We present an innovative, cost-effective framework integrating laboratory Hyperspectral Imaging (HSI) of the Bechar 010 Lunar meteorite with ground-based lunar HSI and supervised Machine Learning (ML) to generate high-fidelity mineralogical maps. A 3 mm thin section of Bechar 010 was imaged under a microscope with a 30 mm focal length lens at 150 mm working distance, using 6x binning to increase the signal-to-noise ratio, producing a data cube (X × Y × λ = 791×1024×224, 0.24 mm × 0.2 mm resolution) across 400 nm to 1000 nm (224 bands, 2.7 nm spectral sampling, 5.5 nm full width at half maximum spectral resolution) using a Specim FX10 camera. Ground-based lunar HSI was captured with a Celestron 8SE telescope (3 km/pixel), yielded a data cube (371×1024×224). Solar calibration was performed using a Spectralon reference (99% reflectance < 2% error) ensured accurate reflectance spectra. A Support Vector Machine (SVM) with a radial basis function kernel, trained on expert-labeled spectra, achieved 93.7% classification accuracy (5-fold cross-validation) for olivine (92% precision, 90% recall) and pyroxene (88% precision, 86% recall) in Bechar 010. LIME analysis identified key wavelengths (e.g., 485 nm, 22.4% for M3; 715 nm, 20.6% for M6) across 10 pre-selected regions (M1 to M10), indicating olivine-rich (Highland-like) and pyroxene-rich (Mare-like) compositions. SAM analysis revealed angles from 0.26 rad to 0.66 rad, linking M3 and M9 to Highlands and M6 and M10 to Mares. K-means clustering of Lunar data identified 10 mineralogical clusters (88% accuracy), validated against Chandrayaan-1 Moon mineralogy Mapper (M3) data (140 m/pixel, 10 nm spectral resolution). A novel push-broom HSI approach with a telescope achieves 0.8 arcsec resolution for lunar spectroscopy, inspiring full-sky multi-object spectral mapping.

Biohydrometallurgical processing of spent lithium-ion batteries offers a low-impact route for critical metal recovery compared with conventional hydrometallurgy. In this work, the iron-oxidizing bacterium Acidithiobacillus ferrooxidans was evaluated for the bioleaching of cobalt (Co), nickel (Ni), lithium (Li) and copper (Cu) from pyrolyzed industrial black mass derived primarily from LiCoO2-based batteries, containing both LiCoO2 and LiNiO2 layered oxide phases. Batch experiments were conducted in 9K medium at 30 degrees C, varying pulp density (1%-2%, w/v), inoculum volume (10-20 mL in 200 mL medium) and initial pH (with and without adjustment). At 1% pulp density and 10% v/v inoculum, metal recoveries after 6-7 days reached about 64%-70% Co, 57%-72% Ni, 52%-60% Li and 81%-100% Cu, with most dissolution occurring in the first 6 days. Higher inoculum loads without initial pH adjustment increased Li recovery up to 79%, but did not further improve Co and Cu, indicating a trade-off between microbial activity, metal toxicity and ferric iron availability. The temporal evolution of pH and metal dissolution is consistent with indirect redoxolysis by biogenic Fe3+ and sulfuric acid generated during ferrous iron and elemental sulfur oxidation. Overall, the results confirm the feasibility of A. ferrooxidans-assisted bioleaching as a green option for Co, Ni, Li and Cu recovery from spent LiCoO2 batteries and provide operating windows for subsequent process optimization and scale-up.

The Blue Earth Project (BEP), an initiative led by the Network of Researchers on the Chemical Emergence of Life (NoRCEL) convenes global public forums to explore the guiding question: How can discussions and recommendations from the Blue Earth Project influence politicians and voters in democracies? As climate change, biodiversity loss, and ecological degradation intensify, the need for inclusive, ethically grounded scientific discourse has never been greater. This paper outlines the theoretical basis, public value, and democratic relevance of BEP, making the case for its role in supporting evidence-based, citizen-informed policymaking. By integrating perspectives from science, ethics, and public participation, BEP serves as a model for engaging democratic societies in shaping planetary futures.

