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This paper addresses light guidance control for human-driven vehicles. We manipulate pace-making-light (PML) installed in the road environment to make drivers accelerate their vehicles unconsciously. Also, since the performance of the control system relies on the human reaction, we address the modeling of the driver's behavior guided by PML. To this end, we tested human subjects by using a driving simulator developed in a virtual reality environment. The collected data were used to model the driver's behavior and to perform a PML control simulation. In particular, the driver model is utilized for the design of a model predictive controller that is implemented as the PML logic.

This study was to investigate the effect of dietary supplementation with xylanase and protease on growth performance, digesta viscosity, apparent ileal digestibility (AID) of nutrients, and gut health in nursery pigs. Forty-eight pigs (24 barrows and 24 gilts at 21 d of age with 7.2 ± 0.4 kg BW) were randomly allotted to 4 dietary treatments (2 × 2 factorial arrangement) in a randomized complete block design and fed in 2 phases (phase 1 for 10 d and phase 2 for 14 d). Factors were xylanase (0 or 45,000 XU/kg) and protease (0 or 300,000 U/kg). Feed intake and BW gain were measured on d 10 and 24. Titanium dioxide (0.25%) was added to all diets as an indigestible external marker from d 20 to 24. On d 24, all pigs were euthanized to obtain jejunal and ileal digesta to measure viscosity and apparent ileal digestibility. The jejunal mucosa was collected to measure immune and oxidative stress status. Jejunal tissues were used to measure morphology and crypt cells proliferation. In phase 2, xylanase increased (P < 0.05) the average daily gain (ADG) which was further increased (P < 0.05) when combined with protease. Overall, combinational use of xylanase and protease increased (P < 0.05) ADG compared with the use of xylanase or protease alone, whereas protease improved (P < 0.05) feed efficiency. In jejunum, xylanase reduced (P < 0.05) viscosity of digesta, mucosal malondialdehyde (MDA), crypt depth and crypt cells proliferation, and protease increased (P < 0.05) villus height, and decreased (P < 0.05) crypt depth and crypt cells proliferation. Collectively, xylanase improved growth performance, digesta viscosity, and oxidative stress, whereas protease improved feed efficiency and gut morphology. The combinational use of xylanase and protease enhanced growth performance of newly weaned pigs.

The atmospheric effects of precipitating electrons are not fully understood, and uncertainties are large for electrons with energies greater than ~30 keV. These electrons are underrepresented in modeling studies today, primarily because valid measurements of their precipitating spectral energy fluxes are lacking. This paper compares simulations from the Whole Atmosphere Community Climate Model (WACCM) that incorporated two different estimates of precipitating electron fluxes for electrons with energies greater than 30 keV. The estimates are both based on data from the Polar Orbiting Environmental Satellite Medium Energy Proton and Electron Detector (MEPED) instruments but differ in several significant ways. Most importantly, only one of the estimates includes both the 0° and 90° telescopes from the MEPED instrument. Comparisons are presented between the WACCM results and satellite observations poleward of 30°S during the austral winter of 2003, a period of significant energetic electron precipitation. Both of the model simulations forced with precipitating electrons with energies >30 keV match the observed descent of reactive odd nitrogen better than a baseline simulation that included auroral electrons, but no higher energy electrons. However, the simulation that included both telescopes shows substantially better agreement with observations, particularly at midlatitudes. The results indicate that including energies >30 keV and the full range of pitch angles to calculate precipitating electron fluxes is necessary for improving simulations of the atmospheric effects of energetic electron precipitation. The study presented here investigates the effects from energetic electron precipitation (EEP) in the southern hemisphere winter of 2003. Electron precipitation is common during periods of enhanced geomagnetic activity and can create reactive nitrogen oxides and hydrogen oxides that can destroy ozone. Most global climate models currently do not include precipitating electrons with energies greater than 30 keV. To test whether this deficiency is important, this investigation compares observations with model simulations that included electrons with energies greater than 30 keV, as observed by the Medium Energy Proton and Electron Detector (MEPED) satellite instruments. In addition, one of the EEP data sets used in the simulations included data from just one of the telescopes on the MEPED instruments, whereas the other included data from both of the telescopes. We found that including both of the telescopes is important for capturing chemistry changes at polar and subpolar latitudes. The model simulation that only included only one of the telescopes showed significant improvement compared to a simulation with only low energy electrons. However, it did not perform as well as the model simulation that included both MEPED telescopes. This work is important because it shows that including energies >30 keV and the full range of precipitating electron pitch angles is necessary to show the impact electrons have on the atmosphere and provides an EEP data set for use in future model simulations. Effects of energetic electron precipitation in southern hemisphere 2003 simulated with Whole Atmosphere Community Climate ModelSimulations of middle atmosphere chemistry improve significantly by including >30‐keV precipitating electronsIncluding the full range of pitch angles is necessary to capture precipitating electron impacts at subpolar latitudes

