Liquid Water Interface Research Articles

The molecular structure of the interface between water and a hydrophobic substrate is liquid-vapor like.

With molecular simulation for water and a tunable hydrophobic substrate, we apply the instantaneous interface construction [A. P. Willard and D. Chandler, "Instantaneous liquid interfaces," J. Phys. Chem. B 114, 1954-1958 (2010)] to examine the similarity between a water-vapor interface and a water-hydrophobic surface interface. We show that attractive interactions between a hydrophobic surface and water affect capillary wave fluctuations of the instantaneous liquid interface, but these attractive interactions have essentially no effect on the intrinsic interface. The intrinsic interface refers to molecular structure in terms of distances from the instantaneous interface. Further, the intrinsic interface of liquid water and a hydrophobic substrate differs little from that of water and its vapor. The same is not true, we show, for an interface between water and a hydrophilic substrate. In that case, strong directional substrate-water interactions disrupt the liquid-vapor-like interfacial hydrogen bonding network.

Impact of Interfacial Water Transport in PEMFCs on Cell Performance

Coupled cell performance evaluation, liquid water visualization by neutron radiography (NRG) and numerical modeling based on multiphase mixture (M2) model were performed with three types of GDMs: Micro Porous Layer (MPL) free; Carbon Paper (CP) with MPL; and CP free to investigate interfacial liquid water transport phenomena in PEMFCs and its effect on cell performance.The visualized results of MPL free GDM with different wettability of bi-polar plates (BPPs) showed hydrophilic BPP improved liquid water transport at the interface between CP and channel. Numerical modeling results indicated that this difference with BPP wettability was caused by the liquid water coverage difference on CP surface. Thus, controlling liquid water coverage is the one of the key strategies for improving cell performance. Additionally, liquid water distributions across the cell for three types of GDMs were compared and significant difference in liquid water content at the interface between Catalyst Layer (CL) and GDM was observed. Numerical modeling suggests this difference is influenced by the gap at the interface and that the MPL could minimize this effect. The CP free cell (i.e. only MPL) showed the best performance and the lowest liquid water content. There were multiple impacts of interfacial liquid water transport both at CL-GDM and GDM-channel interfaces. High hydrophobicity and fine structure of MPLs contributed to enhanced liquid water transport at GDM-channel interface and as a result reduced the liquid water coverage. At the same time, MPL improves contact at the CL-GDM interface in the same manner as seen in CP with MPL case. Thus, the CP free concept showed the best performance. It is suggested that the design of the interface between each component of the PEMFC has a great impact on cell performance and plays a significant role in achievement of high current density operation and cost reduction in FCEVs.

Investigation of Interfacial Water Transport at the Gas Diffusion Media by Neutron Radiography

For cost reduction of fuel cell, it is necessary to realize high current density operation, which requires a thorough understanding of mass transport. However, especially interfacial liquid water transport between carbon paper (CP), micro porous layer (MPL), and catalyst layer (CL) are not fully understood. Coupled cell performance evaluation, liquid water visualization by neutron radiography and numerical modeling were performed with three types of gas diffusion media (GDM): MPL free; CP with MPL; and CP free. It revealed that the presence of a gap at the CL-GDM interface has a significant effect on water accumulation and that the MPL could minimize this effect. At the same time, CP free case showed the best performance and the lowest liquid water content due to multiple impacts of interfacial liquid water transport both at CL-MPL and MPL-channel interfaces. These results confirm the importance of interfacial design between each component of fuel cell for further cost reduction.

