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The article provides several announcements related to the fields of photogrammetry, remote sensing, and GIS. The first announcement discusses RIEGL USA's collaboration with Allen & Company in the NASA Lunabotics Qualification Challenge, where they used the RIEGL VZ-600i terrestrial laser scanner to measure the success of student robotics in transporting simulated lunar regolith. The second announcement highlights Esri's launch of the Central Asia and Caucasus Geoportal, which provides free access to data, GIS tools, and training resources for individuals in the region. Lastly, the article mentions that Woolpert has been contracted by Miami-Dade County to provide GIS and consulting services for their Next Generation 9-1-1 emergency management routing system. [Extracted from the article]

In-situ resource utilization has become a significant issue in recent space projects. For example, various studies have focused on lunar manufacturing using regoliths available on the moon's surface. Although regolith manufacturing will be conducted under lunar gravity, most studies have not considered the adverse effects of low gravity on additive manufacturing processes. This study evaluates the gravitational effect on lunar regolith powder bed fusion (PBF) by applying centrifugal acceleration to the PBF process. The experimental results show that gravitational acceleration influences the density, hardness, and transparency of the fabricated regolith blocks. [ABSTRACT FROM AUTHOR]

The article focuses on the development and application of a novel membrane-based electrolytic process for metal production. It is reported that this process utilizes oxygen-ion-conducting solid oxide membranes (SOM) to enable direct electrolysis of metal oxides dissolved in molten salts, offering advantages such as reduced energy consumption, lower emissions, and higher purity of metals and oxygen produced.

The interactions between nano-silica lunar dust (NSLD) on the moon surface and pulmonary surfactant (PS) monolayer will pose risks to astronaut health in future manned lunar exploration missions, but the specifics of these interactions are unknown. This study investigates them using the coarse-grained molecular dynamics method considering different sizes (5, 10, and 15 nm) and shapes (sphere, ellipsoid, and cube), with special focus on the unique morphology of NSLDs with bugles. The key findings are as follows: (1) The 10 nm and 15 nm NSLDs embed in the PS monolayer through the major sphere of spherical-type, major ellipsoid of ellipsoidal-type, or one edge of cubic-type NSLDs upon contact the PS monolayer. (2) Adsorbed NSLDs cause a higher S z value (AS z > 0.84), while embedded NSLDs cause a lower S z value (0.47 < AS z < 0.83) that decreases with an increase in the number of bulges. (3) The embedding process absorbs 50–342 dipalmitoylphosphatidylcholine (DPPC) molecules, reducing the PS monolayer area by 0.21%–6.05%. NSLDs with bulges absorb approximately 9–126 additional DPPC molecules and cause a 0.05%–3.22% reduction in the PS monolayer area compared to NSLDs without bulges. (4) NSLDs move obliquely or vertically within the PS monolayer, displaying two distinct stages with varying velocities. Their movement direction and speed are influenced by the increasing complexity of NSLD with more bulges on them. In general, larger NSLDs with sharper shapes and increasing complex morphology of more bulges cause more significant damages to the PS monolayer. These findings have implications for safeguarding astronaut health in future manned lunar exploration missions. [Display omitted] • The start of embedding is up to the contact way of large NSLDs with PS monolayer. • AS z is larger than 0.84 for absorbed NSLDs and 0.47–0.83 for embedded NSLDs. • The embedding NLSDs absorb 50–342 molecules, reducing the PS area by 0.21–6.05%. • NSLDs move obliquely or vertically in PS monolayer with two kinds of velocities. • Bulges on NSLDs cause more damages to PS monolayer and affect their moving ways. [ABSTRACT FROM AUTHOR]

Imminent robotic and human activities on the Moon and other planetary bodies would benefit from advanced in situ Computer Vision and Machine Learning capabilities to identify and quantify microparticle terrestrial contaminants, lunar regolith disturbances, the flux of interplanetary dust particles, possible interstellar dust, β -meteoroids, and secondary impact ejecta. The YOLO-ET (ExtraTerrestrial) algorithm, an innovation in this field, fine-tunes Tiny-YOLO to specifically address these challenges. Designed for coreML model transference to mobile devices, the algorithm facilitates edge computing in space environment conditions. YOLO-ET is deployable as an app on an iPhone with LabCam® optical enhancement, ready for space application ruggedisation. Training on images from the Tanpopo aerogel panels returned from Japan's Kibo module of the International Space Station, YOLO-ET demonstrates a 90% detection rate for surface contaminant microparticles on the aerogels, and shows promising early results for detection of both microparticle contaminants on the Moon and for evaluating asteroid return samples. YOLO-ET's application to identifying spacecraft-derived microparticles in lunar regolith simulant samples and SEM images of asteroid Ryugu samples returned by Hayabusa2 and curated by JAXA's Institute of Space and Astronautical Sciences indicate strong model performance and transfer learning capabilities for future extraterrestrial applications. [ABSTRACT FROM AUTHOR]