In December 2022, an extremely low‐density solar wind stream encountered first the Earth and then Mars, shortly after the radial alignment of the two planets (i.e., Mars opposition). As the low‐density stream passed Mars, the properties of the Mars‐solar wind interaction changed dramatically in response to the low solar wind Alfvénic Mach number and dynamic pressure. The Martian magnetosphere and its boundaries expanded by thousands of kilometers, extending outside of the nominal average bow shock location. The low upstream Mach number resulted in a low ratio of plasma to magnetic field pressure in the magnetosheath, allowing the formation of a very high but stable ion temperature anisotropy, together with a very low level of electromagnetic instabilities. Meanwhile, the decrease in solar wind dynamic pressure caused the Martian upper ionosphere at the terminator to transition from a magnetized state to an unmagnetized state. This event provides an opportunity to study a unique end‐member state of the Mars‐solar wind interaction. The solar wind consists of a supersonic flow of hot ionized gas (plasma) from the Sun that flows outward through the solar system. The solar wind interacts with planetary atmospheres and magnetic fields, which form shielded regions known as magnetospheres. The characteristics of the solar wind, including its density and speed, vary over a wide range. The shape, extent, and physical characteristics of planetary magnetospheres in turn respond to these changes in the solar wind. In this work, we study the response of the Martian magnetosphere to an extremely low‐density solar wind stream. During the passage of this stream, the Martian magnetosphere expanded by thousands of kilometers, and its physical characteristics changed dramatically. This event reveals a unique outlier state for the Mars‐solar wind interaction. An extremely low‐density solar wind stream encountered the Earth and Mars just after Mars opposition in December 2022The Martian magnetosheath developed very unusual properties, with a low level of plasma instabilities and a high ion anisotropyThe Martian magnetosphere and its boundaries expanded by thousands of km, extending outside of the location of the nominal bow shock An extremely low‐density solar wind stream encountered the Earth and Mars just after Mars opposition in December 2022 The Martian magnetosheath developed very unusual properties, with a low level of plasma instabilities and a high ion anisotropy The Martian magnetosphere and its boundaries expanded by thousands of km, extending outside of the location of the nominal bow shock