Possibility of H2O2 decomposition in thin liquid films on Mars

In this work the pathways and possibilities of H2O2 decomposition on Mars in microscopic liquid interfacial water were analyzed by kinetic calculations. Thermal and photochemical driven decomposition, just like processes catalyzed by various metal oxides, is too slow compared to the annual duration while such microscopic liquid layers exist on Mars today, to produce substantial decomposition. The most effective analyzed process is catalyzed by Fe ions, which could decompose H2O2 under pH<4.5 with a half life of 1–2 days. This process might be important during volcanically influenced periods when sulfur release produces acidic pH, and rotational axis tilt change driven climatic changes also influence the volatile circulation and spatial occurrence just like the duration of thin liquid layer.Under current conditions, using the value of 200K as the temperature in interfacial water (at the southern hemisphere), and applying Phoenix lander׳s wet chemistry laboratory results, the pH is not favorable for Fe mobility and this kind of decomposition. Despite current conditions (especially pH) being unfavorable for H2O2 decomposition, microscopic scale interfacial liquid water still might support the process. By the reaction called heterogeneous catalysis, without acidic pH and mobile Fe, but with minerals surfaces containing Fe decomposition of H2O2 with half life of 20 days can happen. This duration is still longer but not several orders than the existence of springtime interfacial liquid water on Mars today. This estimation is relevant for activation energy controlled reaction rates. The other main parameter that may influence the reaction rate is the diffusion speed. Although the available tests and theoretical calculations do not provide firm values for the diffusion speed in such a “2-dimensional” environment, using relevant estimations this parameter in the interfacial liquid layer is smaller than in bulk water. But the 20 days׳ duration mentioned above is still relevant, as the activation energy driven reaction rate is the main limiting factor in the decomposition and not the diffusion speed.The duration of dozen(s) days is still longer but not with orders of magnitude than the expected duration for the existence of springtime interfacial liquid water on Mars today. The results suggest such decomposition may happen today, however, because of our limited knowledge on chemical processes in thin interfacial liquid layers, this possibility waits for confirmation – and also points to the importance of conducting laboratory tests to validate the possible process. Although some tests were already realized for diffusion in an almost 2-dimensional liquid, the same is not true for activation energy, where only the value from the “normal” measurements was applied.Even if H2O2 decomposition is too slow today, the analysis of such a process is important, as under volcanic influence more effective decomposition might take place in thin interfacial liquids close to the climate of today if released sulfur produces pH<4.5. Large quantity and widespread occurrence of bulk liquid phase are not expected in the Amazonian period, but interfacial liquid water probably appeared regularly, and its locations, especially during volcanically active periods, might make certain sites than others more interesting for astrobiology with the lower concentration of oxidizing H2O2.

The amorphous silica–liquid water interface studied by ab initio molecular dynamics (AIMD): local organization in global disorder

The structural organization of water at a model of amorphous silica–liquid water interface is investigated by ab initio molecular dynamics (AIMD) simulations at room temperature. The amorphous surface is constructed with isolated, H-bonded vicinal and geminal silanols. In the absence of water, the silanols have orientations that depend on the local surface topology (i.e. presence of concave and convex zones). However, in the presence of liquid water, only the strong inter-silanol H-bonds are maintained, whereas the weaker ones are replaced by H-bonds formed with interfacial water molecules. All silanols are found to act as H-bond donors to water. The vicinal silanols are simultaneously found to be H-bond acceptors from water. The geminal pairs are also characterized by the formation of water H-bonded rings, which could provide special pathways for proton transfer(s) at the interface. The first water layer above the surface is overall rather disordered, with three main domains of orientations of the water molecules. We discuss the similarities and differences in the structural organization of the interfacial water layer at the surface of the amorphous silica and at the surface of the crystalline (0 0 0 1) quartz surface.

