Thematic Articles

Illuminated Worlds: How Spectroscopy Lights the Way in Earth and Planetary Sciences

The study of minerals under light, spanning the ultraviolet, visible, infrared (UV-Vis-IR) spectrum, has played an important role in advancing our understanding of terrestrial and extraterrestrial materials. Here, we review light-based spectroscopic techniques across spatial scales in mineralogy and planetary science. Polarized light microscopy helps characterize optical properties, while vibrational and UV-Vis spectroscopies provide insights into mineral structures and compositions. In mineral physics, spectroscopy probes bonding environments, electronic structure, phase transitions, and elastic properties at high pressures and temperatures. In planetary science, UV-Vis-IR techniques from spacecraft and telescopes reveal planetary mineralogy. These methods support the search for habitable environments, planetary evolution studies, and resource identification. Furthermore, technological advances in portability, imaging, and data analysis have improved the precision and scope of mineralogical research.

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From Atoms to Planets: The Physics of Minerals Across Scales

Mineral science emerged from humanity’s earliest curiosity about the colors, hardness, and magnetic properties of stones and metals. Across centuries, observations by philosophers, naturalists, and early microscopists gradually revealed that these macroscopic traits arise from the hidden architecture of matter. The scientific revolutions of the 17th–20th centuries—from crystallography and optics to quantum mechanics and high-pressure experimentation—established the atomic foundations of minerals and transformed mineralogy into a modern physical science. Today, mineral physics links nuclei, electrons, defects, and crystal structures to the behavior of Earth and planetary interiors. This sets the stage for this Elements issue, showing how insights across disciplines continue to shape our understanding of minerals from atoms to planets.

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Burned or Buried: What Controls the Long-term Preservation of Organic Carbon?

The preservation of organic carbon (OC) in marine sediments is a fundamental control on Earth’s long-term carbon cycle and climate. Globally, less than 2% of carbon fixed by primary producers is ultimately buried, yet specific environments and geological intervals exhibit markedly enhanced preservation. These variations reflect changes in organic matter composition, mineral associations, microbial activity, geochemical conditions, temperature, and sediment transport. Planetary-scale changes in climate, tectonics, continental configuration, biological evolution, and ocean circulation have repeatedly altered these controls, promoting enhanced OC burial during key periods of Earth history. OC preservation has thus acted as an important stabilizing feedback following major carbon-cycle perturbations. Here, we examine these mechanisms and their significance through time.

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The Fate of Ocean Alkalinity: Carbonate Formation and Reverse Weathering Reactions

The ocean’s buffering capacity, or alkalinity, regulates the amount of atmospheric CO2 the ocean can sequester. Typically, it is assumed that the formation of carbonate minerals is the only sink for ocean alkalinity. However, in recent years, the formation of alumino-silicate phases in the seabed via reactions that consume alkalinity and produce CO2 (reverse weathering) has been shown to be significant in the modern ocean and is thought to provide a control on the long-term C cycle. Evolutionary changes in the modes of carbonate production and the availability of certain seawater constituents are also important controls on CaCO3 formation beyond the flux of alkalinity into the ocean. Here we explore the links between biogeochemical cycles, seawater chemistry, and alkalinity sinks.

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The Role of Seawater Interaction with the Ocean Floor in the Carbon Cycle

Seawater circulation through oceanic crust acts as an essential sink for CO2 and affects the alkalinity budget of the ocean. Seafloor weathering and ridge flank hydrothermal activity contribute to modern carbon sequestration by taking up carbon at a rate < 0.5 Tmol y−1. In addition, these processes release < 1 Tmol y−1 alkalinity to the ocean. During warmer eras in Earth history, the carbon uptake rates were considerably higher. Estimates range between 2.1 and 3.4 Tmol y−1 during the Cretaceous and Jurassic. The more intense carbonation of the seafloor in the Mesozoic is due to higher temperatures and less pelagic sedimentation in the deep ocean. Accelerated rates of reaction between seawater and basalt and prolonged durations of exposure of igneous crust to seawater led to more intense basalt alteration and carbonate formation within the crust. The interactions between oceanic crust and seawater hence profoundly influence global carbon cycling on long time scales.