Hydrochlorofluorocarbons (HCFCs), the main substitutes of chlorofluorocarbons, are regulated by the Montreal Protocol. Chinese HCFC emissions increased fast from the beginning of this century. However, limit reports based on atmospheric measurement are available for years after 2011, an important period when significant changes are expected. Combining atmospheric observations at seven sites across China with a FLEXible PARTicle dispersion model‐based Bayesian inversion technique, we estimate emission magnitudes and changes of four major HCFCs in China during 2011–2017. The emissions of all four HCFCs reached peaks before 2015. Our results agreed well with the reported bottom‐up inventories. The Chinese ozone depletion potential (ODP)‐weighted emission of the three most abundant HCFCs accounted for 37% of global totals from 2011 to 2016. The total emission of HCFC‐22 from China, the European Union, and the United States accounted approximately a half of the global totals, suggesting large HCFC emission emitted from the rest of the world. Hydrochlorofluorocarbons (HCFCs) are used to replace chlorofluorocarbons, or well known as Freon, a group of gases which contribute to the polar ozone hole. However, HCFCs are also important ozone depletion substances and are regulated by the Montreal Protocol. As the largest developing country, the HCFC emissions in China are of great interest. In this study, we estimate emission magnitudes and changes of four major HCFCs in China over the period 2011–2017 based on atmospheric observations at seven sites. We find the emissions of all four HCFCs reached their peaks before 2015, which generally agree with the emission inventories estimated using production and consumption information, suggesting the effectiveness of the implementation of Montreal Protocol in China. However, there is a big gap between the total HCFC‐22 emission from China, the European Union, and the United States and global totals, suggesting large emissions from the rest of the world. The Chinese emissions of HCFC‐22, HCFC‐141b, HCFC‐142b, and HCFC‐124 all reached peaks before 2015The Chinese ODP‐weighted emission of the three most abundant HCFCs accounted for 37% of global totals from 2011 to 2016Large gaps were found between the global HCFC‐22 emissions and total HCFC‐22 emissions from the European Union, the United States, and China

We present a study of the magnetic field in the Martian magnetosheath using data from the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission and provide a proxy for the upstream interplanetary magnetic field (IMF) clock angles based on the sheath field directions. The magnetic field data from MAVEN taken in the sheath region are organized in the Mars Solar Electric field coordinate system and sorted by the IMF polarity. The sheath magnetic field distributions clearly illustrate the morphology of draped IMF around the planetary obstacle and show strong asymmetries between the quasi‐perpendicular and quasi‐parallel bow shock quadrants as well as a slight asymmetry between the +Eand –Equadrants. We have also studied the effects of different drivers on the strengths and clock angles of the sheath magnetic field and find that the sheath field is strongly affected by upstream IMF and solar wind and that Martian crustal fields also have small contributions to the sheath magnetic field strength. Based on the morphology of the draped field in the sheath, we developed a simple IMF clock angle proxy as the clock angle of the orbital‐averaged sheath magnetic field, which works well under steady IMF conditions. This proxy has an error <44° for 75% of all instances. The uncertainty of the proxy depends on upstream conditions and spacecraft orbit geometry. We also provide estimates of the proxy uncertainty based on sheath magnetic field variability and proxy clock angle. The magnetic field in the Martian magnetosheath shows asymmetric features with respect to the upstream electric field and IMF directionsThe sheath magnetic field is mainly controlled by IMF and solar wind conditions and slightly modified by Martian crustal fieldsThe sheath magnetic field can be used as an IMF clock angle proxy with an error <45 degrees for 75% of all instances

To analyze the size and location distribution of ruptured intracranial aneurysms (IAs) helps to provide evidence for clinical treatment of unruptured IAs using this feature of aneurysms. In this study, 415 patients who presented with an acute subarachnoid hemorrhage caused by IAs were enrolled from eight tertiary referral centers between June 2016 and March 2018. The size, aspect ratio and anatomic location of ruptured IAs were defined and reported by patient sex. In the study cohort of 415 patients (60.5% women) with saccular ruptured IAs, the three most common locations of ruptured IAs were posterior communicating artery (32.0%), anterior communicating artery (28.7%), and middle cerebral artery (13.5%). The mean size of all ruptured IAs was 5.3±3.1 mm (range 1.1–28.5 mm), but the size varied considerably by location. For example, ruptured IAs of the posterior communicating artery had a mean size of 5.8±3.1 mm, whereas the mean size of ruptured anterior communicating artery aneurysms was 4.6±1.7 mm. The mean AR in all ruptured IAs was 1.66±0.76. Of those aneurysms, 243 (58.6%) had an AR smaller than 1.6 and 318 (76.6%) had an AR smaller than 2.0. Our results suggested that the size of the most ruptured IAs are smaller than 7 mm or even 5 mm. The size and AR varied by sex and location. With the knowledge of size, location and AR, multiplicity should be considered for treatment strategies of unruptured IAs.

