Investigating water ice content at different locations on the Moon is crucial for crewed space missions and serves as a foundation for establishing lunar bases, which necessitates lunar soil sampling to gather information. Aiming to minimize the water ice loss caused by heat generation during drilling, this paper proposes a water ice highconservation sampling system based on frozen CO2 spray cooling. The thermodynamic and hydrodynamic models of the frozen CO2 generation subsystem and heat exchange subsystem are established. The impact of design parameters, flow and thermal conditions, and operation modes on water content has been analyzed. The spray cooling method indirectly affects the lunar soil temperature by reducing the drill bit temperature to increase the water conservation ratio (WCR) during drilling. The method combines frozen CO2 sublimation heat flow and jet cooling flow. Jet cooling is closely associated with the temperature difference between the fluid and the drill bit, as well as the flow velocity. Meanwhile, sublimation heat flow depends on the temperature difference between the drill bit and the saturation temperature of frozen CO2, along with the content of frozen CO2. Jet cooling is predominant at lower mass flow rates, while sublimation cooling prevails at higher rates. In addition, the time the lunar soil is at low-sublimation temperature is an important factor in WCR. Thus, to increase WCR, one can enhance flow velocity by reducing the nozzle diameter, raise sublimation heat flow by increasing mass flow and lowering the initial temperature, and maintain lunar soil at low-sublimation temperatures by increasing cooling time, duty ratio and decreasing the cooling period. Among others, increasing the cooling time has the most significant effect. The increasing slopes of WCR with cooling durations are about 20 %/100 s (at 0.4 g/s, liquid CO2) and 10 %/100 s (at 0.1 g/s, liquid CO2). However, the cooling time should not exceed the drilling time. This study provides an effective water ice conservation system that is useful for other planetary sampling missions.

H2O extraction from remote icy lunar regolith using concentrated irradiation was investigated under high-vacuum and low-temperature conditions. The thermal sublimation of H2O(s) from packed beds of lunar regolith simulants was quantified with and without an indirect solar receiver for average concentrated irradiations of 37.06 f 2.66 and 74.62 f 3.57 kW/m2. The indirect solar receiver increased sublimation by an average of 18.7 % f 10.4 %, despite slower heating rates due to its increased thermal mass. Different average concentrated irradiations affected the heating rates and thermal gradients within the packed bed, but the impact on overall sublimation was not statistically significant. An inverse relationship between heating rates and normalized sublimation was also observed, where rapid sublimation near the heating elements led to the formation of a desiccated layer of regolith, which behaved as a thermal insulator and further limited heat transfer, reducing the sublimation efficiency. These findings provide key insights for optimizing in-situ resource utilization technologies, contributing to the development of efficient methods for extracting H2O from lunar regolith, which is essential for sustainable space exploration.

Ice records provide a qualitative rather than a quantitative indication of the trend of climate change. Using the bulk aerodynamic method and degree day model, this study quantified ice mass loss attributable to sublimation/evaporation (S/E) and meltwater on the basis of integrated observations (1960-2006) of glacier-related and atmospheric variables in the northeastern Tibetan Plateau. During 1961-2005, the average annual mass loss in the ice core was 95.33 +/- 20.56 mm w.e. (minimum: 78.97 mm w.e. in 1967, maximum: 146.67 mm w.e. in 2001), while the average ratio of the revised annual ice accumulation was 21.2 +/- 7.7% (minimum: 11.0% in 1992, maximum 44.8% in 2000). A quantitative formula expressing the relationship between S/E and air temperature at the monthly scale was established, which could be extended to estimation of S/E changes of other glaciers in other regions. The elevation effect on alpine precipitation determined using revised ice accumulation and instrumental data was found remarkable. This work established a method for quantitative assessment of the temporal variation in ice core mass loss, and advanced the reconstruction of long-term precipitation at high elevations. Importantly, the formula established for reconstruction of S/E from temperature time series data could be used in other regions.

Water ice in the polar regions of the Moon is crucial for potential manned lunar bases and as a source of fuel for rockets. Confirmation of the presence requires in-situ sampling which may result in the water ice sublimation. Therefore, it is necessary to analyze the water loss during the drilling, brushing and transfer processes. This paper establishes the heat and mass dynamic model of the sampling system. It explores the effects of design and drilling parameters and the initial state of lunar soil and components on water ice loss. It indicates that the water loss decreases with the increasing heat transfer of the bit. Higher rotational speed and faster feed rate result in greater water loss. The effect of the feed speed is slight when the rotational speed is below 120 rpm. The increase in initial water content significantly increases the water loss percentage due to more difficult drilling. The initial temperature of the drilling tool has a significant influence on the initial stage of drilling. The water loss increases rapidly after the temperature exceeds 210 K. This paper points out the water loss under different parameters and provides a theoretical basis for the design of drilling tools and drilling parameters.

