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Abstract: This paper provides new data on various pyrite and pyrrhotite generations at the Golets Vysochaishy gold deposit, Bodaibo district, Irkutsk Oblast. These generations are distinguished by morphological, geochemical, and isotope (δ34S) features. The established features of pyrite generations reflect the evolution of the Golets Vysochaishy deposit. Each pyrite generation is associated with a certain evolutionary stage of Neoproterozoic rocks in the region: (1) diagenesis (610 Ma), (2) catagenesis (570–520 Ma), (3) metamorphism (~450–430 Ma), and (4) tectono-magmatic activation (330–270 Ma). The 40Ar/39Ar ages of the third and fourth pyrite generations correspond to those of previously determined gold mineralization and granite magmatism.

Creating hardening coatings through thermo-reactive diffusion is an effective method for increasing the service life of cast iron parts. The influence of aluminium on the process of thermo-reactive diffusion of cast irons with vanadium has been studied. It has been found that the concentration of aluminium in the reaction powder medium affects the structure, thickness, and hardness of the coating. The most optimal concentration of aluminium is 0.5–2.5%. This concentration makes it possible to increase the thickness of the hardened coating by 1.5 times with a decrease in microhardness by 10–25% compared to pure vanadization.

Creating hardening coatings through thermo-reactive diffusion is an effective method for increasing the service life of cast iron parts. The influence of aluminium on the process of thermo-reactive diffusion of cast irons with vanadium has been studied. It has been found that the concentration of aluminium in the reaction powder medium affects the structure, thickness, and hardness of the coating. The most optimal concentration of aluminium is 0.5–2.5%. This concentration makes it possible to increase the thickness of the hardened coating by 1.5 times with a decrease in microhardness by 10–25% compared to pure vanadization.

The paper proposes a method for calculating the mode of single-pass arc welding depending on the geometric parameters of the T-fillet weld. The authors reveal the dependence of the residual welding stress level on the welding mode, taking into account the stress concentration due to uneven heating and transverse weld shrinkage. Resulting from the comparison of three modes of single-pass arc welding (manual, mechanized, and automatic), the optimal modes that ensure the maximum lifetime of welded structures are determined.

The paper discusses the change of phosphogypsum surface state produced by Apatit (Cherepovetsky branch, Vologda region) during calcination at 298-1173 K. The authors have determined the average size of its crystallites and studied the atomic composition of raw materials and finished composites that include crushed rock fraction (5-10 mm), oil bitumen, and polyethylene terephthalate additive (1.0-1.2 wt. %). The compounds present in calcined phosphogypsum have been analyzed by X-ray diffraction. The granulate was obtained by pelletizing phosphogypsum with a mixture of the above components. The paper presents the assessment of its physical and chemical properties. The granulated composites based on the specified samples of calcined phosphogypsum, bitumen, and melted polyethylene terephthalate waste show great promise for construction road works in European countries in summer and winter, as well as countries with tropical climates.

The authors developed technology for obtaining surface composite materials. This technology includes high-energy mechanical treatment, HVOF in a protective atmosphere, subsequent thermomechanical and thermal treatment of ZrCuNiCoTi, cBNNi3AlSiCCoY layers in a protective atmosphere. The processing allowed to increase the adhesive strength of the surface composites, reduce their porosity and improve their functional and operational properties. Staged methods of heat treatment and plastic deformation of surface layers have been developed. These methods stabilize material structure while reducing residual stresses. On the basis of complex X-ray diffraction and electron microscopic studies, the structural parameters of surface composites were determined. It was shown that the ZrCuNiCoTi alloy is in the austenitic-martensitic state and has a nanocrystalline structure with a grain size of 80–120 nm. Meanwhile, the cBNNi3AlSiCCoY alloy consists of many intermetallic phases and inclusions and has a nanosized structure with a grain size of 100–200 nm. A microhardness study of the surface layers in ZrCuNiCoTi – cBNNi3AlSiCCoY composite showed that thermomechanical treatment increases microhardness. The experimental data were statistically processed. As a result, empirical mathematical dependences of the stress amplitude on cyclic durability were compiled. Mechanical tests included tests of NiCoTiZrHf – cBNCoMo, ZrCuNiCoTi – cBNNi3AlSiCCoY, TiNiZrHfCoCu – cBNCoNiAlY composites for multi-cycle fatigue during bending with rotation.