Searching for springtime zonal liquid interfacial water on Mars

We analyzed the spatial and temporal characteristics of the surface temperature at the northern water ice annulus on Mars that is left behind the receding seasonal carbon dioxide cap in springtime. Using OMEGA hyperspectral images we show that water ice without carbon dioxide ice coverage lasts for 10–30days between 55° and 70°N. The longest water ice coverage without CO2 ice is observed between 40–55°N and 300–330°E and lasts 80–110days in ideal case. Using TES temperature data, we show that thin interfacial liquid water may be present at the water ice annulus. Higher spatial resolution THEMIS temperature data shows that the above mentioned finding is relevant to a spatial scale of 100m. Although the exact near surface water vapor concentration is not known, beside the average 10pr-μm we used two elevated values and corresponding threshold temperatures for interfacial liquid water formation: 190 and 199K beside the average 180K. While the area of interfacial liquid water is substantially smaller in the case of higher threshold temperature values, even for 199K terrains exist at THEMIS and OMEGA scale of resolution where such thin interfacial liquid water could be present on the surface. Summarizing: good chance exists for the presence of liquid interfacial water in the warmest part of the day on at the northern hemisphere of Mars at extended areas – although firm evidence requires better targeted future observations.

Coupling of a continuum fuel cell model with a discrete liquid water percolation model

An iterative algorithm is developed to directly integrate a discrete liquid water percolation model into a 3D continuum fuel cell model. In the continuum model the thermodynamic processes, most relevant for the water management and fuel cell performance, are calculated. For the discrete liquid water distribution in the porous transport layer (PTL), a water path network model is used, calculating the discrete, injection pressure and condensation scenario dependent saturation distribution.The saturation in the PTL is compared to synchrotron visualization data and a good comparison is found. Using the model, the influence of PTFE content, the application of a microporous layer, PTL perforation and ionomer desorption rate on the water configuration and fuel cell performance are analyzed. The interfacial liquid water is identified as an important parameter for the liquid water transport and the oxygen diffusivity to the active areas.

Heat Transfer Calculations for Decomposition of Structure I Methane Hydrates by Molecular Dynamics Simulation

Microcanonical ensemble molecular dynamics simulations of structure I methane hydrate is presented in this work to study the endothermic decomposition process. The mechanism of decomposition of methane hydrate as a function of time was explained at the molecular level. The initial temperature and pressure of the simulation were chosen so as to depict the natural gas hydrate in conditions of oceanic sediments. A more realistic strategy was developed to perform the microcanonical ensemble simulation of solid–liquid interface of hydrate and amorphous water. Two water models, SPC/E and TIP4P, were used for the simulations, and the results of the simulations were compared. Heat transfer calculations were performed on the adiabatic system, and an attempt has been made to fit the MD simulation results to the heat balance equations derived from the heat transfer calculations. Estimates of the properties at the macroscopic scale, like the equilibrium temperature of methane hydrate and rate of supply of hot water f...

Redox-active Microcapsules of Cytochrome c Formed at the Ionic Liquid–Water Interface

Abstract Microcapsules of cytochrome c (Cyt c) are spontaneously formed by introducing aqueous Cyt c microdroplets in ionic liquids (ILs), which are facilely transferred to aqueous phase after crosslinking and hydrophilic augmentation of the capsule surface.

Morphology of Carbon Dioxide–Hydrogen–Cyclopentane Hydrates with or without Sodium Dodecyl Sulfate

In this study, effects of cyclopentane (CP) and sodium dodecyl sulfate (SDS) on the hydrate formation morphology were investigated. A gas mixture of 40.0 mol % carbon dioxide and 60.0 mol % hydrogen was used in an unstirred system with subcooling as the driving force. Experimental pressure is at 6.0 MPa and experimental temperatures used are at 275.65 and 277.65 K (ΔT = 15.15 and 13.15 K). Formation of hydrates started at the cyclopentane–liquid water interface. Cloud-like, equiaxed skewed dendritic, equiaxed orthogonal dendritic, long dendritic, and cactus-like crystals could be observed for the experiments in the absence of surfactants. Rapid hydrate formation was observed for the experiments with 0.9 mL CP with or without the presence of surfactants compared to the experiments with 0.45 mL CP system at the same experimental conditions. The addition of SDS had led to a change in the hydrate crystal morphology, forming fiber-like crystals from the hydrate layer. Hydrates had also shown affinity to metal ...

