Understanding membrane fouling mechanisms, particularly the pretreatment-mediated fouling mitigation mechanism, is critical for controlling algal fouling. This study examined the fouling control mechanism of extracellular organic matter (EOM) by combined heat-activated potassium peroxymonosulfate (PMS) and polyaluminum chloride (PACl) treatment using extended Derjaguin-Landau-Verwey-Overbeek (XDLVO)-based interaction energy analysis. Results showed that combined PMS and PACltreatment effectively mitigated membrane fouling, with the fouling control performance being highly dependent on PACldosage. PACl5 mg/L under combined PMS treatment worsened membrane fouling, while PACldosages 10-40 mg/L alleviated it, with the best performance achieved at 40 mg/L. XDLVO theory analysis revealed that PMS-PACl (10-40 mg/L) treatment enhanced repulsive membrane-foulant interactions and transformed membrane-foulants and foulantsfoulants interactions from attractive to repulsive. Moreover, both membrane-foulant and foulant-foulant repulsive interactions increased with increasing PACldosage. In contrast, although integrated PMS and PACl5 mg/L weakened foulant-foulant attractive interaction than control EOM, serious membrane fouling was still observed, likely due to stronger attractive membrane-foulant interactions during the initial filtration stage. This research offers new mechanistic insights into fouling control and provides a theoretical basis for algal-laden water treatment.

Alternating current (AC) electric fields have the potential to induce complex morphological transitions in liquid-liquid systems. In this paper, the instability evolution of the charged methanol droplets in oleic acid under non-uniform AC electric field is investigated by using high-speed imaging. It is found that charged droplets experienced various morphological transitions induced by the AC electric field. For low electric Bond number (Bo(E)), a finger-shaped instability is initiated from the droplet, followed with finger growth and subsequent branching. With the increase in electric field strength, novel morphologies of stretched bottom membrane and radially ejected annulus-shaped film emerge while an explosive Coulomb breakup is found at extremely high field strengths. Throughout the range of instabilities, a transition from disordered to highly ordered polygonal droplet contours is found to be driven by the bifurcation effect in the internal electrohydrodynamics (EHD) flow. Moreover, the growth rate and characteristic wavelength of the instabilities exhibit saturation at high Bo(E). This nonlinear effect is attributed to the dominance of charge convection, which limits the local surface charge density at the finger tips. Overall, the non-uniform AC electric field provides a method for regulating multi-scale fluid interface morphology in high-viscosity-ratio fluids.

Despite significant progress in cosmological simulations of galaxy formation, the role of subgrid physics in shaping the detailed properties of galaxies remains incompletely understood. In this work, we analyze two sets of zoom-in simulations that share identical initial conditions but adopt distinct implementations of baryonic physics, enabling a controlled comparison of their predictions. We examine the stellar properties, morphological structures, and satellite populations of the simulated galaxies at z=0. We find that AURIGA galaxies systematically exhibit higher stellar masses and surface densities than their APOSTLE counterparts. These differences are primarily driven by variations in the efficiency of gas cooling from the circumgalactic medium (CGM) into the star-forming gas. Both simulations form well-defined disk galaxies; however, AURIGA systems generally display higher disk-to-total mass ratios, earlier disk formation, and more prominent dynamical structures such as bars and spiral arms. Nevertheless, strongly disk-dominated systems are present in both simulations, although they do not arise in the same host haloes. The vertical disk structure in both simulations is well described by a sech density profile, with scale heights below 1 kpc in the inner regions. The satellite populations also differ, with AURIGA producing systematically more massive satellites, including a 0.3 dex increase in the most massive system, while the number of satellites above 10^6 M_⊙ remains comparable in most halo pairs. Both simulations reproduce similar satellite stellar mass–metallicity relations, albeit 0.25 dex higher than observation. This comparative study therefore provides useful benchmarks for future efforts to better constrain galaxy formation models.

The impact of cosmic web environments on galaxy properties plays a critical role in understanding galaxy formation. Using the state-of-the-art cosmological simulation IllustrisTNG, we investigate how satellite galaxy abundance differs between filaments and the field, with filaments identified using the DisPerSE algorithm. When filaments are identified using galaxies as tracers, we find that, across all magnitude bins, central galaxies in filaments tend to host more satellite galaxies than their counterparts in the field, in qualitative agreement with observational results from the Sloan Digital Sky Survey. The average ratios between satellite luminosity functions in filaments and the field are 3.49, 2.61, and 1.90 in the central galaxy r -band magnitude bins of M _r _,cen ∼ −22, −21, and −20, respectively. We show that much of this excess can be attributed to the higher host halo masses of galaxies in filaments. After resampling central galaxies in both environments to match the halo mass distributions within each magnitude bin, the satellite abundance enhancement in filaments is reduced by up to 79%. Additionally, the choice of tracers used to identify filaments introduces a significant bias: when filaments are identified using the dark matter density field, the environmental difference in satellite abundance is reduced by more than 70%; after further resampling in both magnitude and halo mass, the difference is further suppressed by another ∼60%–95%. Our results highlight the importance of halo mass differences and tracer choice biases when interpreting and understanding the impact of environment on satellite galaxy properties.