The recovery of the stratospheric ozone layer relies on the continued decline in the atmospheric concentrations of ozone-depleting gases such as chlorofluorocarbons1. The atmospheric concentration of trichlorofluoromethane (CFC-11), the second-most abundant chlorofluorocarbon, has declined substantially since the mid-1990s2. A recently reported slowdown in the decline of the atmospheric concentration of CFC-11 after 2012, however, suggests that global emissions have increased3,4. A concurrent increase in CFC-11 emissions from eastern Asia contributes to the global emission increase, but the location and magnitude of this regional source are unknown3. Here, using high-frequency atmospheric observations from Gosan, South Korea, and Hateruma, Japan, together with global monitoring data and atmospheric chemical transport model simulations, we investigate regional CFC-11 emissions from eastern Asia. We show that emissions from eastern mainland China are 7.0 ± 3.0 (±1 standard deviation) gigagrams per year higher in 2014–2017 than in 2008–2012, and that the increase in emissions arises primarily around the northeastern provinces of Shandong and Hebei. This increase accounts for a substantial fraction (at least 40 to 60 per cent) of the global rise in CFC-11 emissions. We find no evidence for a significant increase in CFC-11 emissions from any other eastern Asian countries or other regions of the world where there are available data for the detection of regional emissions. The attribution of any remaining fraction of the global CFC-11 emission rise to other regions is limited by the sparsity of long-term measurements of sufficient frequency near potentially emissive regions. Several considerations suggest that the increase in CFC-11 emissions from eastern mainland China is likely to be the result of new production and use, which is inconsistent with the Montreal Protocol agreement to phase out global chlorofluorocarbon production by 2010. Emissions from eastern China account for approximately 40 to 60 per cent of the global rise in emissions of trichlorofluoromethane (CFC-11), which may be a result of new production and use.

The Total least-squares (TLS) adjustment with inequality constraints has received increased attention in geodesy over the last three years. In the most recent work, inequality constraints have been presented that can restrict unknown parameters and independent variables, but no one has provided an inequality-constrained adjustment for restricting dependent variables. In this work, we review the TLS adjustment methods in terms of different model formulations and then investigate the errors-in-variables model with inequality constraints for dependent variables. Finally, we demonstrate the practicality of our approach with a planar geodetic transformation, where the uncertainty of the target observations is reduced via the inequality constraints for dependent variables.

Si-doped GaN films grown by metal organic chemical vapour deposition have been annealed under different annealing conditions in N2ambient. The annealed films have been characterized by photoluminescence and high resolution X-ray diffraction. The results show that the rapid thermal annealing (RTA) treatment suppresses the yellow and blue luminescence bands in the annealed Si-doped GaN films. For the sample annealed at 850 °C for 3 min, the yellow and blue band intensities even decreases by approximate one order of magnitude over the as-grown sample. In addition, the densities of the edge and screw threading dislocations in the Si-doped GaN also decrease after the RTA treatment. These facts provide the evidence that the RTA technique can effectively improve the crystalline quality of the Si-GaN films.

The diagnosis of polycystic ovary syndrome (PCOS) is based on a combination of various clinical phenotypes in each patient. However, insulin resistance (IR) and dysmetabolism are not included in the diagnostic criteria of PCOS. Therefore, the definition of PCOS is controversial. The objective of this study is to investigate whether some PCOS phenotypes can be predicted by a circulating biomarker related to IR and metabolic dysfunction in PCOS women. One hundred and seventeen women with PCOS and 95 healthy women were recruited for this study. All individuals were assessed by the phenotypic and metabolic characteristics related to PCOS. A euglycemic–hyperinsulinemic clamp was performed to assess insulin sensitivity. Circulating irisin concentrations were determined with ELISA. In our PCOS cohort, 65.8% of individuals were found to have hyperandrogenism. 83.8% had chronic oligoanovulation, and 80.3% of subjects showed polycystic ovaries. According to the diagnostic criteria of PCOS, 30.8% of PCOS subjects were diagnosed with the classic phenotype. In addition, 65.8% of PCOS women had insulin resistance. Serum irisin levels were significantly higher in PCOS women compared with healthy women. However, PCOS women with a normoandrogenic phenotype had similar circulating irisin levels as healthy women. PCOS women with the normoandrogenic phenotype had a low homeostasis model assessment of insulin resistance (HOMA-IR) and higher M-values than PCOS women with other phenotypes. Circulating irisin levels were associated with hyperandrogenism, but not with oligoanovulation or PCO morphology. Circulating irisin may allow physicians to establish which women merit screening by a biomarker for PCOS.