Spectral properties of potassium aluminoborate glasses activated by various concentrations of trivalent chromium compounds are studied. The temperatures of glass transition (434°C) and bulk crystallization of the glass matrix (600°C) are determined. The heat treatment of the glass at the crystallization temperature results in the appearance of intensive narrow luminescence bands in the area of 685–715 nm that is connected with the crystallization of the LiAl7B4O17:Cr3+phase in the glass matrix; in this phase chromium is located in a highly symmetrical octahedral surrounding. Concentration dependences of lifetime and quantum yield show the existence of the concentration luminescence quenching at increasing chromium content in the glass from 0.05 to 0.2 mol %. The maximum value of quantum yield is 30%.

Global dust storms on Mars are rare1,2but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere.

The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today1. A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations2–5. These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere6,7, which—given methane’s lifetime of several centuries—predicts an even, well mixed distribution of methane1,6,8. Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. We did not detect any methane over a range of latitudes in both hemispheres, obtaining an upper limit for methane of about 0.05 parts per billion by volume, which is 10 to 100 times lower than previously reported positive detections2,4. We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater4would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally.

Migrating tides dominate the tropical climate on Mars and are known to reach high amplitudes during global dust events (GDE). In this study, we characterize the amplitude, phase and vertical wavelength of the diurnal and semidiurnal migrating tides in Mars' lower atmosphere (up to 50 km) by exploiting temperature vertical profiles retrieved from TIRVIM, an infrared spectrometer onboard the ExoMars Trace Gas Orbiter covering multiple local times. Observations from the Mars Climate Sounder onboard the Mars Reconnaissance Orbiter are used to complement the local time coverage when needed, and to estimate a seasonal trend to subtract from TIRVIM observations. We focus on two time periods in Martian Year 34, near Ls = 150° and near Ls = 200° (during the 2018 GDE). The characteristics of the migrating tides at Ls = 150° agree very well with tidal theory: a downward propagation, amplitudes of typically 2–5 K, and a larger vertical wavelength for the semidiurnal compared to the diurnal mode. Comparisons with model predictions from the Mars Planetary Climate Model reveal an excellent agreement, except for a slightly different phase of the diurnal tide. During the GDE, the tide pattern changes spectacularly: the diurnal tide amplitude reaches 35 K at 65°S and 17 K at 50°N, being vertically trapped up to 10 Pa. The semidiurnal tide is maximum near 20–30°S with an amplitude of 8–12 K. The phase of this mode is tilted with latitude, which was not the case before the storm. This indicates a significant contribution of the asymmetric Hough modes due to hemispheric asymmetry in the dust distribution. Important temperature variations are observed in the Martian atmosphere at diurnal scale. Part of these variations are due to a phenomenon called migrating thermal tides, which take the form of global oscillations with periods that are diurnal, or fractions of a day (half a day period = semidiurnal, a third of a day = terdiurnal, etc). Using satellite observations sampling different local times on Mars, we separated these different components and derived their amplitude and phase (the local time at which these oscillations peak) in particular during the global dust event that occurred in 2018. During this major storm, diurnal temperature variations reached 65 K at high southern latitudes near 25 km altitude between the late morning (minimum of temperature) and late evening (maximum of temperature). We also report on the characteristics of the semidiurnal tide and even the terdiurnal tide, which have been less studied during dust storms. The phase of the semidiurnal tide is not the same at all latitudes, which we interpret as a consequence of the asymmetric dust distribution (more dust in the southern hemisphere). Our results agree with predictions from a Global Climate Model, although some small disagreements are found, calling for future improvements in the model. The characteristics of the migrating tides derived from TIRVIM at Ls = 150° agree with tidal theory and model predictionsDuring the 2018 global dust event (GDE), the diurnal tide reached an amplitude of 35 K at 65°S and we tentatively detect the terdiurnal tideDuring the 2018 GDE, the semidiurnal tide amplitude reached 10 K at 20°S and exhibited a phase tilt with latitude The characteristics of the migrating tides derived from TIRVIM at Ls = 150° agree with tidal theory and model predictions During the 2018 global dust event (GDE), the diurnal tide reached an amplitude of 35 K at 65°S and we tentatively detect the terdiurnal tide During the 2018 GDE, the semidiurnal tide amplitude reached 10 K at 20°S and exhibited a phase tilt with latitude