Observations of highly rotationally supported gas discs in high-redshift ( z > 3) star-forming galaxies challenge our understanding of galaxy formation, as the prevailing view holds that galaxies in the early universe are dynamically hot due to frequent mergers, gas accretion, and strong stellar feedback. We examined the kinematic properties of massive (M-* > 10(10) M-circle dot) star-forming galaxies in the TNG50 cosmological hydrodynamical simulation in the redshift range 3 <= z <= 5 . Mock emission-line datacubes were constructed and analysed using the same methodology as for [C ii ] observations with ALMA. We measured the ratio of the gas rotation velocity ( V ) to velocity dispersion (sigma) finding that most galaxies have V/sigma 2-3, lower than observed. However, a few simulated galaxies show V/sigma > 5. Such 'cold' discs, selected at z = 4 , remain dynamically colder than most of the TNG population across z = 3-5. A galaxy with V/sigma > 10 appears in a transient phase that lasts <= 200 Myr. Dynamically cold disc formation in TNG50 is promoted by gas accretion with angular momentum aligned with the pre-existing disc, while most galaxies undergo misaligned accretion. Dynamically cold discs also show lower mass accretion rates and better-aligned stellar and dark-matter angular momentum vectors. By tracing their evolution to z = 0 , we find that one-third become massive disc galaxies and two-thirds become early-type galaxies.

The regulation of particle-laden droplet behavior is crucial for interfacial heat and mass transfer in the liquid-liquid reaction systems. Accordingly, a clear understanding of droplet dynamic behaviors is of crucial importance. In this study, the behaviors of solid-particle-laden droplets in an immiscible dielectric liquid are experimentally investigated under the effect of a non-uniform AC electric field by high-speed imaging. The evolution processes of droplet formation, coalescence, dispersion as well as liquid bridge are analyzed systematically in variable applied voltages and particle concentrations. Results show that the droplet formation process are accelerated by increasing particle concentration, producing smaller droplets. When the applied voltage exceeds a certain threshold, the charged droplet coalescence occurs while the presence of particles would reduce this critical voltage. Cascade coalescence happens in the pure system with increasing voltage while the particle-laden droplets tend to coalesce individually. The droplet dispersion is found to dominate at high electric field strengths with its oscillation angle increased by particle concentration. Additionally, the liquid bridge expansion is reduced by the addition of particles, hindering the droplet coalescence. These findings provide insights into the regulation of particle-laden droplet behavior under the effect of electric fields.

Li-rich Mn-based oxide (LRMO) are promising cathode candidates for next-generation Li-ion batteries with combined cost-effectiveness and high specific capacity. Designing Co-free LRMO can further leverage the low cost of this class of cathodes given the capacity can be maintained. However, implementing cobalt-free LRMO cathode materials are hampered by their sluggish kinetics, resulting in low capacity and poor rate performance that underperform compared with their Co-containing counterparts. Here, it is confirmed that the slow kinetics of Co-free LRMO originates from the structural disorder caused by transition metals (TMs) migration at high voltages (above 4.5 V Vs. Li+/Li) and consequent irreversible oxygen redox process. Aware of this, Na+/F- is introduced in surficial lattice to alleviate these issues, ultimately achieving improved discharge voltage (approximate to 0.2 V above 1 C, 1 C = 0.25 A g-1), exceptional cycle stability in pouch-type cell (95.1% capacity retention in 1 C after 400 cycles at 25 degrees C, and 80.9% capacity retention after 300 cycles in 0.5 C at 45 degrees C) and excellent C-rate performance (approximate to 150 mA h g-1 at 5 C). The newly developed Na+/F- gradient design unleashes the surficial charge transfer kinetics limitation and greatly improves the lattice structure stability, consequently providing valuable guidelines for future high-capacity LRMO cathode design.