Several studies have shown that diabetes confers a higher relative risk of vascular mortality among women than among men, but whether this increased relative risk in women exists across age groups and within defined levels of other risk factors is uncertain. We aimed to determine whether differences in established risk factors, such as blood pressure, BMI, smoking, and cholesterol, explain the higher relative risks of vascular mortality among women than among men.

The classical Least-Squares (LS) adjustment has been widely used in processing and analysing observations from Global Satellite Navigation System (GNSS). However, in detecting temporal correlations of GNSS observations, which can be described by means of autoregressive (AR) process, the LS method may not provide reliable estimates of process coefficients, since the Yule-Walker (YW) equations refer to structured Errors-In-Variables (EIV) equations. In this contribution, we proposed a Total Least-Squares (TLS) solution with the singular cofactor matrix to solve the YW equations. The proposed TLS solution is obtained based on the fact that random errors belong to column space of its cofactor matrix. In addition the proposed solution does not need any substitution of the squared true parameter vector as done by the current publications. Finally, we simulate the AR process to prove that our solution is more reliable than the existing methods.

Waxy wheat (Triticum aestivumL.) is grown throughout the world for its specific quality. Fertilization and planting density are two crucial factors that affect waxy wheat yield and photosynthetic capacity. The objectives of the research were to determine the effects of fertilization and planting density on photosynthetic characteristics, yield, and yield components of waxy wheat, including Yield, SSR, TGW, GNPP, GWPP, PH, HI, Pn, Gs, Ci, E and WUE using the method of field experiment, in which there were three levels (150, 300, and 450 kg ha–1) of fertilizer application rate and three levels (1.35, 1.8, and 2.25 × 106plants ha–1) of planting density. The results suggested that photosynthetic characteristics, yield, and yield components had close relationship with fertilization levels and planting density. Under the same plant density, with the increase of fertilization, Yield, SSR, TGW, GNPP, GWPP, HI, Pn, Gs, E and WUE increased and then decreased, PH increased, but Ci decreased. Under the same fertilization, with the increase of plant density, Yield, SSR, TGW, GNPP, GWPP, HI increased and then decreased, PH, Pn, Gs and E increased, PH and WUE declined. The results also showed that F2 (300 kg ha–1) and D2 (1.8 × 106plants ha–1) was a better match in this experiment, which could obtain a higher grain yield 4961.61 kg ha–1. Consequently, this combination of fertilizer application rate and plant densities are useful to get high yield of waxy wheat.

Oral verrucous carcinoma (OVC) is a verrucous variant of oral cavity squamous carcinoma (OSCC). The expression of miRNA from OVC and OSCC including their matched normal oral mucosa tissues was profiled through the Affymetrix GeneChip miRNA Arrays. TargetScan and miRanda databases were used to predict the target gene of miRNA-195. The quantitative real-time PCR was applied to validate the expression of miRNA-195. The expression of CDK6 was investigated by the quantitative real-time PCR and immunohistochemistry. In this study, a total of 23 and 35 differentially expressed miRNAs were identified in OVC and OSCC, respectively. Moreover, 44 miRNAs were differentially expressed between OSCC and OVC. In addition, miRNA-195 was significantly decreased in both OVC and OSCC compared to normal oral mucosa. Target gene prediction demonstrated that CDK6 was a potential target gene of miRNA-195. In the quantitative real-time PCR, miR-195 was decreased in OVC and OSCC, which was consistent with the result of miRNA chip analysis. CDK6 was increased in OVC and OSCC, which was opposite to the expression of miRNA-195. In conclusion, miRNA-195 could be the potential diagnosis biomarker and therapy target of OVC.