Metamorphic soles are key petrotectonic units that offer valuable insights into the processes governing ophiolite emplacement on continental margins (obduction). In this work, we have investigated the metamorphic sole of the Pindos ophiolite in northwestern Greece. In the studied locality, the sole is sandwiched between mantle peridotites and pillow lavas of N-MORB affinity. Our study focuses on two lithologies from the metamorphic sole: a garnet-mica schist (metapelite) and a mafic amphibolite. Kinematic indicators from the garnet-mica schists are consistent with top-to-the-NE shearing of the Pindos ophiolite on the Pelagonian zone. Petrographic and textural evidence, geothermometry results (FeMg garnet-biotite exchange and paragonite-muscovite solvus thermometry), and phase-equilibria modelling bracket the upper-limit of metamorphism at amphibolite-facies conditions (630 +/- 20 degrees C and 1.1 +/- 0.2GPa). Moreover, Quartz-in-Garnet (QuiG) barometry yields a pressure of similar to 1.2GPa for 630 degrees C demonstrating the equilibration of garnet inclusions at high-pressure conditions. New Ar-40/Ar-39 dating results from syn-kinematic muscovite from the metapelite and amphibole from the amphibolite indicate an apparent minimum age of 164.16 +/- 0.37 Ma and a consistent age plateau at 165.5 +/- 0.73 Ma respectively. Notably, the amphibole exhibits no evidence of argon loss. The muscovite age, by contrast, should be considered a minimum apparent age due to the potential influence of argon diffusion. Finally, UPb geochronology of garnet was dominated by inclusions and did not result in a meaningful age. The measured ages imply cooling rates for the Pindos metamorphic sole ranging from 60 to 625 degrees C/Ma.

The recent return of samples from asteroid 162173 Ryugu provides a first insight into early Solar System prebiotic evolution from known planetary bodies. Ryugu's samples are CI chondrite-like, rich in water and organic material, and primarily composed of phyllosilicate. This phyllosilicate surrounds micron to submicron macromolecular organic particles known as insoluble organic matter. Using advanced microscopy techniques on Hayabusa-2 samples, we find that aqueous alteration on Ryugu produced organic particles richer in aromatics compared to less altered carbonaceous chondrites. This challenges the view that aromatic-rich organic matter formed pre-accretion. Additionally, widespread diffuse organic material occurs in phyllosilicate more aliphatic-, carboxylic-rich, and aromatic-poor than the discrete organic particles, likely preserving the soluble organic material. Some organic particles evolved to encapsulate phyllosilicate, indicating that aqueous alteration on Ryugu led to the containment of soluble organic matter within these particles. Earth therefore has been, and continues to be, delivered micron-sized polymeric organic objects containing biologically relevant molecules. Studies of samples of asteroid Ryugu returned by the Hayabusa-2 mission show that the action of water and organic material on carbonaceous asteroids lead to the widespread occurrence of micron-sized polymeric organic particles encapsulating clays and biological relevant molecules.

This study reviews major sensing technologies for the Lunar environment and its resources, as they have been developed since the times of Apollo missions. Selected technologies of sensors and instruments for the chemical, isotopic, and structural analysis of Lunar rocks and regoliths, as well as of the Lunar exosphere environment, are presented in a critical review towards an optimised and information-rich framework. Special focus is given on the activated Lunar regolith, and especially the Lunar dust, describing the development of Lunar simulants as the only accessible materials for experimentation and testing of the above technologies. New technologies are also highlighted, such as the development of the OxR microfluidic and spectroscopy integrated device, which, in its small scale aims to detect reactive oxygen species in the Lunar regolith, while in its larger format it is used to release oxygen gas from the Lunar dust and regolith, enabling astronaut respiration and fuel production on the Moon. It is finally suggested that miniaturisation of instruments and sensors, together with the standardisation of output information and characterisation protocols through holistic informational frameworks, will enhance the dynamic expansion and further integration and interoperation of sensors and devices, aiming to an efficient, safer, and resilient utilisation on the Moon and the establishment of sustainable settlements in the near future.

The invention of the laser has pushed the boundaries of technological advancements with its variety of uses. This use case chapter analyses the implementation of an Autonomous Laser-Induced Breakdown Spectroscopy System for Chemical and Mineralogical Designation of Interplanetary Materials. In more detail, it highlights all the major components of the development of an autonomous system that maps the material composition of a meteorite sample using the Laser-Induced Breakdown Spectroscopy method. In the first chapter all key concepts are presented while offering a short literature survey regarding (calibration-free) Laser-Induced Breakdown Spectroscopy. It also highlights the use of the Robot Operating System (ROS) as a tool for the implementation of hardware drivers and autonomy components. Continuing with the details of the implementation, the manuscript focuses on the reference and description of all major hardware components. In the third chapter, the software components of the implementation are discussed. These components include hardware drivers, autonomy capabilities, data visualisation and user interfacing. For interested readers, chapter four offers a quick tutorial on compiling, configuring and running the implemented software. Chapter five summarises the experimental setup and presents results. Finally, this chapter concludes with a quick summary and an overview of the limitations of the implementation along with future work.