Using six Milky Way analogs with two different numerical resolutions from the Auriga simulation, we investigate the total mass, spatial distribution, and kinematics of the Population III (Pop III) star relics in the Milky Way analogs at z = 0. These relics (primarily second-generation stars) formed over a wide redshift range, from about z = 22 to z = 4, with an average formation redshift of z ∼ 10.0, and comprise about 2 × 10 ^−5 of the entire galactic stellar population. The disk and bulge components host only a small fraction of these relics, contributing less than 12% in total. The stellar halo, in particular the outer stellar halo of galactic radius r > 30 kpc, hosts the largest fraction (about 46% on average), with an average of one relic star per 4000 to 10,000 stars, making it a promising region for observational searches. Additionally, around 18% of the Pop III star relics are found in satellite galaxies, with smaller and older satellite galaxies tending to contain a higher proportion of these stars. Thus, low-mass and early-formed satellite galaxies are also ideal targets for finding such relics, although some satellite galaxies may lack them entirely. The spatial distribution and kinematics of these stars show good numerical convergence across different simulation resolutions. Our results provide valuable guidance for searches of the Pop III star relics and offer insights for interpreting findings from ongoing and future stellar archaeology surveys.

A major challenge in circumgalactic medium (CGM) studies is determining the three-dimensional (3D) properties from the observed projected observations. Here, we decompose the 3D gas density and spatial distribution of cool clouds by fitting a cool CGM model with the absorption observations, including the cool gas density, Ly alpha, and Mg ii equivalent widths. The clumpiness in the cool CGM is considered by modelling individual clouds. This model has four major components: the radial profile of the cool gas density; the number density of clouds; the absorption properties within individual clouds; and the velocity dispersion in the CGM. The observed cool gas density exhibits a large dispersion of approximate to 2-3 dex within the virial radius (r(vir)). This dispersion can be reproduced with a combination of the projection effect (i.e. distant low-density clouds projected at small radii) and the intrinsic variation in the gas density. By modelling the probability density functions of gas density at different radii, the cool gas density is modelled as a beta-model with a characteristic gas density of log n(H,0)/cm(-3) = -2.57(-0.25)(+0.43) at r(vir) and a slope of beta(c) = 0.63(-0.20)(+0.16), and the intrinsic dispersion is sigma(nH) approximate to 0.56(-0.20)(+0.19) dex. Assuming a cloud mass of 10(4) M-circle dot, we further constrain the number density of cool clouds by jointly reproducing Ly alpha and Mg ii equivalent width samples, resulting into a number density of log n(Ncl,0)/r(vir)(-3) = 4.76(-0.21)(+0.27) at r(vir) and a slope of beta(Ncl) = 0.65(-0.07)(+0.06). This spatial distribution of the cool CGM leads to a total cool gas mass of log M-cool/M-circle dot = 10.01(-0.06)(+0.06) for L* galaxies, while varying the cloud mass from 10(3) to 10(6) M-circle dot leads to the total cool CGM mass of 9.62(-0.07)(+0.05) to 10.46(-0.05)(+0.05).

Dark matter halos are spun up by tidal torques originating from large-scale structures, resulting in an average spin parameter—a dimensionless measure of halo angular momentum—of approximately 0.04. Measurement of this angular momentum is crucial for validating the ΛCDM model and understanding the evolution of fundamental characteristics of the galaxy such as morphology and size. However, due to the invisible nature of dark matter, measuring the actual value angular momentum of dark halos is challenging. Here we report the first measurement for the value of angular momentum of dark matter haloes using a novel methodology. By stacking the orbital motions of satellite galaxies according to the projected rotation axes of their central galaxies, we calculate the projected orbital angular momentum of these satellites. This value is then converted into the intrinsic angular momentum of the dark matter halos using a conversion factor obtained from sophisticated hydrodynamical simulations. Applying this method to a selection of galaxy groups and clusters from the Sloan Digital Sky Survey (SDSS), we observe dark matter halo spins ranging between 0.0025 and 0.066 for halos with masses from [1012.5,1014] M⊙. These results are in excellent agreement with the predictions from the widely accepted ΛCDM model, thus substantiating a fundamental aspect of the theory of structure formation.

Utilizing the apostle-auriga simulations, which start from the same zoom-in initial conditions of Local Group-like systems, but run with different galaxy formation subgrid models and hydrodynamic solvers, we study the impact of stellar feedback models on the evolution of angular momentum in disc galaxies. At z=0, auriga disc galaxies tend to exhibit higher specific angular momenta compared to their cross-matched apostle counterparts. By tracing the evolution history of the Lagrangian mass tracers of the in-situ star particles in the z=0 galaxies, we find that the specific angular momentum distributions of the gas tracers from the two simulations at the halo accretion time are relatively similar. The present-day angular momentum difference is mainly driven by the physical processes occurring inside dark matter haloes, especially galactic fountains. Due to the different subgrid implementations of stellar feedback processes, auriga galaxies contain a high fraction of gas that has gone through recycled fountain (similar to 65 per cent) which could acquire angular momentum through mixing with the high angular momentum circumgalactic medium (CGM). In apostle, however, the fraction of gas that has undergone the recycled fountain process is significantly lower (down to similar to 20 per cent for Milky Way-sized galaxies) and the angular momentum acquisition from the CGM is marginal. As a result, the present-day auriga galaxies overall have higher specific angular momenta.

