of paired metamorphism originally identified by Akiho Miyashiro. Together these belts represent an important study area for developing and testing ideas about how convergent margins behave over geological time based on studies of the rock record including petrology, geochemistry, deformation, and geochronology. The two sides of the pair represent ancient examples of a subduction zone in the Sanbagawa belt and an associated volcanic arc in the Ryoke belt. This issue of Elements brings together the results of a wide range of different approaches summarizing the current state of knowledge about the Sanbagawa-Ryoke pair and how this informs our understanding of convergent margins in general.

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Analytical Techniques for Identification and Characterization of Extraterrestrial Organic Matter

Advances in analytical techniques are essential for understanding the nature, formation, and evolutionary history of extraterrestrial organic matter. In this chapter, we briefly review analytical techniques used to detect and characterize organic matter in extraterrestrial materials. Mass spectrometry is often coupled with gas chromatography or liquid chromatography for elemental and isotopic analysis, and for identifying specific organic compounds. Spectroscopy involves interaction of molecules with electromagnetic radiation at various wavelengths. Almost every wavelength—from X-rays to radio waves—can be used for spectroscopic measurements. The most major microscopic and nanoscopic techniques are scanning and/or transmission electron microscopy. Spectroscopy and mass spectrometry can also be coupled with microscopic analysis for detailed compositional investigations.

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Asteroidal Organics from the Sample Return Mission Hayabusa2 and their Implication for Understanding our Origins

The C-type asteroid Ryugu samples returned by the Hayabusa2 spacecraft are the chemically most pristine material in the Solar System, as they have not been exposed to terrestrial environments. The organic matter in Ryugu records the molecular evolution from the Sun’s parent molecular cloud chemistry to asteroidal aqueous alteration. In this article, we review the results of Ryugu sample analysis and discuss the evolution of organic matter in the early Solar System by comparing these results with recent radio and infrared observations of protostars and protoplanetary disks.

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Diversity of Complex Organic Matter in Carbonaceous Chondrites, IDPs, and UCAMMs

Complex organic matter is present in many extraterrestrial materials such as chondrite meteorites, micrometeorites, and interplanetary dust. The observed complexity of this organic matter is due to the combination of diversity of primitive organic materials that accreted onto asteroids and the subsequent effect of hydrothermal and/or metamorphic alteration that took place after accretion. These processes resulted in a variety of carbonaceous grain morphologies, elemental abundances, and organic functional group compositions. Some carbonaceous dust grains and micrometeorites have cometary origins and provide insights into the unique processing histories on those outer Solar System bodies. Isotopic analyses can help distinguish carbonaceous grains that retain their pre-accretion heritage, while advanced microscopy techniques reveal the interplay of complex organic matter with surrounding mineral.

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Delivery of Organic Matter to the Early Earth

The inner Solar System—including the planet Earth—was heavily bombarded by comets, asteroids, and their fragments (i.e., meteorites, micrometeorites, and interplanetary dust particles) from 4.56 to about 3.5 billion years ago. This bombardment resulted in a rich assortment of organics delivered to the Earth, as comets and many asteroids contain carbonaceous material. These organic compounds were likely further processed on the early Earth (e.g., by impact-shock reactions), providing a feedstock of prebiotic molecules to the crust and oceans. In this chapter, we review the mechanisms of organic matter delivery to the primitive Earth, further reactions and processing, and the importance of exogenous material in the evolution of our planet and life.

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Formation and Evolution Mechanisms for Organic Matter in Space

Organic compounds are a major component of dust in molecular clouds, alongside silicates and water ice, due to the high abundances of elements that make up these compounds in the Galaxy. The initial molecular inventory of the Solar System, inherited from the molecular cloud, was modified and new complex molecules were formed in the protoplanetary disk and planetesimals. Because astronomical observations mainly target gas, while cosmochemical evidence deals with solid phases, it is crucial to link discrepant knowledge on organic species through state-of-the-art modeling. This chapter reviews the latest understanding of surface reactions on inter- stellar dusts, gas–dust reactions in the protoplanetary disk, and alteration processes on planetesimals in the early Solar System.

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Extraterrestrial Organic Matter: An Introduction

Extraterrestrial organic matter forms in a variety of locations in space through different mechanisms. Its nature, distribution, formation mechanisms and locations are of particular interest. Some organic molecules can even be considered as key players for the emergence of life. Although new organic species are continuously detected in the interstellar media, Solar System bodies, and extraterrestrial materials, their formation and evolution are still not fully understood. Ground-based and space observations can detect organic matter in different objects with a range of complexity and diversity, while laboratory investigations of astromaterials allow detailed characterization of extraterrestrial organic matter with high precision. This issue reviews different aspects of extraterrestrial organic matter, including its origin, evolution, diversity, and delivery.

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Uncertainty and Value: Optimising Geometallurgical Performance Along the Mining Value Chain

To maximise the value of a mining operation and minimise its environ- mental and social impacts, all processes—from the ore deposit to the final product and waste streams—should be optimised together. However, mining and metallurgical processes are inherently variable and uncertain due to the natural heterogeneity of ore deposits and the limited information and incomplete models available on ore behaviour throughout the process chain. Propagating these effects to geometallurgical models is important because they are used to make decisions with potentially large environmental and economic impacts. In this paper, we describe the need for geometallurgical optimisation routines to account for the effects of uncertainties, and the tools needed to manage them, by summarising the routines that already exist and those that are still missing.

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Action Versus Reaction: How Geometallurgy Can Improve Mine Waste Management Across the Life-Of-Mine

The raw materials industry produces billions of tonnes of mine waste per year. Given increasing metal demand and the global appetite for waste reduction, strategic opportunities to minimise its production must be embedded across the life-of-mine. Adopting a geometallurgical approach to total deposit characterisation—where mineralogical and geochemical data are routinely collected and used to model geoenvironmental domains—offers profound benefits for improving the understanding of the composition and environmental impact of different residues. Using established and emerging technologies, from handheld instruments and core scanners to synchrotrons, throughout a mine’s life—starting already during exploration—may assist the raw materials industry to reduce their waste footprint and adopt circular economy principles.

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