Water and Brines on Mars: Current Evidence and Implications for MSL

Liquid water is a basic ingredient for life as we know it. Therefore, in order to understand the habitability of other planets we must first understand the behavior of water on them. Mars is the most Earth-like planet in the solar system and it has large reservoirs of H2O. Here, we review the current evidence for pure liquid water and brines on Mars, and discuss their implications for future and current missions such as the Mars Science Laboratory.Neither liquid water nor liquid brines are currently stable on the surface of Mars, but they could be present temporarily in a few areas of the planet. Pure liquid water is unlikely to be present, even temporarily, on the surface of Mars because evaporation into the extremely dry atmosphere would inhibit the formation of the liquid phase, where the temperature and pressure are high enough so that water would neither freeze nor boil. The exception to this is that monolayers of liquid water, referred to as undercooled liquid interfacial water, could exist on most of the Martian surface. In a few places liquid brines could exist temporarily on the surface because they could form at cryogenic temperatures, near ice or frost deposits where sublimation could be inhibited by the presence of nearly saturated air.Both liquid water and liquid brines might exist in the shallow subsurface because even a thin layer of soil forms an effective barrier against sublimation allowing pure liquid water to form sporadically in a few places, or liquid brines to form over longer periods of time in large portions of the planet. At greater depths, ice deposits could melt where the soil conductivity is low enough to blanket the deeper subsurface effectively. This could cause the formation of aquifers if the deeper soil is sufficiently permeable and an impermeable layer exists below the source of water.The fact that liquid brines and groundwater are likely to exist on Mars has important implications for geochemistry, glaciology, mineralogy, weathering and the habitability of Mars.

Biopolymer-Encapsulated Protein Microcapsules Spontaneously Formed at the Ionic Liquid–Water Interface

Aqueous microdroplets introduced in ionic liquids (ILs) provide unique interfaces where surface-modified protein microcapsules are spontaneously formed at systemic temperature. The susceptibility of proteins to form microcapsules at the water-IL microinterface depends on protein species and is related to the number of charged residues exhibited on protein surfaces. When both of the capsule-forming (host) proteins and guests biopolymers such as nucleic acids or enzymes are introduced in the aqueous microdroplets, microcapsules are formed selectively from host proteins while the guest biopolymers remain encapsulated in the aqueous pool. Microcapsules formed in the IL phase are facilely extracted to aqueous phase after consecutive cross-linking and surface modification reactions, and the whole processes can be done in one pot. Enzymes confined in the inner water phase of aqueous protein microcapsules showed innate activity, as visualized by site-specific fluorescence detection using confocal laser scanning microscopy (CLSM). The present IL-water interfacial synthesis of protein microcapsules eliminates the use of volatile organic solvents or solid colloid templates, which creates a much-coveted solution to existing technologies.

Locations of thin liquid water layers on present-day Mars

CRISM indicates the presence of water ice patches in Richardson crater, located on Mars’ southern polar region at the area of the seasonal ice cap. Numerical simulations suggest that the maximum daytime temperature of the ice at these locations is between 195 and 220K during local spring. Previous studies suggest that at these temperatures liquid interfacial water could be present. Here, for the first time, we provide an example where the environmental conditions allow for the formation of such liquid films on present day Mars at the southern hemisphere. The upper bound estimated H2O loss during the presence of these water ice patches is approximately 30μm between Ls=200 and 220, though it may be as low as 0.1μm depending on the ambient water vapor. The upper bound value is larger than the expected condensation thickness in autumn; however, it may still be realistic due to CO2 gas jet generated deposition and possible subsequent accumulation on mineral grains. The presence of this interfacial water may have impact on local chemical processes along with astrobiological importance.