In space, every carbon atom matters. It is a potential source for a wealth of products essential for human space exploration and habitation. Here, we report the use of Martian and Lunar regolith simulants as catalysts for the thermochemical catalytic conversion of CO 2. Results of this study clearly underlines activity towards CO production through the RWGS reaction at high temperature for all Martian and Lunar regolith simulants. Characterization of the samples reveals improved catalytic activities directly correlated with the presence and further transformation of iron and magnesium-based compounds and their subsequent migration at the surface. These findings point towards the feasibility of producing propellants in other celestial bodies using local resources. [Display omitted] • Propellant production using Martian and Lunar regolith simulants. • Martian and Lunar regolith simulants promote the RWGS reaction. • Martian simulants exhibited higher catalytic activity compared to Lunar simulants. • Iron carbide and MgO surface hydroxyl groups found as active sites. [ABSTRACT FROM AUTHOR]

Methods of deriving FeO and TiO2 contents from Clementine spacecraft data are discussed, and our own approach is developed for deriving the contents from measurements made by the M³ instrument on Chandrayaan-1. The density of lunar soil bedrock is modeled based on the derived FeO and TiO2 information. The FeO and TiO2 abundance we derived from the M³ data is compared with previous results from the Clementine data and is in good agreement. The FeO abundance data also agree well with the Lunar Prospector data, which were used as an independent source. The previous Clementine and new M3-derived abundances are compared with the laboratory-measured FeO and TiO2 contents in the Apollo and Luna returned samples. The Clementine-derived FeO content was systematically 1--2% lower in all the returned samples than the laboratory measurements. The M3-derived content agrees better with the returned Apollo samples and is within ±2.8% of the laboratory-measured ones. The Clementine-derived TiO2 abundance is systematically 0.1--4% higher than the laboratory measurements of the returned samples. The M3-derived TiO2 content agrees well (±0.6%) with the laboratory measurements of the returned samples, except for the samples with a high TiO2 content. However, caution should be taken when interpreting these results, as the error range needs further study. Unfortunately, no error analysis was provided with the previous Clementine-derived contents. [ABSTRACT FROM AUTHOR]

Since about half a century samples from the lunar and asteroidal regoliths been used to derive information about elemental and isotopic composition and other properties of the present and past solar wind, predominantly for the noble gases and nitrogen. Secular changes of several important compositional parameters in the solar wind were proposed, as was a likely secular decrease of the solar wind flux. In 2004 NASA’s Genesis mission returned samples which had been exposed to the solar wind for almost 2.5 years. Their analyses resulted in an unprecendented accuracy for the isotopic and elemental composition of several elements in the solar wind, including noble gases, O and N. The Genesis data therefore also allow to re-evaluate the lunar and meteorite data, which is done here. In particular, claims for long-term changes of solar wind composition are reviewed. Outermost grain layers from relatively recently irradiated lunar regolith samples conserve the true isotopic ratios of implanted solar wind species. This conclusion had been made before Genesis based on the agreement of He and Ne isotopic data measured in the aluminum foils exposed to the solar wind on the Moon during the Apollo missions with data obtained in the first gas release fractions of stepwise in-vacuo etch experiments. Genesis data allowed to strengthen this conclusion and to extend it to all five noble gases. Minor variations in the isotopic compositions of implanted solar noble gases between relatively recently irradiated samples (<100 Ma) and samples irradiated billions of years ago are very likely the result of isotopic fractionation processes that happened after trapping of the gases rather than indicative of true secular changes in the solar wind composition. This is particularly important for the 3 He/ 4 He ratio, whose constancy over billions of years indicates that hardly any 3 He produced as transient product of the pp-chains has been mixed from the solar interior into its outer convective zone. The He isotopic composition measured in the present-day solar wind therefore is identical to the (D + 3 He)/ 4 He ratio at the start of the suns’s main sequence phase and hence can be used to determine the protosolar D/H ratio. Genesis settled the long-standing controversy on the isotopic composition of nitrogen in lunar regolith samples. The 15 N/ 14 N ratio in the solar wind as measured by Genesis is lower than in any lunar sample. This proves that nitrogen in regolith samples is dominated by non-solar sources. A postulated secular increase of 15 N/ 14 N by some 30% over the past few Ga is not tenable any longer. Genesis also provided accurate data on the isotopic composition of oxygen in the solar wind, invaluable for cosmochemisty. These data superseded but essentially confirmed one value – and disproved a second one – derived from lunar regolith samples shortly prior to Genesis. Genesis also confirmed prior conclusions that lunar regolith samples essentially conserve the true elemental ratios of the heavy noble gases in the solar wind (Ar/Kr, Kr/Xe). Several secular changes of elemental abundances of noble gases in the solar wind had been proposed based on lunar and meteoritic data. I argue here that lunar data – in concert with Genesis – provide convincing evidence only for a long-term decrease of the Kr/Xe ratio by almost a factor of two over the past several Ga. It appears that the enhancement of abundances of elements with a low first ionisation potential in the solar wind (FIP effect) changed with time. Finally, Genesis allows a somewhat improved comparison of the present-day flux of solar wind Kr and Xe with the total amount of heavy solar wind noble gases in the lunar regolith. It remains unclear whether the past solar wind flux has been several times higher on average than it is today. [ABSTRACT FROM AUTHOR]