Bauxite residue (BR) is the main by-product of the alkaline production of alumina from bauxite containing significant amounts of valuable metals such as scandium that belongs to rare-earth elements (REEs), classified by the European Community as critical raw materials (CRMs). BR is considered a hazardous waste due to its huge volume and high alkalinity making its disposal a serious universal environmental problem. The recovery of scandium from Greek BR can be an excellent approach for waste management and resource efficiency of the waste using environmentally friendly biometallurgical methods. In this work, bioleaching of scandium from bauxite residue using the fungus Aspergillus niger was studied. Bioleaching experiments were performed using the Taguchi experimental design, in batch cultures with BR at various pulp densities (1, 5 and 10%, w/v), sucrose concentrations (40, 90 and 140 g/L) and fungus suspension of 2, 4, and 6% v/v under one-step bioleaching condition and subculturing. The highest Sc recovery equal to 46%, was achieved in 20 days at 1% pulp density. Biosorption phenomena were observed during the leaching process. Lactic, acetic, oxalic and citric were the main organic acids identified. Graphical Abstract

Meteor plasmas and impact events are complex, dynamic natural phenomena. Simulating these processes in the laboratory is, however, a challenge. The technique of laser induced dielectric breakdown was first used for this purpose almost 50 years ago. Since then, laser-based experiments have helped to simulate high energy processes in the Tunguska and Chicxulub impact events, heavy bombardment on the early Earth, prebiotic chemical evolution, space weathering of celestial bodies and meteor plasma. This review summarizes the current level of knowledge and outlines possible paths of future development.

The AstroScience Exploration Network (ASEN) is the latest innovative initiative from the Network of Researchers on the Chemical Emergence of Life (NoRCEL). Materializing on the vibrancy of the African continent, recognizing its people as a key asset, and building on specific strategic advantages, ASEN will funnel the appetite for scientific knowledge through an educational hub that paves the way for the Global South to come to the fore in new global endeavors and will eventually help build a variety of career paths in a diversifying economy.

We studied the occurrence of secondary minerals and inferred their formation in the Yamato-000593 Martian meteorite using multiple technological approaches such as electron probe micro analysis, optical microscope, Raman spectroscopy, scanning electron microscopy, as well as Fourier transform-infrared microscopy and spectroscopy. Two separate hydrothermal alteration events and their sequence of formation (based on superpositional relationship) can be identified: an elevated temperature phase producing high-temperature sulfidic hydrothermal alteration and a lower temperature hydrothermal alteration phase by iron-rich fluids. This meteorite shows signatures more compatible with magmatic effects, rather than impact-induced hydrothermal alteration, as has been proposed earlier. The sulfidic alteration probably formed by magmatic hydrothermal fluids, whereas iron-rich hydrothermal fluid circulation after a possible early impact event has also been proposed, when the fluids cooled down to 50 degrees C. Most of the secondary minerals formed at alkaline-neutral conditions, and the few observed signatures (clay-silica-bearing veins, siderite-iron-oxide veins) of briny conditions are probably from local spatial effects in larger cavities. The ferrous minerals (hematite and siderite) along the fractures could be crystallized from Fe-HCO3-bearing fluids. Alternatively, the primary magmatic minerals could have been oxidized easily (Fe-rich olivines, magnetite) during the cooling to iron oxides (hematite, goethite). The results suggest the possible existence of at least ephemerally habitable environments on Mars, mainly at volcanically heated locations. Following published geochemical models, the carbonates formed within acidic-circumneutral condition, which was followed by formation of phyllosilicates in alkaline condition.

