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1. A new model of the Earth system nitrogen cycle: how plates and life affect the atmosphere

   Johnson, Benjamin W; Goldblatt, Colin (October 2017, Habitable Worlds 2017)

   Nitrogen is the main component of Earth’s atmosphere. Nitrogen plays a key role in the evolution of the biosphere and surface of Earth [1]. There are contrasting views, however, on how N has evolved on the surface of the Earth over time. Some modeling efforts [e.g., 2] indicate a steady-state level of N in the atmosphere over geologic time, while geochemical [e.g., 3], other proxies [e.g., 4], and more recent models [5] indicate the mass of N in the atmosphere can change dramatically over Earth history. This conundrum, and potential solutions to it, present distinct interpretations of the history of Earth, and teleconnections between the surface and interior of the planet have applications to other terrestrial bodies as well. To help investigate this conundrum, we have constructed an Earth-system N cycle box model. To our knowledge, this is the most capable model for addressing evolution of the N reservoirs of Earth through time. The model combines biologic and geologic processes, driven by a mantle cooling history, to more fully describe the N cycle through geologic history. In addition to a full biologic N cycle (fixing, nitrification, denitrification), we also dynamically solve for PO4 through time and we have a prescribed O2 history. Initial model results indicate that the atmosphere of Earth could have experienced major changes in mass over geologic time. High initial atmospheric mass, suggested as a solution to the Faint Young Sun Paradox [1], is drawn down over time, supports work that indicates the mantle has significantly more N than the atmosphere does today [6]. Importantly, the amount of N in the atmosphere today is directly dependent on the total N mass in the silicate Earth. Thus, given some assumptions, the atmosphere itself may be a proxy for total planetary N. References: Use the brief numbered style common in many abstracts, e.g., [1], [2], etc. References should then appear in numerical order in the reference list, and should use the following abbreviated style: [1] Goldblatt et al. (2009) Nat. Geosci., 2, 891-896. [2] Berner, R. (2006) Geology., 34, 413-415. [3] Barry, P.H. and Hilton (2016) Geochem. Persp. Letters, 2, 148-159. [4] Som, S.M. et al. (2016) Nat. Geosci., 9, 448-451. [5] Stueken et al. (2016) Astrobiology, 16, in press. [6] Johnson et al. (2015) Earth Science Reviews, 148,150-173. 

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2. A halogen budget of the bulk silicate Earth points to a history of early halogen degassing followed by net regassing

   https://doi.org/10.1073/pnas.2116083118  

   Guo, Meng; Korenaga, Jun (December 2021, Proceedings of the National Academy of Sciences)

   Halogens are important tracers of various planetary formation and evolution processes, and an accurate understanding of their abundances in the Earth’s silicate reservoirs can help us reconstruct the history of interactions among mantle, atmosphere, and oceans. The previous studies of halogen abundances in the bulk silicate Earth (BSE) are based on the assumption of constant ratios of element abundances, which is shown to result in a gross underestimation of the BSE halogen budget. Here we present a more robust approach using a log-log linear model. Using this method, we provide an internally consistent estimate of halogen abundances in the depleted mid-ocean ridge basalts (MORB)-source mantle, the enriched ocean island basalts (OIB)-source mantle, the depleted mantle, and BSE. Unlike previous studies, our results suggest that halogens in BSE are not more depleted compared to elements with similar volatility, thereby indicating sufficient halogen retention during planetary accretion. According to halogen abundances in the depleted mantle and BSE, we estimate that ∼87% of all stable halogens reside in the present-day mantle. Given our understanding of the history of mantle degassing and the evolution of crustal recycling, the revised halogen budget suggests that deep halogen cycle is characterized by efficient degassing in the early Earth and subsequent net regassing in the rest of Earth history. Such an evolution of deep halogen cycle presents a major step toward a more comprehensive understanding of ancient ocean alkalinity, which affects carbon partitioning within the hydrosphere, the stability of crustal and authigenic minerals, and the development of early life. 

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3. Lithological Heterogeneities in the Mantle: Origins and Contributions to Magma Genesis (Keynote 3a)

   https://doi.org/10.46427/gold2020.1405  

   Lambart, Sarah; Lang, Otto (January 2020, Goldschmidt 2020)

   null (Ed.)