Post-traumatic stress disorder (PTSD) is characterized by exaggerated fear expression and impaired fear extinction. The underlying molecular and cellular mechanisms of PTSD are largely unknown. The current pharmacological and non-pharmacological treatments for PTSD are either ineffective or temporary with high relapse rates. Here we report that adiponectin-deficient mice exhibited normal contextual fear conditioning but displayed slower extinction learning. Infusions of adiponectin into the dentate gyrus (DG) of the hippocampus in fear-conditioned mice facilitated extinction of contextual fear. Whole-cell patch-clamp recordings in brain slices revealed that intrinsic excitability of DG granule neurons was enhanced by adiponectin deficiency and suppressed after treatment with the adiponectin mimetic AdipoRon, which were associated with increased input resistance and hyperpolarized resting membrane potential, respectively. Moreover, deletion of AdipoR2, but not AdipoR1 in the DG, resulted in augmented fear expression and reduced extinction, accompanied by intrinsic hyperexcitability of DG granule neurons. Adiponectin and AdipoRon failed to induce facilitation of fear extinction and elicit inhibition of intrinsic excitability of DG neurons in AdipoR2 knockout mice. These results indicated that adiponectin action via AdipoR2 was both necessary and sufficient for extinction of contextual fear and intrinsic excitability of DG granule neurons, implying that enhancing or dampening DG neuronal excitability may cause resistance to or facilitation of extinction. Therefore, our findings provide a functional link between adiponectin/AdipoR2 activation, DG neuronal excitability and contextual fear extinction, and suggest that targeting adiponectin/AdipoR2 may be used to strengthen extinction-based exposure therapies for PTSD.

In this Letter, we propose a method to design ultrabroadband near-perfect absorbers, consisting of a periodic dielectric–metal multilayer. In the method, the Bloch theorem and optical topological transition (OTT) of iso-frequency surfaces are employed to manipulate the start and end of the near-perfect spectral absorption band, respectively. Moreover, we design and fabricate an ultrabroadband near-perfect absorber utilizing the proposed method. The average absorption of the designed absorber is ∼95% in the focused visible and near-infrared range (0.4–2 μm). This omnidirectional and polarization-independent near-perfect absorber is promising for solar energy harvesting, emissivity control, and thermal imaging.

We study the Mars Atmosphere and Volatile Evolution spacecraft observations of Martian planetary ion escape during two time periods: 11 November 2014 to 19 March 2015 and 4 June 2015 to 24 October 2015, with the focus on understanding the seasonal variability of Martian ion escape in response to the solar extreme ultraviolet (EUV) flux. We organize the >6 eV O+ion data by the upstream electric field direction to estimate the escape rates through the plume and tail. To investigate the ion escape dependence on the solar EUV flux, we constrain the solar wind dynamic pressure and interplanetary magnetic filed strength and compare the ion escape rates through the plume and tail in different energy ranges under high and low EUV conditions. We found that the total >6 eV O+escape rate increases from 2 to 3 × 1024s−1as the EUV irradiance increases by almost the same factor, mostly on the <1 keV tailward escape. The plume escape rate does not vary significantly with EUV. The relative contribution from the plume to the total escape varies between ~30% and ~20% from low to high EUV. Our results suggest that the Martian ion escape is sensitive to the seasonal EUV variation, and the contribution from plume escape becomes more important under low EUV conditions. The total >6 eV O+ion escape rate increases from 2 to 3 × 1024s−1as the EUV irradiance increases by almost the same factorThe tailward escape rate increases with EUV, while the plume escape rate does not change significantlyThe ratio of the plume escape to the total escape drops from ~30% to ~20% as the EUV increases