The analysis of the Csatalja H4 chondrite (which was found in August 2012) suggests shock-related textures and spatial inhomogeneities, indicating a complex geological history. In the most heavily fractured and sheared units, small opaque grains and older fractures have locally enhanced the shock effect, producing melt. While the impact textures were evident in most units of the meteorite, mechanical shearing is apparent in only two units, suggesting that these units might have been present at somewhat different locations inside the parent body. Shearing also occurred at the border of the so-called xenolith unit, confirming its mechanical mixing with the other units. Besides fragmentation and melting, chemical changes due to impact have also been identified, producing compositional homogenization of olivines in 30% of the investigated area of the sample's thin section (23 mm(2)), and moderate accumulation of Fe, Ca, and Na in the strongly shocked zones, initiating crystallization of feldspar in veins with a specific spatial distribution (feldspar glass with metal-sulfide globules). Analyzing the high P-T minerals, the peak shock pressure and temperature values differed substantially in the various units, ranging between 2 and 17 GPa, 100 and >1200 degrees C. The xenolith unit crystallized more slowly after the impact event and does not show shock impact alterations, suggesting that it was formed in a deeper region of the parent body. This was later shifted to its current surroundings and was lithified (fixed) to the rest of the sample. This "randomly selected" Csatalja sample provides information on the range of the formation temperatures, pressures, and processes that contributed to the heterogeneity of meteorites at the mm spatial scale, in general. The identified heterogeneity is a result not purely of the shock effects but also of the different pre-shock structural characteristics. The shock also mixed fragments mechanically that have been formed at different environments, with at least several dozens or even 100 m depth in the parent body.

Abstract The polarising microscope is the most common and basic tool for geologists to study rocks and minerals in thin sections. The analysis and processing are mainly qualitatively when conventional methods are used. Nevertheless, due to technological development and evolution, the use of digital methods makes the petrographic studies much easier, reliable, and quantitative. In this paper, we describe a method to characterise the petrographic microscope based on its setup (i.e., nicols, lenses, light source). For the characterization procedure, a spectrometer has been used in order to acquire the spectrum of microscope’s light source, based on the different microscope’s components and setups, including the use of plane polarised, crossed polarised and circular polarised light conditions, from which the Correlated Colour Temperature (CCT) was computed. It is shown that the individual microscope setups have a direct effect on light source spectrum and therefore on the CCT value. This procedure is vital when image processing techniques are combined with traditional petrography interpretations for quantitative measurements. Technological applications can also be on materials showing birefringence, such as liquid crystals, polymeric fluids, thin films, plastics, optical fibres, and biological samples such as collagen and some proteins.