Molecular dynamics simulation of replacement of methane hydrate with carbon dioxide

Molecular dynamics simulation was performed to analyse the phenomena of replacement of methane hydrate with carbon dioxide (CO2) at 270 K and 5.0 MPa for 5300 ps. The methane hydrate phase was constructed with 16 unit cells of hydrate. Every cage in the hydrate was occupied by one methane molecule. The methane hydrate phase was sandwiched between two CO2 phases. During the simulation the hydrate partially melted and liquid water phase appeared, and CO2 dissolved in the liquid water phase. The replacements were observed three times at the hydrate–liquid water interface during the simulation. In the first case, the replacement occurred at a S-cage without changing the structure. In the second case, an M-cage of methane hydrate partially collapsed, and methane and CO2 molecules exchanged. After the exchange, the cage occupied by CO2 remained in the M-cage structure. In the third case, a S-cage of methane hydrate partially collapsed, and methane and CO2 molecules exchanged. After the exchange, the cage occupied by CO2 changed to an M-cage-like structure.

Molecular Dynamics Investigation of the Various Atomic Force Contributions to the Interfacial Tension at the Supercritical CO2–Water Interface

Sequestration of carbon dioxide (CO(2)) in deep, geological formations involves the injection of supercritical CO(2) into depleted reservoirs containing fluids such as brine or oil. The interfacial tension (IFT) between supercritical CO(2) and the reservoir fluid is an important contribution to the sequestration efficiency. In turn, the IFT is a complex function of the reservoir fluid phase composition, the molecular structure of each reservoir fluid component, and environmental conditions (i.e., temperature and pressure). Molecular dynamics simulations can be used to probe the dependence of the IFT on these factors, since the IFT can be calculated directly from the simulated atomic forces and velocities at system equilibrium using the mechanical definition of the IFT. Here, we examine the contribution of each type of atomic force to the IFT, including bonded and nonbonded forces, as quantified by the anisotropy of the atomic virial tensor. In particular, we first examine a supercritical CO(2)-pure liquid water interface, at typical reservoir conditions (temperature of 343 K and pressure of 20 MPa), as a reference state against which CO(2)-brine systems can be compared. In this system, we note that the interactions between water molecules and between CO(2) molecules ("self" interactions) contribute positively to the IFT, while the interactions between water and CO(2) molecules ("cross" interactions) contribute negatively to the IFT. We find that the magnitude of the water "self" interactions is the dominant contribution. In terms of specific types of forces, we find that nonbonded electrostatic (QQ), bonded angle-bending, and bonded bond-stretching interactions contribute positively to the IFT, while nonbonded Lennard-Jones (LJ) interactions contribute negatively to the IFT. We also find that the balance between the LJ interactions and the bond-stretching interactions, in particular, plays a significant role in determining the magnitude of the IFT. Using orientational probability distribution functions to study molecular ordering about the interface, we find that the CO(2) molecules prefer to lie parallel to the interface at the Gibbs dividing surface (GDS) and that both the CO(2) and the water molecules are more ordered at the GDS than in the bulk. Finally, we present an initial study of a CO(2)-brine system with CaCl(2) as the model salt at a concentration of 2.7 M. We quantify the effect of the salt on the molecular orientation of water, and show that this effect leads to an increase in the IFT, relative to the CO(2)-water system, which is consistent with experimental measurements.

Molecular orientations at interfaces by extended polarizable continuum model

This study presents an investigation into orientation of molecular solutes at the interface of liquid water and other media. The calculation of electrostatic free energy of molecular solute is based on an extension of the polarizable continuum model (PCM) to interfacial system. The extended PCM computational scheme is incorporated with the self-consistent field procedure which is necessary to obtain more accurate electrostatic free energy and charge density distribution. The computation of non-electrostatic energy for interfacial system is also realized. Applying the numerical procedure to molecular systems, N,N′-diethyl-p-nitroaniline (DEPNA) at air/water interface and p-nitrophenol (PNP) at cyclohexane/water interface, the average orientational angles are in reasonable agreement with the experimental results. Taking both the electrostatic and the non-electrostatic energies into account, the analysis on the energy profiles shows that the electrostatic solvation energy is the dominant factor in determining the orientation angle for PNP, whereas for DEPNA, the orientation angle mainly depends on the cavitation energy. This suggests that, in addition to the electrostatic energy, taking the cavitation energy into account may provide a more complete view when we survey the molecular orientation at interface. © 2010 Wiley Periodicals, Inc. Int J Quantum Chem, 2011