Analyzing ~1.3 year data set of O+ion velocity distribution functions obtained from the Suprathermal and Thermal Ion Composition instrument on the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft, we statistically investigate reflections of incident O+pickup ions (>10 keV) occurring below the Martian bow shock. To quantitatively evaluate importance of the reflection of incident O+pickup ions, we estimate reflection ratios by calculating average inward and outward O+ion fluxes above the Martian bow shock. Our result shows that an average reflection ratio is 14.1 ± 6.7%. We also investigate dependences of the reflection ratio on the solar wind, solar EUV flux, and southern hemispheric crustal magnetic field on Mars. We find that the reflection ratio strongly depends on the magnitude of the interplanetary magnetic field (IMF), solar wind dynamic pressure, and gyroradius of O+pickup ions in the solar wind, rather than the solar EUV flux and the crustal magnetic field. We suggest that the reflection ratio is determined by the magnetic field both in the solar wind and below the bow shock that mainly controls gyroradius of incident O+pickup ions in these regions. We also find that the reflection ratio increases to 38.9 ± 10.2% as these parameters become extreme conditions (i.e., IMF magnitude >6 nT). Since incident O+pickup ions are known to be a major source of atmospheric sputtering escape from Mars, our result suggests that ion reflections may have a role to reduce the sputtering escape from Mars under the extreme solar wind condition. Average reflection ratio of incident O+pickup ions from the Martian magnetosheath/magnetic pileup region is ~14%The reflection ratio reaches ~39% under extreme solar wind conditionsThe reflection ratio is determined by magnetic fields both in the solar wind and below the bow shock

The Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft observed a strong interplanetary coronal mass ejection (ICME) impacting Mars on 8 March 2015. We use a time‐dependent global MHD model to investigate the response of the Martian ionosphere and induced magnetosphere to the large solar wind disturbance associated with the ICME. Taking observed upstream solar wind conditions from MAVEN as inputs to the MHD model, the variations of the Martian plasma environments are simulated realistically in a time period from 2.5 h prior to the arrival of the ICME shock to about 12 h after the impact. Detailed comparisons between the model results and the relevant MAVEN plasma measurements are presented, which clearly show that the time‐dependent multispecies single‐fluid MHD model is able to reproduce the main features observed by the spacecraft during the ICME passage. Model results suggest that the induced magnetosphere responds to solar wind variation on a very short time scale (approximately minutes). The variations of the plasma boundaries' distances from the planet along the subsolar line are examined in detail, which show a clear anticorrelation with the magnetosonic Mach number. Plasma properties in the ionosphere (especially the induced magnetic field) varied rapidly with solar wind changes. Model results also show that ion escape rates could be enhanced by an order of magnitude in response to the high solar wind dynamic pressure during the ICME event. A time‐dependent MHD model is used to quantify the impact of a strong ICME on MarsPlasma environment varied rapidly in response to the solar wind disturbancesIon escape rates were enhanced by more than an order of magnitude during the ICME event

Ni–Co electro-brush plating on stainless steel FV520(b) surface was conducted in a perpendicular magnetic field with different intensities. The effects of the applied magnetic field on surface morphology, alloy microstructure, tribological properties and residual stress were investigated by scanning electron microscope, X-ray diffraction, X-ray photoelectron spectroscopy, mechanical tests and a nanoindentation technique. The results showed that a smoother and more uniform Ni–Co alloy coating layer with less defects could be obtained in magnetic field of high intensity. Furthermore, by increasing the intensity of the magnetic field, the content of Co in the alloy coating and the wear resistance of the coating layers increased, and the residual stress decreased. In addition, the magnetic field had a significant influence on the valence change of Ni and Co. In particular, when the intensity of magnetic field was 0.2 T a coating with best integrated performance was obtained.