For more than 8 years the Venus Monitoring Camera (VMC) onboard the Venus Express orbiter performed continuous imaging of the Venus cloud layer in UV, visible and near‐IR filters. We applied the correlation approach to sequences of the near‐IR images at 965 nm to track cloud features and determine the wind field in the middle and lower cloud (49–57 km). From the VMC images that spanned from December of 2006 through August of 2013 we derived zonal and meridional components of the wind field. In low‐to‐middle latitudes (5–65°S) the velocity of the retrograde zonal wind was found to be 68–70 m/s. The meridional wind velocity slowly decreases from peak value of +5.8 ± 1.2 m/s at 15°S to 0 at 65–70°S. The mean meridional speed has a positive sign at 5–65°S suggesting equatorward flow. This result, together with the earlier measurements of the poleward flow at the cloud tops, indicates the presence of a closed Hadley cell in the altitude range 55–65 km. Long‐term variations of zonal and meridional velocity components were found during 1,200 Earth days of observation. At 20° ± 5°S the zonal wind speed increases from −67.18 ± 1.81 m/s to −77.30 ± 2.49 m/s. The meridional wind gradually increases from +1.30 ± 1.82 m/s to +8.53 ± 2.14 m/s. Following Bertaux et al. (2016) we attribute this long‐term trend to the influence from the surface topography on the dynamical process in the atmosphere via the upward propagation of gravity waves that became apparent in the VMC observations due to slow drift of the Venus Express orbit over Aphrodite Terra. VMC near‐IR (965 nm) images of Venus dayside were used to derive atmospheric circulation in the middle cloud layerFor the first time the closed Hadley cell that encompasses the upper cloud layer (55–67 km) was observedZonal and meridional components of wind speed in the Venusian middle cloud demonstrate a connection with the underlying topography

The influence of optical illumination on transmission of THz radiation through a bulk crystal of semi-insulating GaAs is experimentally studied. It is established that, without additional illumination, absorption of electromagnetic waves with a frequency of about 1 THz in the studied crystal is almost absent. Optical illumination in the spectral range of fundamental absorption of the crystal does not affect the transmission of THz waves. At the same time, if the illumination photon energy is a little below the edge of fundamental absorption, i.e., actually in the transparency region, the transmission of THz radiation drops sharply. At liquid helium temperature, the maximum effect is achieved for the energy of optical photons lower by approximately 30 meV than the crystal band gap. Further shift of the illumination toward lower photon energies is accompanied by almost complete recovery of the transmission. With increasing sample temperature, the spectral range of efficient action of the illumination shifts together with the edge of fundamental absorption toward lower photon energies.

Context. Airglow emissions, such as previously observed from NO and O$_2(a-X)$(0-0) on Venus, provide insight into the chemical and dynamical processes that control the composition and energy balance in the upper atmospheres of planets. The OH airglow emission has been observed previously only in the Earth's atmosphere where it has been used to infer atomic oxygen abundances. The O$_2(a-X)$(0-1) airglow emission also has only been observed in the Earth's atmosphere, and neither laboratory nor theoretical studies have reached a consensus on its transition probability.

Venus is known to have been volcanically resurfaced in the last third of solar system history and to have undergone a significant decrease in volcanic activity a few hundred million years ago. However, fundamental questions remain: Is Venus still volcanically active today, and if so, where and in what geological and geodynamic environment? Here we show evidence from the Venus Express Venus Monitoring Camera for transient bright spots that are consistent with the extrusion of lava flows that locally cause significantly elevated surface temperatures. The very strong spatial correlation of the transient bright spots with the extremely young Ganiki Chasma, their similarity to locations of rift‐associated volcanism on Earth, provide strong evidence for their volcanic origin and suggests that Venus is currently geodynamically active. VMC was able to sound Venus surface through the atmosphere transparency windowTransient bright phenomena were observed in the Ganiki Chasma zoneThey are consistent with hypothesis of lava lakes on the surface

Maximum Satisfiability (MaxSAT) is a well-known optimization version of Propositional Satisfiability (SAT) that finds a wide range of practical applications. This work describes and evaluates the Maximum Satisfiability using the Core-Guided approachsolver (MSCG), which is a robust MaxSATsolver that participated in the MaxSATEvaluation 2014.