Water ice in the dark dune spots of Richardson crater on Mars

Interfacial liquid water has been hypothesized to form during the seasonal evolution of the dark dune spots observed in the high latitudes of Mars. In this study we assess the presence, nature and properties of ices – in particular water ice – that occur within these spots using HIRISE and CRISM observations, as well as the LMD Global Climate Model. Our studies focus on Richardson crater (72°S, 179°E) and cover southern spring and summer ( L S =175–341°). Three units have been identified of these spots: dark core, gray ring and bright halo. Each unit show characteristic changes as the season progress. In winter, the whole area is covered by CO 2 ice with H 2O ice contamination. Dark spots form during late winter and early spring. During spring, the dark spots are located in a 10 cm thick depression compared to the surrounding bright ice-rich layer. They are spectrally characterized by weak CO 2 ice signatures that probably result from spatial mixing of CO 2 ice-rich and ice-free regions within pixels, and from mixing of surface signatures due to aerosols scattering. The bright halo shaped by winds shows stronger CO 2 absorptions than the average ice-covered terrain, which is consistent with a formation process involving CO 2 re-condensation. According to spectral, morphological and modeling considerations, the gray ring is composed of a thin layer of a few tens of μm of water ice. Two sources/processes could participate to the enrichment of water ice in the gray ring unit: (i) water ice condensation at the surface in early fall (prior to the condensation of a CO 2-rich winter layer) or during wintertime (due to cold trapping of the CO 2 layer) and (ii) ejection of dust grains surrounded by water ice by the geyser activity responsible for the dark spot. In any case, water ice remains longer in the gray ring unit after the complete sublimation of the CO 2. Finally, we also looked for liquid water in the near-IR CRISM spectra using linear unmixing modeling but found no conclusive evidence for it.

Photochemically induced formation of Mars relevant oxygenates and methane from carbon dioxide and water

The existence of methane in the Martian atmosphere is well established today. Several mechanisms have been discussed, which could be able to produce methane. However no mechanism is presently accepted to explain the observations satisfactorily. It is the aim of this paper to describe results of experimental laboratory investigations to study relationships and possible chemical reactions between Martian atmospheric carbon dioxide, liquid interfacial water (at least temporarily present), UV irradiation, and the possibly catalyzing influence of minerals like hematite with respect to the possible formation of oxygenate molecules. It is assumed that hematite can act as a photocatalyst under laboratory conditions (and also on the surface of Mars), and the formation of oxygenates evolves in course of the irradiation of carbon dioxide with UV-light in the presence of water, finally resulting in C–, O–, and H– containing molecules, which have been identified by GC–MS. The experiments were carried out under terrestrial atmospheric pressure and room temperature. Oxygenate molecules with one carbon atom like formaldehyde and methanol were found to be reaction products, but also C 2- and C 3-species like acetone. The important role of hematite as a photocatalytic active solid could be shown. The conversion of carbon dioxide increases in the presence of hematite. It has also a significant influence on the distribution of the products. Experiments with 18O-labeled water show a transfer of oxygen from water to carbon, which results in labeled oxygenate molecules. Oxygenates could have been formed from CO 2 via a photocatalytic reduction processes. The observed formation of C 2- and C 3-species might point to secondary competitive and consecutive reactions via complex and less selective mechanisms. All these results indicate the action of different reaction mechanisms, supporting therefore the assumption that both photocatalytic and radical reactions can contribute to the formation of oxygenates from carbon dioxide and water by UV irradiation. More importantly, the results give indication of a potential formation of hydrocarbons, such as methane, via conversion of atmospheric carbon dioxide and water on Martian soil mineral/water interfaces. Summarizing, it must be stated that, based on these first and promising results, a deeper and more quantitative understanding is necessary to model the contribution of photocatalytic processes to the apparent presence of oxygenates and hydrocarbons in the near surface atmosphere of Mars.