   The quantification of the mantle heterogeneity and its contribution to magma genesis are crucial for our understanding of the nature of Earth’s geochemical reservoirs and recycling processes. Today, the source of basalts is often envisioned as a heterogeneous mantle that comprises a range of lithological heterogeneities, especially pyroxenites, introduced into the mantle by various geodynamic and magmatic processes. Different chemical parameters have been proposed to trace evidence for the contribution of lithological heterogeneities during magma genesis (e.g., major elements1-2, major element ratios1,3 or logratios4, first row transition element concentrations5-6, iron isotopes7) and several empirical models for partial melting of a heterogeneous mantle have been developed in an attempt to quantify the proportion of pyroxenites in the mantle source of magmas8-11. However, the large range of compositions covered by the potential lithologies present in the mantle makes it challenging to determine a unique proxy for their contributions in the magmas2,12. Additionally, these contributions are controlled by various factors, such as the abundances of the different lithologies in the mantle, their respective melting behaviors (solidus temperatures and melt productivities) and the thermal and melting regimes of the mantle. Finally, interpretations from the magma compositions are complicated by the potential presence of volatiles in the mantle source and/or by modifications experienced by the magmas during their journey through the mantle8,12. This keynote presentation will present examples of challenges that can rise when we try to quantify the nature and abundance of the mantle heterogeneity, the efforts that have been published by various authors, and a few potential research directions that could bring prospects for success. 1- Hauri (1996), Nature 382, 2- Lambart et al. (2013), Lithos 160-161, 3- Hirschmann et al. (2003), Geology 31, 4- Yang et al. (2019), JGR-Solid Earth 124, 5- Sobolev et al (2007), Science 316, 6- Sobolev et al. (2008), Science 321, 7- Williams and Bizimis, EPSL 404, 8- Mallik and Dasgupta (2014), GGG 15, 9- Kimura and Kawabata (2015), GGG 16, 10- Lambart et al. (2016), JGR-Solid Earth 121, 11- Brown and Lesher (2016), GGG 17, 12- Mallik et al. (in press), in: Konter J., Ballmer M, Cottaar S, & Marquardt H. (Eds. ), AGU monograph. 

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4. Carbonation and decarbonation reactions: Implications for planetary habitability

   https://doi.org/10.2138/am-2019-6884  

   Stewart, E.M.; Ague, Jay J.; Ferry, John M.; Schiffries, Craig M.; Tao, Ren-Biao; Isson, Terry T.; Planavsky, Noah J. (October 2019, American Mineralogist)

   Abstract The geologic carbon cycle plays a fundamental role in controlling Earth's climate and habitability. For billions of years, stabilizing feedbacks inherent in the cycle have maintained a surface environment that could sustain life. Carbonation/decarbonation reactions are the primary mechanisms for transferring carbon between the solid Earth and the ocean–atmosphere system. These processes can be broadly represented by the reaction: CaSiO3 (wollastonite) + CO2 (gas) ↔ CaCO3 (calcite) + SiO2 (quartz). This class of reactions is therefore critical to Earth's past and future habitability. Here, we summarize their significance as part of the Deep Carbon Obsevatory's “Earth in Five Reactions” project. In the forward direction, carbonation reactions like the one above describe silicate weathering and carbonate formation on Earth's surface. Recent work aims to resolve the balance between silicate weathering in terrestrial and marine settings both in the modern Earth system and through Earth's history. Rocks may also undergo carbonation reactions at high temperatures in the ultramafic mantle wedge of a subduction zone or during retrograde regional metamorphism. In the reverse direction, the reaction above represents various prograde metamorphic decarbonation processes that can occur in continental collisions, rift zones, subduction zones, and in aureoles around magmatic systems. We summarize the fluxes and uncertainties of major carbonation/decarbonation reactions and review the key feedback mechanisms that are likely to have stabilized atmospheric CO2 levels. Future work on planetary habitability and Earth's past and future climate will rely on an enhanced understanding of the long-term carbon cycle. 

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5. Discovery of davemaoite, CaSiO ₃ -perovskite, as a mineral from the lower mantle

   https://doi.org/10.1126/science.abl8568  

   Tschauner, Oliver; Huang, Shichun; Yang, Shuying; Humayun, Munir; Liu, Wenjun; Gilbert Corder, Stephanie N; Bechtel, Hans A.; Tischler, Jon; Rossman, George R. (November 2021, Science)

   Calcium silicate perovskite, CaSiO 3 , is arguably the most geochemically important phase in the lower mantle, because it concentrates elements that are incompatible in the upper mantle, including the heat-generating elements thorium and uranium, which have half-lives longer than the geologic history of Earth. We report CaSiO 3 -perovskite as an approved mineral (IMA2020-012a) with the name davemaoite. The natural specimen of davemaoite proves the existence of compositional heterogeneity within the lower mantle. Our observations indicate that davemaoite also hosts potassium in addition to uranium and thorium in its structure. Hence, the regional and global abundances of davemaoite influence the heat budget of the deep mantle, where the mineral is thermodynamically stable. 

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