The feasibility of compensating for aberrations of the optical-beam initial wavefront by aperture sounding, based on the atmospheric backscatter signal from an additional laser source with a different wavelength, is experimentally studied. It is shown that the adaptive system based on this principle makes it possible to compensate for distortions of the initial beam wavefront on a surface path in atmosphere. Specifically, the beam divergence decreases, while the level of the detected mean backscatter power from the additional laser source increases.

The thermal state of material in the zone of laser action is one of the main integrated parameters to determine the evolution of physicochemical processes and structural phase transformations. The conditions of temperature measurements in laser machining are among the most severe even for noncontact technique of optical pyrometry. From a general point of view, the absence of on-line control and monitoring is one of the main limitations of laser technology integration into modern industry. Data on surface temperature dynamics obtained by pyrometry could be widely used to : (a) understand and optimize the laser processes (i.e. define of the links between surface temperature history and the properties of treated materials) ; (b) create process control on-line including feedback from a pyrometer. The main technical parameters of high speed pyrometer (HSP) are the following : brightness temperature range 1150K (1550K)-3500K (threshold sensitivity depends on selected wavelength) ; error of measurement 1 % ; response time 190 µs ; 200 µm spatial resolution at 350 mm distance of pyrometer from the zone of temperature measurements ; wavelength variation in 2 colour channels from 0.5 to 1.1 µm. The opportunities of actual temperature measurements by high speed high spatial resolution pyrometer system in wide range of laser applications are illustrated by : heat treatment, welding, cladding, and pulsed action.

Key knowledge about planetary composition can be recovered from the study of thermal infrared spectral range datasets. This range has a huge diagnostic potential because it contains diagnostic absorptions from a planetary surface and atmosphere. The main goal of this study is to process and interpret the dataset from the Thermal Infrared channel (TIRVIM) which is part of the Atmospheric Chemistry Suite of the ExoMars2016 Trace Gas Orbiter mission to find and characterize dust and water ice clouds in the atmosphere. The method employed here is based on the application of principal component analysis and target transformation techniques to extract the independent variable components present in the analyzed dataset. Spectral shapes of both atmospheric dust and water ice aerosols have been recovered from the analysis of TIRVIM data. The comparison between our results with those previously obtained on Thermal Emission Spectrometer (TES) data and with previous analysis on TIRVIM data, validates the methodology here applied, showing that it allows to correctly recover the atmospheric spectral endmembers present in the TIRVIM data. Moreover, comparison with atmospheric retrievals on PFS, TES and IRIS data, allowed us to assess the temporal stability and homogeneity of dust and water ice components in the Martian atmosphere over a time period of almost 50 years. The analysis of thermal infrared datasets from planetary bodies is of key importance for the understanding of a planet's climate evolution and history: it contains valuable information about composition, temperature and state of the atmosphere. Moreover, surface properties and the surface‐atmosphere interaction can be studied. Here we investigated new thermal infrared data from the Thermal Infrared channel instrument of the ExoMars Trace Gas Orbiter with the main goal of carefully identifying Martian atmospheric dust and water ice clouds components. A methodology based on principal component and target transformation factor analysis techniques has been applied. Based on our results, this methodology can correctly recover both atmospheric dust and water ice aerosols spectral shapes and their abundances in the Martian atmosphere. First successful application of principal components and target transformation techniques to high‐resolution Thermal Infrared channel (TIRVIM) dataSpectral shapes of both atmospheric dust and water ice clouds are recognized and recoveredTIRVIM data are successfully modeled through a linear combination of the recovered water ice and dust end‐members First successful application of principal components and target transformation techniques to high‐resolution Thermal Infrared channel (TIRVIM) data Spectral shapes of both atmospheric dust and water ice clouds are recognized and recovered TIRVIM data are successfully modeled through a linear combination of the recovered water ice and dust end‐members