Physical or chemical phase changes in ablation, such as sublimation, melting or dissolution, are studied in physics for their many engineering applications. At solid/fluid interfaces, the interaction between a phase change and a flow can lead to pattern formation. In this case, the fluid mechanics associated with such phase changes play a key role in the evolution of terrestrial and planetary landscapes, observed by probes orbiting planets and moons. On Earth, sea ice, glaciers and karst plateaus extend over meters or kilometers. The scale of these landscapes contrasts with the scale of the physical mechanisms that govern their evolutionary dynamics. Indeed, it is the typical size of atmospheric boundary layers or meltwater/vapor/solute films that constrain the heat/concentration transfer at the phase change/dissolution interface, and hence the rate of solid ablation. In many situations, these layers are controlled by fluid flow, either natural or forced convection. In the former case, the flow may be buoyancy driven by the melting/dissolution/sublimation itself, resulting in density stratification caused by, for example, temperature/concentration gradients. This stratification may be stable or unstable. In the second case, the flow forced by winds or slopes can be considered as a flow of an infinite height or of a finite height, such as shallow water flow. In all cases, the mass flux modifies topography, which in turn affects the boundary layer flows and thus the ablation rate in a retroactive way. In nature, the positive feedback between geometry and mass transfer drives the spontaneous formation of characteristic patterns at different scales. These patterns are not just geological curiosities, such as Zen stones or dirt cones but markers of the hydrodynamic processes at work. Many landscapes are shaped by regular, repeated patterns, whether sharp-edged, scalloped, parallel-crested, or stepped. By experimentally investigating different modes of flow transport on solid substrates undergoing physical or chemical phase change, this review aims to highlight the role of the flow transport mode in the diversity of patterns observed on analogous materials. Understanding the diversity of these patterns is key to assessing the environmental conditions under which they form on planets such as Mars or Pluto, where phase changes play a very important geomorphological role.

In order to study the processes related to the origin and retention of water on the surface of the Moon, an experimental setup has been created at the Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences (GEOKHI RAS), for the analysis of (re)sublimation processes of water ice in a vacuum at low temperatures. The temperature range for (re)sublimation varies from -100 to 0 degrees C. The setup is connected to an Isotope Ratio Mass Spectrometer (IRMS), which allows for measuring the isotopic composition of the vapor of the evaporating substance and providing an estimation of the (re)sublimation rate under specific physicochemical conditions. The direct introduction of gases into the mass spectrometer in real-time mode sets the developed setup apart from foreign counterparts. The setup is equipped with a transparent quartz window through which the surface of the studied substance can be heated using a halogen lamp, simulating the movement of solar rays on the surface of mineral grain compositions under conditions similar to those on the lunar surface. In addition to studying gas (de)sorption on the surfaces of mineral grains of various compositions, the setup can also be used for researching the (re)sublimation of gas hydrates and CO2.

The surface morphology of airless, ice-covered moons of the outer solar system, such as Europa, Enceladus, and Callisto, is not well known at centimeter- to meter-scales. Ice and snow erode differently on such worlds in part because sublimation is the dominant process. On Earth, ice penitentes have been observed in sublimation-driven environments, and may provide a guide for similar formations on ice-covered worlds. Penitentes are blade-like snow features observed on Earth in high-altitude, low-latitude snowfields. Models of penitente formation on Earth break down within the free-molecular regime of airless bodies, leaving a major gap in understanding whether such morphologies can form on their surfaces. To investigate the morphologic evolution of icy bodies, we developed a Sublimation Monte Carlo (SMC) model that enables a numerical approach to modeling exosphere-surface interactions at free-molecular conditions. The SMC model uses Monte Carlo tracking of molecules emitted from the surface to determine the net molecular interchange that drives surface changes. We validated results against experiments, matching the evolution of pre-formed penitentes as they receded in height and became less pronounced. Our results reveal the importance of molecular redeposition on topology, indicating that the stable morphology of isothermal topographies is a planar morphology on regions of net sublimation, regardless of initial surface shape. A study of parametrically varying temperature profiles for sinusoidal penitentes resulted in the following requirement for penitente growth: the trough temperature must exceed the peak temperature by a threshold value, which notably depends on the surface aspect ratio and peak temperature.