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Continental Weathering as Climate Stabilizer

Conventional wisdom on Earth’s long-term habitability relies on a negative feedback loop among climate, silicate weathering, and atmospheric CO2 concentrations. Essentially, climate modulates the rate of CO2 consumption associated with silicate weathering, which in turn stabilizes climate through the greenhouse effect of atmospheric CO2. This review assesses the efficacy of continental weathering as a climate stabilizer, including the supply of bedrock available for weathering, the influences of atmospheric oxygenation and land-plant colonization on weathering efficiency, and CO2-emitting weathering processes that may counteract the negative feedback associated with silicate weathering. Basalt weathering plays a key role in mitigating these constraints, as it can sustain a large weathering-derived CO2 sink and has exhibited a high sensitivity to climatic changes through much of the Earth’s history.

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Igneous and Metamorphic CO₂ Sources: How Large and How Variable?

Igneous and metamorphic processes play a critical role in the geological carbon cycle and Earth’s long-term habitability by transferring carbon between rocks and the ocean–atmosphere system. The magnitude of these carbon fluxes, both in the present day and throughout Earth’s history, remains poorly constrained. Traditional models link carbon degassing to riverine bicarbonate fluxes, but these approaches rely on the questionable assumption that the modern system is in steady-state. Here, we summarize the current state of research on quantifying igneous and metamorphic carbon fluxes using direct measurements, geochemical proxies, and ancient rock records. We also examine the spatial and temporal variability of these processes, which is crucial for understanding their influence on Earth’s carbon cycle over geological timescales.

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How Well Do We Understand the Geological Carbon Cycle?

The foundation of our understanding of the geological carbon cycle, and how this acts as Earth’s “thermostat,” was articulated in a seminal paper in 1981 (Walker et al). They suggested that silicate weathering on the continents acts as a stabilizing feedback on the carbon cycle such that increased atmospheric pCO2 leads to increased weathering rates and hence increased removal of CO from the atmosphere. This “textbook model” is at the core 2 of most models of long-term biogeochemical cycles. We summarize evidence that there are many other processes in the geological carbon cycle that may be equally or more important than those in the Walker model. We argue there is a need to move beyond the textbook model in both teaching and research.

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Assembling Pangaea – The Complex Morphology of the Laurussia – Gondwana Collision

The Late Paleozoic convergence and collision between Gondwana and Laurentia resulted in along-strike variations in the Alleghanian–Mauritanide–Variscan orogeny during the assembly of the greater part of Pangaea. A series of ca. 380–290 Ma events segmented the orogen into two principal geodynamic domains with contrasting tectonic evolutions. In the northeast, the European Variscan belt records multiple subduction–collisional tectonic events, including indentation by Laurussian and later Gondwanan promontories and by Gondwana-derived terranes. Late-stage events (330–290 Ma) produced strongly curved deformation belts (oroclines), and late- to post-orogenic extension. In contrast, the southern Appalachians formed southwest of the promontory collisions where subduction of Rheic Ocean remnants produced a continuous Andean-style orogenic arc that preceded ca. 290 Ma terminal collision. We explain Pangaea amalgamation using a global model of mantle convection like that of modern Earth.

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Granites and the Nature of the Variscan Crust

The orogenic crust of the European Variscan belt is granite-rich and only locally has a mafic lower layer. The core of the belt originated by massive melting of fertile quartzo–feldspathic sources (felsic meta-sedimentary or meta-igneous) derived from an Ediacaran–Ordovician accretionary system. An unusually felsic lower crust formed either by relamination of previously subducted continental crust or by melting of crustal rocks to produce a granitic upper crust and a laminated, restitic lower crust. This is in strong contrast to conventional models, developed mainly for magmatic arcs, that find or infer mafic lower crustal compositions. Thus, global estimates on the nature and evolution of the continental crust should consider the heterogeneity of the deep crust produced in various types of orogenies.

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December 2025 --The Variscan Orogeny in Europe – Understanding Supercontinent Formation

The Variscan orogen formed between 380 and 300 million years ago through several accretionary and collisional cycles, culminating with the construction of the Pangea supercontinent. This process occurred via sequential opening and closure of oceanic basins, synchronous detachment of Gondwana derived continental ribbons, and their outboard amalgamation onto the Laurussia margin. The Variscan orogen is rather unique compared with other orogenic belts on Earth: its overthickened and dominantly magmatic crust in the central belt, surprisingly minor mantle involvement in the magmatic and geodynamic processes, coherent and pulsed magmatism along the collision suture, and its complex accretionary history. Because its final product, Pangea, is the youngest and best-understood supercontinent on Earth, the Variscan orogeny offers clues for understanding the mechanisms of supercontinent formation.