We assimilate atmospheric temperature profiles and column dust optical depth observations from the ExoMars Trace Gas Orbiter Atmospheric Chemistry Suite thermal infrared channel (TIRVIM) into the Mars Planetary Climate Model. The assimilation period is Mars Year 34 Ls= 182.3°–211.4°, covering the onset and peak of the 2018 global dust storm. We assimilated observations using the Local Ensemble Transform Kalman Filter with 36 ensemble members and adaptive inflation; our nominal configuration assimilated TIRVIM temperature profiles to update temperature and dust profiles, followed by dust column optical depths to update the total column dust abundance. The observation operator for temperature used the averaging kernels and prior profile from the TIRVIM retrievals. We verified our analyses against in‐sample TIRVIM observations and independent Mars Climate Sounder (MCS) temperature and dust density‐scaled opacity profiles. When dust observations were assimilated, the root‐mean‐square temperature error verified against MCS fell by 50% during the onset period of the storm, compared with assimilating temperature alone. At the peak of the storm the analysis reproduced the location and magnitude of the peak in the nighttime MCS dust distribution, along with the surface pressure diurnal cycle measured by Curiosity with a bias of less than 10 Pa. The analysis winds showed that, at the peak of the storm, the meridional circulation strengthened, a 125 m s−1asymmetry developed in the midlatitude zonal jets, the diurnal tide weakened near the equator and strengthened to 10–15 K at midlatitudes, and the semi‐diurnal tide strengthened almost everywhere, particularly in the equatorial lower atmosphere. ExoMars Trace Gas Orbiter has been in low orbit around Mars since early 2018. During 2018 a large amount of dust was lifted from Mars' surface into the atmosphere. This eventually obscured most of the planet, forming a global dust storm. These storms have a large effect on the temperature and weather in Mars' atmosphere. We used observations from the spacecraft's thermal infrared instrument. This measures how much light comes from the atmosphere and surface at wavelengths where heat is emitted, and can be used to work out the atmospheric temperature and dust content at different times of day. We combined these observations with a numerical model of Mars' atmosphere, considering uncertainties in the measured atmospheric properties and the modeled atmosphere. We compared our results with temperature and dust observations made by Mars Climate Sounder on board Mars Reconnaissance Orbiter. Including dust observations was better than just using temperature observations. While the dust storm was raging, north‐south wind speeds increased, the strong eastward wind in the northern hemisphere became much stronger than in the southern hemisphere, and differences between day and night became larger. Our results mean we can better understand aspects of Mars' atmosphere throughout the daily cycle. We assimilate temperature and dust observations from ExoMars Trace Gas Orbiter‐Atmospheric Chemistry Suite‐TIRVIM during the MY34 global dust storm (GDS)The analysis verifies well against independent Mars Climate Sounder temperature and dust profiles, and Curiosity pressure measurementsAt the peak of the GDS the winds strengthen, the diurnal tide migrates poleward, and the semi‐diurnal tide strengthens We assimilate temperature and dust observations from ExoMars Trace Gas Orbiter‐Atmospheric Chemistry Suite‐TIRVIM during the MY34 global dust storm (GDS) The analysis verifies well against independent Mars Climate Sounder temperature and dust profiles, and Curiosity pressure measurements At the peak of the GDS the winds strengthen, the diurnal tide migrates poleward, and the semi‐diurnal tide strengthens

Carbon monoxide is a non‐condensable gas in the Martian atmosphere produced by the photolysis of CO2. Its abundance responds to the condensation and sublimation of CO2from the polar caps, resulting in seasonal variations of the CO mixing ratio. ACS onboard the ExoMars Trace Gas Orbiter have measured CO in infrared bands by solar occultation. Here we provide the first long‐term monitoring of the CO vertical distribution at the altitude range from 0 to 80 km for 1.5 Martian years from Ls = 163° of MY34 to the end of MY35. We obtained a mean CO mixing ratio of ∼960 ppmv at latitudes from 45°S to 45°N and altitudes below 40 km, mostly consistent with previous observations. We found a strong enrichment of CO near the surface at Ls = 100–200° in high southern latitudes with a layer of 3,000–4,000 ppmv, corresponding to local depletion of CO2. At equinoxes we found an increase of the CO mixing ratio above 50 km to 3,000–4,000 ppmv at high latitudes of both hemispheres explained by the downwelling flux of the Hadley circulation on Mars, which drags the CO enriched air. General circulation models tend to overestimate the intensity of this process, bringing too much CO. The observed minimum of CO in the high and mid‐latitudes southern summer atmosphere amounts to 700–750 ppmv, agreeing with nadir measurements. During the global dust storm of MY34, when the H2O abundance peaks, we see less CO than during the calm MY35, suggesting an impact of HOxchemistry on the CO abundance. Carbon monoxide (CO) is a product of the photodissociation of the main component of the Martian atmosphere, CO2(96%). During the polar night on Mars, the temperature drops so low that ∼30% of the global atmospheric carbon dioxide freezes out, condensed into snowflakes. They settle to the ground to form a seasonal polar cap, which sublimates in spring. Unlike CO2, CO is not a condensable species, so its relative abundance increases when CO2and the atmospheric pressure drops, forming a prominent seasonal cycle. This behavior of CO was well documented by spacecraft measurements of column abundances, while its vertical distribution remained poorly known until recently. Still, it helps to separate the impacts of atmospheric dynamics and chemistry, addressing the problem of the Martian atmosphere's stability. We present the first climatology of the CO vertical distribution lasting more than one Martian year based on solar occultations by the ExoMars Trace Gas Orbiter. We report a previously unobserved CO layer near the surface in high southern latitudes in late winter and spring and document the difference between two Martian years caused by the global dust storm. These observations give new challenges to General Circulation Models for understanding the modern atmosphere of Mars. The first climatology of CO vertical profiles is collected for the period Ls = 163° of Martian Year 34 to the end of Martian Year 35The mean CO volume mixing ratio is ∼960 ppmv at 0–35 km and 45°S–45°NStrong enrichment of CO, >3,000 ppmv, is detected at 10–20 km at Ls = 100–200 in high southern latitudes and above 50 km at equinoxes near Poles The first climatology of CO vertical profiles is collected for the period Ls = 163° of Martian Year 34 to the end of Martian Year 35 The mean CO volume mixing ratio is ∼960 ppmv at 0–35 km and 45°S–45°N Strong enrichment of CO, >3,000 ppmv, is detected at 10–20 km at Ls = 100–200 in high southern latitudes and above 50 km at equinoxes near Poles