In recent years, the Moon, as the closest celestial body to the Earth, has become the foremost target of human exploration outward. Some lunar exploration missions and studies have shown that ice may exist in the polar regions of the Moon. Water is very important for human survival. The ice mining and utilization is based on the understanding of the sublimation mechanism. Simulation of ground-based tests is an effective means to explore the sublimation of ice. Therefore, in this paper, the thermal environment of Shackleton Crater and the particle size distribution of typical lunar soils are analyzed as the basis of parameter settings for the ground test. Four operating conditions are established for ground tests, including the influence of heat sink temperature, vacuum level, particle size distribution and dry soil density. The larger the radiation heat flow, the higher the heat sink temperature, the smaller the vacuum degree, the larger the average particle size, resulting in a larger sublimation rate. The decrease of density makes the sublimation process faster and then slower. The sublimation process proceeds fastest when the dry soil density is 1200 kg/m3. The heat sink temperature has the greatest effect on the sublimation process, and the vacuum has the least effect. When the radiation heat flow ranges from 39.01 W/m2 to 45.63 W/m2 at the heat sink temperature of 120 K, the maximum sublimation rate is 5.79E-15 kg/s, the maximum sublimation area is 1.93E-9 m2 and the maximum sublimation heat flow is 1.59E-8 W. However, the effect of vacuum degree and particle size distribution on the sample temperature variation is not significant, due to the small order of magnitude of the sublimation heat flow compared to the radiation and conduction heat flows. This paper gives a range of parameters for ground-based simulation experiments and points out the microscopic changes of the ice sublimation process, which provides ideas for the next ground-based experiments and the exploitation of water-ice resources on the Moon.

When considering the extraction of metals from lunar regolith for use in space, one reductive method of interest is vacuum thermal dissociation. Given the high vacuum environment on the Moon, the sub-liquidus operation of such a process, i.e., sublimation, warrants investigation. In the current work, the kinetics of the vacuum sublimation of the more volatile major oxides found in the lunar regolith, Na2O, K2O, and FeO, are evaluated. Two distinct factors are accounted for in the current work: the change in the evaporation flux due to temperature; and the reduction in available surface area for evaporation due to sintering of the feedstock. Surface area change due to the sintering of compressed LMS-1 regolith simulant pellets was quantified via a Brunauer-Emmett-Teller analysis. The surface area of the samples was measured to vary from 3.29 m(2)/g in the unsintered sample, to 1.04 m(2)/g in the samples sintered at 800 degrees C, and down to 0.09 m(2)/g in the sample sintered at 1150 degrees C. Evaporation flux was calculated using the Hertz-Knudsen-Langmuir equation using saturated vapor pressures predicted from the FactSage thermochemical package and verified against Knudsen Effusion Mass Spectroscopy data from tests conducted on lunar regolith sample #12022. The combination of these studies resulted in the conclusion that no local maxima in evaporation rate below the melting point was found for the current system, as such the highest rate of sublimation was determined to be 1200 degrees C for all species, at temperatures of 1200 degrees C and above, partial melting of the material occurs. The predicted maximum rate of sublimation for the species Fe, Na, and K at 1200 degrees C was 0.08, 1.38, and 1.02 g/h/g of regolith, respectively. It is noted that significant variation was seen between FactSage predictions of saturated vapor pressures and the measured values. Future work generating detailed thermochemical databases to predict the behavior of complex systems similar in composition to lunar regolith would benefit the accuracy of similar kinetic studies in the future.

Tall, spiky snow structures (penitentes) occur high in subtropical mountains, in the form of blades oriented east-west and tilted toward the noontime sun. By trapping sunlight, they cause a reduction of albedo by similar to 0.3 relative to flat snow. The formation of penitentes, explained by Lliboutry in 1954, requires weather conditions allowing the troughs to deepen rapidly by melting while the peaks remain dry and cold by sublimation, losing little mass, because of the 8.5-fold difference in latent heats. Lliboutry's explanation has been misrepresented in some recent publications. A concern has been raised that in the low latitudes of Jupiter's moon Europa, the ice surface may have developed penitentes, which would pose a hazard to a lander. They would require a different mechanism of formation, because Europa is too cold for melting to occur. If penitentes are present on Europa, they cannot be resolved by the coarse-resolution satellite images available now, but the high albedo of Europa (similar to 0.7 at visible wavelengths) argues against the existence of such extreme roughness.