Ni–Co electro-brush plating on stainless steel FV520(b) surface was conducted in a perpendicular magnetic field with different intensities. The effects of the applied magnetic field on surface morphology, alloy microstructure, tribological properties and residual stress were investigated by scanning electron microscope, X-ray diffraction, X-ray photoelectron spectroscopy, mechanical tests and a nanoindentation technique. The results showed that a smoother and more uniform Ni–Co alloy coating layer with less defects could be obtained in magnetic field of high intensity. Furthermore, by increasing the intensity of the magnetic field, the content of Co in the alloy coating and the wear resistance of the coating layers increased, and the residual stress decreased. In addition, the magnetic field had a significant influence on the valence change of Ni and Co. In particular, when the intensity of magnetic field was 0.2 T a coating with best integrated performance was obtained.

Effects of laser shock peening (LSP) on laser-welded aluminium alloy joints filling Al?+?1.0 wt-% CeO2were investigated. Porosity ratio, microstructure, residual stress, hardness, tensile strength and fracture morphology were evaluated. Double-side LSP decreased the porosity ratio, refined microstructure, relieved the residual compressive stresses and increased the micro-hardness and tensile strength of the welds. Interaction between porosity and residual stress was also illustrated.

Effects of laser shock peening (LSP) on laser-welded aluminium alloy joints filling Al + 1.0 wt-% CeO2were investigated. Porosity ratio, microstructure, residual stress, hardness, tensile strength and fracture morphology were evaluated. Double-side LSP decreased the porosity ratio, refined microstructure, relieved the residual compressive stresses and increased the micro-hardness and tensile strength of the welds. Interaction between porosity and residual stress was also illustrated.

A high rate of aerobic glycolysis is a hallmark of malignant transformation. Accumulating evidence suggests that diverse regulatory mechanisms mediate this cancer-associated metabolic change seen in a wide spectrum of cancer. The echinoderm microtubule-associated protein-like 4-anaplastic lymphoma kinase (EML4-ALK) fusion protein is found in approximately 3–7% of non-small cell lung carcinomas (NSCLC). Molecular evidence and therapeutic effectiveness of FDA-approved ALK inhibitors indicated that EML4-ALK is a driving factor of lung tumorigenesis. A recent clinical study showed that NSCLC harboring EML4-ALK rearrangements displayed higher glucose metabolism compared with EML4-ALK-negative NSCLC. In the current work, we presented evidence that EML4-ALK is coupled to overexpression of hexokinase II (HK2), one of the rate-limiting enzymes of the glycolytic pathway. The link from EML4-ALK to HK2 upregulation is essential for a high rate of glycolysis and proliferation of EML4-ALK-rearranged NSCLC cells. We identified hypoxia-inducible factor 1α (HIF1α) as a key transcription factor to drive HK2 gene expression in normoxia in these cells. EML4-ALK induced hypoxia-independent but glucose-dependent accumulation of HIF1α protein via both transcriptional activation of HIF1α mRNA and the phosphatidylinositol 3 kinase-AKT pathway to enhance HIF1α protein synthesis. The EML4-ALK-mediated upregulation of HIF1α, HK2 and glycolytic metabolism was also highly active in vivoas demonstrated by fluorodeoxyglucose-positron emission tomography imaging of xenografts grown from EML4-ALK-positive NSCLC cells. Our data reveal a novel EML4-ALK-HIF1α-HK2 cascade to enhance glucose metabolism in EML4-ALK-positive NSCLC.

A mixed weighted least squares (WLS) and weighted total least squares (WTLS) (mixed WLS–WTLS) method is presented for an errors-in-variables (EIV) model with some fixed columns in the design matrix. The numerical computational scheme and an approximate accuracy assessment method are also provided. It is extended from the mixed Least squares (LS)–Total least squares (TLS) method to deal with the case that the random columns are corrupted by heteroscedastic correlated noises. The mixed WLS–WTLS method can improve the computational efficiency compared with the existing WTLS methods without loss of accuracy, particularly when the fixed columns are far more than random ones. The Bursa transformation and parallel lines fitting examples are carried out to demonstrate the performance of the proposed algorithm. Since the mixed WLS–WTLS problem includes both the WLS and the WTLS problem, it will have a more wide range of applications.