The Thermal InfraRed channel in honor of professor Vassili Ivanovich Moroz (TIRVIM) of the Atmospheric Chemistry Suite onboard ExoMars Trace Gas Orbiter has continuously monitored the Martian atmosphere from 13 March 2018 until 2 December 2019, covering almost a complete Martian Year (MY). In the nadir mode of observations, infrared spectra obtained by TIRVIM in the spectral range 600–1,300 cm−1permit retrievals of vertical temperature profiles from the surface up to 60 km of altitude, surface temperatures and column aerosol optical depths. Here we report the retrieved atmospheric thermal structure and the column dust content during the global dust storm (GDS) of MY 34 monitored from Ls= 182.2° to Ls= 211.8° (Solar Longitude), capturing the evolution of the GDS and the response of the atmospheric thermal structure to the changing dust loading. The global storm caused asymmetric atmosphere heating, predominantly in the southern hemisphere, and changed diurnal contrast of atmospheric thermal structure. We also observe a reduced diurnal contrast of surface temperatures at the peak of the GDS. The thermal radiation emitted by Mars in the spectral range 7.7–16.7 μm was measured by the Atmospheric Chemistry Suite Thermal InfraRed channel in honor of professor Vassili Ivanovich Moroz (ACS TIRVIM) onboard ExoMars Trace Gas Orbiter. The nadir spectra carry information about the temperature of the atmosphere at different altitudes thanks to a deep CO2absorption present around 15 μm. Also, the dust loading can be found from the 9‐μm silicate absorption, and the surface temperature can be estimated at 7 μm where the atmosphere is mostly transparent. We follow the evolution of these parameters during the strong global dust storm of Martian Year (MY) 34 (2018). The peculiarity of the ACS TIRVIM data set is the exceptionally dense coverage providing a new look at this otherwise well‐studied dust event. Atmospheric thermal structure and dust content on Mars are retrieved from Atmospheric Chemistry Suite Thermal InfraRed channel nadir measurements in the spectral range 7.7–16.7 μmThe 2018 global dust storm covered the entire planet and caused an asymmetric heating of the atmosphere with a hotter southern hemisphereWe observe a reduced diurnal contrast of surface temperatures and a changed contrast of atmospheric thermal structure during the storm Atmospheric thermal structure and dust content on Mars are retrieved from Atmospheric Chemistry Suite Thermal InfraRed channel nadir measurements in the spectral range 7.7–16.7 μm The 2018 global dust storm covered the entire planet and caused an asymmetric heating of the atmosphere with a hotter southern hemisphere We observe a reduced diurnal contrast of surface temperatures and a changed contrast of atmospheric thermal structure during the storm