Introduction: The interest for the Moon has risen with many missions being planned for the Moon surface culminating to the Artemis missions, spearheading a new era of human presence on the lunar surface. At the same time a recent paper (1) provided an overview of the current state of Martian research and understanding. A common theme on both of these endeavors is the requirement of extensive research across the fields of astrobiology, the frontier of ISRU technologies and habitability research under simulated conditions of those environments. A large number of Lunar and Martian Simulants has been developed over the past decades, often though produced rapidly with lower fidelity to satisfy demand (2). Towards this purpose, our group made an effort to develop such materials, since in Greece only potentially analogue locations for simulated research exists. This research was initiated with the introduction of a new simulant classification system, after having highlighted a number of issues that pertain on the facet of Martian Simulants. We here report on the development of new simulants we produced for the Lunar and Martian surfaces. Methodology: Initially, we scrutinised the literature focusing on three focal points of research to collect data on the composition of Lunar and Martian surface location, the Lunar Curator Facility, the Analyst’s Notebook and the respective publications on simulant production, in order to identify which datasets have been already utilised. Based on these data, we selected one Lunar and two Martian locations to produce simulants. For the Moon we selected the 15260 Apollo Sample which has been extensively studied. (3) For Mars, we opted for the Rocknest and Gobabeb targets, which are 2 of the most cited and compared sites for simulant production. More specifically, for Moon we utilised the chemical analysis provided by (3) and for Mars those provided by (4). For the simulant development we collected a number of igneous rock samples from the field, and acquire a number of pure mineral phases, for use as individual components, presented in table 1. All of the materials utilised by our team in the synthesis of the simulants have been firstly crushed and grounded to a grain fraction of under 1 mm. A portion of the material was further crushed in under 250 μm, and later refined for XRD analysis. Each sample was then scanned in three random locations via SEM-EDS and the average analysis was taken as the sample’s chemistry. Thus, via those two analytical techniques, the background of the chemical and mineralogical make up of our inventory of materials was established. In order to establish the quality of our simulants we utilised the Figure of Merit (FOM) proposed by (5) and applied by (6). By using this system you can deduce the accuracy of your simulant based on how close the percentages of chemical oxides are to the reference sample. Simulants: Up to the point of writing, our team has produced a total of four simulants, two for the Moon and two for Mars. Initially a production of two prototypes for a Lunar and Martian simulant, Simulant #1 and #2 respectively, were made by mixing three individual mineral and rock components to verify the method of synthesis and correct any mistakes. However, even at that stage the theoretical FOM of our Simulant #1 was above 95% when compared to the Apollo 15260 sample, and Simulant #2 for Mars had FOM 90,7% and 89% for the Rocknest and Gobabeb targets respectively. (Table 1) Based on the preliminary results we produced refined simulants, Simulant #3 and #4 for Moon and Mars respectively, using additional components materials as showed in table 1. Thus, Simulant #3 for the Apollo 15260 sample reached FOM of almost 96% and Simulant #4 for Mars reached FOM of 94,6% and 91,6% for the Rocknest and Gobabeb targets, respectively. (Table 1) Future Goals: The goal of this project is to try and make simulant materials for Moon and Mars more accessible to the scientific community, but also provide materials of higher fidelity and accuracy. Based on their chemistry, the FOM values on the martian simulants are higher than those presented in (6), suggesting that our endeavor has significant prospects compared with the fidelity of other simulants and providing the confidence that higher accuracy simulants can be synthesised. Furthermore, an additional number of analytical techniques will be used to verify their fidelity. Additionally, by the acquisition of additional mineral phases and rock samples we are targeting to increasing the FOM values. A short term requirement is also the availability of well-known simulants in order to be used in the OxR ESA project (7). References: * H. G. Changela et al., Mars: new insights and unresolved questions. International Journal of Astrobiology, 1-33 (2021). * G. H. Peters et al., Mojave Mars simulant—Characterization of a new geologic Mars analog. Icarus 197, 470-479 (2008). * A. Duncan et al. (1975) Interpretation of the compositional variability of Apollo 15 soils. in Lunar and Planetary Science Conference Proceedings, pp 2309-2320. * C. Achilles et al., Mineralogy of an active eolian sediment from the Namib dune, Gale crater, Mars. Journal of Geophysical Research: Planets 122, 2344-2361 (2017). * C. Schrader et al. (2009) Lunar regolith characterization for simulant design and evaluation using figure of merit algorithms. in 47th AIAA Aerospace Sciences Meeting Including the New Horizons Forum and Aerospace Exposition, p 755. * L. E. Fackrell, P. A. Schroeder, A. Thompson, K. Stockstill-Cahill, C. A. Hibbitts, Development of Martian regolith and bedrock simulants: Potential and limitations of Martian regolith as an in-situ resource. Icarus 354, 114055 (2021). * ESA (2022) https://www.esa.int/Enabling_Support/Space_Engineering_Technology/Moon_and_Mars_superoxides_for_oxygen_farming. Table 1. Simulant components and Figure of Merit percentages.

Bauxite residue, the high alkaline and fine-grained byproduct of Bayer process for alumina’s production, is a material rich in numerous minerals and elements of high value and techno-economical interest in high tech applications such as rare earths, including scandium. Lately, the European Committee has characterized scandium as a critical element because of its risk supply chain. Scandium's high concentration in Greek bauxite residue classifies the waste as a candidate for low cost and high availability of the element, additionally improving its environmental fingerprint. For scandium recovery, hydrometallurgical treatment with inorganic acids is the most common, effective and simple method. In this study, the efficiency of phosphoric acid is investigated for scandium recovery by a direct leaching of bauxite residue without pretreatment. Multi leaching variables, such as acid molarity, solid/liquid ratio, process temperature and leaching time, were examined and optimized individually as well as in a comparative way aiming to scandium selective extraction (mainly with regard to iron) and process viability. A Sc selective recovery of 40% was obtained for phosphoric acid molarity 5 M, solid/liquid ratio 10%, leaching time, 60 min under ambient conditions with low iron leachability, no gel formation and no energy consumption.

This is a report from NoRCELs Blue Earth Project symposium BEP2022 held online on January 8th, 2022. We are reporting the outcome pertaining to the following question: Is Humanity Settling its own Fate on Ecological Survival? A succinct conclusion drawn is that the Earth is facing the sixth mass extinction of flora and fauna; this being different from the previous five extinctions, in that it is entirely due to mankinds activities. Five invited eminent speakers delivered their input, highlighting the fact that there is extensive deterioration of the environment at large, coupled with an unprecedented demise of ecosystems leading to the extinction of species across the globe.