Interfacial liquid water on Mars and its potential role in formation of hill and dune gullies

Gullies are among the most intriguing structures identified on the surface of Mars. Most common are gullies located on the slopes of craters which are probably formed by liquid water transported by shallow aquifers (Heldmann, J.L., Carlsson, E., Johansson, H., Mellon, M.T., Toon, O.B. [2007]. Icarus 188, 324–344). Two particular types of gullies are found on slopes of isolated hills and dunes. The hill-slope gullies are located mostly at 50°S, which is at the high end of latitudes of bulk of the gullies found so far. The dune gullies are found in several locations up to 65°S (Reiss, D., Jaumann, R., Kereszturi, A., Sik, A., Neukum, G. [2007]. Lunar Planet. Sci. XXXVIII. Abstract 1993), but the best known are those in Russel crater at 54°S. The hill and dune gullies are longer than others making the aquifers explanation for their formation unlikely (Balme, M., Mangold, N., Baratoux, D., Costard, F., Gosselin, M., Masson, P., Pnet, P., Neukum, G. [2006]. J. Geophys. Res. 111. doi:10.1029/2005JE002607). Recently it has been noted that thin liquid films of interfacial water can play a role in rheological processes on the surface of Mars (Moehlmann, D. [2008]. Icarus 195, 131–139. Kereszturi, A., Moehlmann, D., Berczi, Sz., Ganti, T., Kuti, A., Sik, A., Horvath, A. [2009]. Icarus 201, 492–503.). Here we try to answer the question whether interfacial liquid water may occur on Mars in quantities large enough to play a role in formation of gullies. To verify this hypothesis we have calculated thermal models for hills and dunes of various steepness, orientation and physical properties. We find that within a range of average expected values of parameters it is not possible to have more than a few monolayers of liquid water at depths greater than a centimeter. To create subsurface interfacial water film significantly thicker and hence to produce conditions for the slope instability, parameters have to be chosen to have their extreme realistic values or an additional source of surface heating is needed. One possibility for additional heating is a change of atmospheric conditions due to a local dust storm. We conclude that if interfacial water is responsible for the formation of the hill-slope gullies, our results may explain why the hill gullies are rare.

A reagent-free SIA module for monitoring of sugar, color and dissolved CO 2 content in soft drinks

This work presents a new sequential injection analysis (SIA) method and a module for simultaneous and real-time monitoring of three key parameters for the beverage industry, i.e., the sugar content (measured in Brix), color and dissolved CO 2. Detection of the light reflection at the liquid interface (the schlieren effect) of sucrose and water was utilized for sucrose content measurement. A near infrared LED (890 ± 40 nm) was chosen as the light source to ensure that all the ingredients and dyes in soft drinks will not interfere by contributing light absorption. A linear calibration was obtained for sucrose over a wide concentration range (3.1–46.5 Brix). The same module can be used to monitor the color of the soft drink as well as the dissolved CO 2 during production. For measuring the color, the sample is segmented between air plugs to avoid dispersion. An RGB-LED was chosen as the light source in order to make this module applicable to a wide range of colored samples. The module also has a section where dissolved CO 2 is measured via vaporization of the gas from the liquid phase. Dissolved CO 2, in a flowing acceptor stream of water resulting in the change of the acceptor conductivity, is detected using an in-house capacitively coupled contactless conductivity detector (C 4D). The module includes a vaporization unit that is also used to degas the carbonated drink, prior the measurements of sucrose and color within the same system. The method requires no chemicals and is therefore completely friendly to the environment.