Electrolyte solutions, containing the lithium sulfonyl methide salts lithium-tris(trifluoromethanesulfonyl)methide (LiTFSM) and lithium-[bis(trifluoromethylsulfonyl)-pentafluoroethylsulfonyl]methide (LiPFSM) dissolved in organic carbonate solvents, were electrochemically investigated in Li/graphite, Li/LiNi1/3Co1/3Mn1/3O2 (NCM) half-cells and compared to the LiPF6 based electrolyte with regard to their ionic conductivity, electrochemical stability, thermal stability at 60degC and the anodic dissolution behavior vs. Al. While the investigated salts show almost the same performance in Li/graphite half-cells compared to the LiPF6 containing electrolyte, the methide salts show very promising results in Li/NCM half-cells, which depict superior capacity retention as well as higher Coulombic efficiencies compared to the LiPF6 containing electrolyte. Taking the limited anodic stability as well as the occurring anodic dissolution into account, both salts but especially LiTFSM indicate the applicability in lithium ion battery electrolytes for cells with a cutoff potential up to 4.3 V vs. Li/Li+.

Experimental data on studying structural-phase states developed in the subsurface of TiC/Ni-Cr-Al alloy cermet under condition of superfast heating and cooling produced by pulse electron beam melting have been presented in this paper. The effect of the surface structural state multimodality on the temperature dependencies of friction and endurance of the cermet tool in cutting metal has been investigated. The effect of structural states on the cermet’s properties consists in improving its endurance for cutting metal by a factor of 20.

Electrolyte solutions containing the di-lithium cation salts Li2CF(SO2NSO2CF3)2 (abbreviated bisimide), Li2(SO2NSO2CF3)(SO3) (imide-sulfonate), Li2CF2(SO2NSO2CF3)(SO2C(SO2CF3)2 (imide-methanide) dissolved in carbonate solvents were electrochemically investigated on graphite and LiFePO4 electrodes and compared to the electrolyte salt LiPF6. An electrochemical characterization containing the conductivity, the electrochemical stability window, the anodic dissolution behavior of aluminum as well as the thermal behavior at 60degC was performed for these electrolyte solutions. Constant current cycling experiments proved the potential applicability of the investigated salts for use in lithium ion batteries. The order of the salts in regard to their cycling performance reaches from methanide-imide showing the best results over bisimide to imide-sulfonate which is the worst among the investigated salts.

This paper reports a study of the speckle images of a scattered laser beam in the focal plane of a receiver objective, experimentally recorded by a photodetector array, as a function of the laser-pulse energy, the illumination angle of the objective, and the spectral composition of the radiation. Regularities are revealed that connect the statistical parameters of the images under various irradiation conditions. It is shown that the speckles obey Gaussian statistics only at small angles of illumination of the receiver objective.

A homoleptic cyanoborate with nucleophilic boron atom: An unprecedented dianion in the salts M2[B(CN)3] (M=Li, Na, K) with nucleophilic boron in the formal oxidation state +1 was obtained by reductive BC bond cleavage in the [B(CN)4]−anion and characterized by NMR (11B, 13C), vibrational spectroscopy and single crystal X‐ray diffraction.

Ein homoleptisches Cyanoborat mit nukleophilem Boratom:Das beispiellose Dianion in den Salzen M2[B(CN)3] (M=Li, Na, K), das nukleophiles Bor in der Oxidationsstufe +I enthält, wurde durch reduktive B‐C‐Bindungsspaltung im [B(CN)4]−‐Anion erhalten (siehe Schema) und durch 11B‐ und 13C‐NMR‐ und Schwingungsspektroskopie sowie durch Strukturanalyse charakterisiert.

To locate actively geodesic satellites stationed on the low Earth orbits lasers are often used via illumination of the satellites and detection of the laser reflected radiation. But, the lasers can strongly affect electronic devices of the satellites because of scattering of the laser radiation inside its optical systems. To exclude the influence of laser radiation on operating capabilities of the satellites, the characteristic properties of scattered laser radiation in a plane of receiver optical systems are studied in the paper. It is known that scattered laser radiation fields have a speckled character and registered speckles depend on both the laser and photo detector array spectral and power characteristics. In the paper, the laser radiation recorded experimentally in a focal plane of optical system by using photo detector array is investigated at various conditions of the array illumination. Theoretical analysis of the speckles is carried out to determine such characteristics of speckled images as dispersion and covariance and its dependence on the illumination conditions.