The Moon is generally depleted in volatile elements and this depletion extends to the surface where the most abundant mineral, anorthite, features <6 ppm H 2 O. Presumably the other nominally anhydrous minerals that dominate the mineral composition of the global surface—olivine and pyroxene—are similarly depleted in water and other volatiles. Thus the Moon is tabula rasa for the study of volatiles introduced in the wake of its origin. Since the formation of the last major basin (Orientale), volatiles from the solar wind, from impactors of all sizes, and from volatiles expelled from the interior during volcanic eruptions have all interacted with the lunar surface, leaving a volatile record that can be used to understand the processes that enable processing, transport, sequestration, and loss of volatiles from the lunar system. Recent discoveries have shown the lunar system to be complex, featuring emerging recognition of chemistry unanticipated from the Apollo era, confounding issues regarding transport of volatiles to the lunar poles, the role of the lunar regolith as a sink for volatiles, and the potential for active volatile dynamics in the polar cold traps. While much has been learned since the overturn of the "Moon is dry" paradigm by innovative sample and spacecraft measurements, the data point to a more complex lunar volatile environment than is currently perceived. [ABSTRACT FROM AUTHOR]

Abstract: Based on the analysis results of components and the particle diameter distribution of lunar soil, some basalt particles with different diameters are mixed into homogeneous soil to simulate the drilling process and particles conveying condition. Lunar soil containing basalt particles with different diameters can affect drilling process, penetration rate and conveying power consumption. The experiment results revealed that basalt particles move upward in an irregular spiral state during drilling; the basalt particles can convey smoothly and has little effect on drilling process, penetration rate and power consumption when the particle diameter is less than 5 mm. The basalt particles can’t convey smoothly and has great effect on penetration rate and power consumption while particle diameter is bigger than 10 mm. Particles in lunar soil will lead to torque increasing sharply and drilling pressure on bit adding to achieve continuous drilling. [Copyright &y& Elsevier]

In order to understand the influence of lunar soil's properties on wheel-soil interaction mechanics, physical and mechanical properties of lunar soil were analyzed; lunar soil simulant was made and experiments were performed to measure soil parameters and wheel-soil interaction mechanics. The parameters of lunar soil simulant are estimated or identified according to the experimental data. Theoretical and numerical analysis have been done by substituting typical lunar soil parameters into the model, and the results are compared with the experimental data which shows that the soil parameters of bearing property primarily influence the wheel sinkage, the resistance moment of wheel is mainly influenced by shearing property of soil, and the contact angle coefficients that can reflect the physical property of soil has relatively small influence on wheel-soil interaction. [ABSTRACT FROM AUTHOR]

Ureilite meteorites contain iron silicide minerals including suessite (Fe,Ni) 3 Si, hapkeite (Fe 2 Si) and xifengite (Fe 5 Si 3). Despite occurring mostly in brecciated varieties presumed to be derived from the regolith of the ureilite parent asteroid, suessite has also been confirmed in one lithology of a dimict ureilite (NWA 1241). In contrast, Si-bearing Fe-metals occur in both brecciated and unbrecciated ureilites, implying that they were formed throughout the ureilite parent asteroid. We examined major, minor and trace element data of Fe-metals in seven brecciated ureilites (DaG 319, DaG 999, DaG 1000, DaG 1023, DaG 1047, EET 83309, and EET 87720) in addition to the dimict ureilite NWA 1241. In this study we show that the silicides and Si-bearing metals in ureilites have similar siderophile trace element patterns; therefore, the precursors to the silicides were indigenous to the ureilite parent body. Si-free kamacite grains in brecciated ureilites show flatter, more chondritic siderophile element patterns. They may also be derived from the interior of the ureilite parent body, but some may be of exogenous origin (impactor debris), as are rare taenite grains. On Earth, iron silicides are often formed under high-temperature and strongly reducing conditions (e.g. blast furnaces, lightning strikes). On the Moon, hapkeite (Fe 2 Si) and other silicides have been found in the regolith where they were formed by impact-induced space weathering. In the Stardust aerogel, iron silicides derived from comet Wild2 were also formed by an impact-related reduction process. Silicides in ureilite regolith breccias may have formed by similar processes but ureilites additionally contain abundant elemental carbon which probably acted as a reducing agent, thus larger and more abundant silicide grains were formed than in the lunar regolith or cometary material. The origin of suessite in NWA 1241 may be analogous to that of reduced lithologies in the terrestrial mantle, although a regolith origin may also be possible since this sample is shown here to be a dimict breccia. [ABSTRACT FROM AUTHOR]