ABSTRACT The origin of diverse kinematic morphologies observed in low-mass galaxies is unclear. In this study, we investigate the kinematic morphologies of central galaxies with stellar mass $10^{8.5-9.0}{\rm M}_{\odot }$ at $z=0$ in the TNG50-1 cosmological simulation. The majority of the low-mass galaxies in TNG50-1 are dispersion-dominated, consistent with observations. By tracing the evolutionary histories of simulated low-mass galaxies, we find that while most stars form in rotating cold gas discs, the orientation of the star-forming discs relative to the galaxies may evolve with cosmic time. If the cold gas disc remains aligning with the galaxy during its evolution, stars formed at different times share the same rotational direction, leading to a rotation-dominated system. On the contrary, frequent misalignment of cold gas disc would result in a dispersion-dominated system. In addition, we also find that the two-body scattering can have a non-negligible numerical heating effect on the simulated galaxy morphology, especially at central regions of galaxies and for relatively low-mass galaxies. By comparing results of simulations with different resolutions, our results suggest that the simulated morphology of galaxies is roughly reliable when their number of stellar particles exceeds about $10^{4}$, and bulge morphology of galaxies can not be resolved robustly at the resolution level of TNG50-1.

The size of the pressure field is affected by the concave shape and area of the optical element.In order to study the formation of the pressure field of the concave surface,first it is necessary to establish a polished optical element model,and simulate and analyze the pressure of the concave surface;by chan-ging the curvature radius of the concave surface of the optical element,changing the rotation speed of the polishing wheel,and changing the optical element with the same radius of curvature to immerse into the magnetic and the angle in the rheological fluid,the concave surface pressure is calculated.Finally,it is an-alyzed and found that the radius of curvature has little effect on the pressure of the concave surface.The pressure distribution of the concave surface with different radius of curvature in the magnetorheological polishing flow field is similar;the pressure change trend of the concave surface first decreases gently,then decreases rapidly,and finally tends to become flatten out.The effect of changing the rotation speed of the polishing wheel on the concave surface pressure is only the change of the maximum pressure on the con-cave surface.The rotation speed of the polishing wheel is directly proportional to the maximum pressure on the concave surface.The pressure change trend is fast in the front area,and the middle area decelerates faster,and the pressure in the back area tends to become gentle.Changing the angle at which the concave surface is immersed in the polishing solution changes significantly.The pressure in the first half of the con-cave surface decreases sharply and then tends to be flat,and the pressure in the back section of the con-cave surface is almost unchanged.

The galaxy-galaxy lensing technique allows us to measure the subhalo mass of satellite galaxies, studying their mass loss and evolution within galaxy clusters and providing direct observational validation for theories of galaxy formation. In this study, we use the weak gravitational lensing observations from DECaLS DR8, in combination with the redMaPPer galaxy cluster catalog from Sloan Digital Sky Survey data (SDSS) DR8 to accurately measure the dark matter halo mass of satellite galaxies. We confirm a significant increase in the stellar-to-halo mass ratio of satellite galaxies with their halo-centric radius, indicating clear evidence of mass loss due to tidal stripping. Additionally, we find that this mass loss is strongly dependent on the mass of the satellite galaxies, with satellite galaxies above $10^{11}~{\rm M_{\odot}/h}$ experiencing more pronounced mass loss compared to lower mass satellites, reaching 86\% at projected halo-centric radius $0.5R_{\rm 200c}$. The average mass loss rate, when not considering halo-centric radius, displays a U-shaped variation with stellar mass, with galaxies of approximately $4\times10^{10}~{\rm M_{\odot}/h}$ exhibiting the least mass loss, around 60\%. We compare our results with state-of-the-art hydrodynamical numerical simulations and find that the satellite galaxy stellar-to-halo mass ratio in the outskirts of galaxy clusters is higher compared to the predictions of the Illustris-TNG project about factor 5. Furthermore, the Illustris-TNG project's numerical simulations did not predict the observed dependence of satellite galaxy mass loss rate on satellite galaxy mass.

To reduce switch numbers and voltage stress in semiconductor devices, this paper proposes a novel single-phase converter combined Active Power Factor Correction (APFC) with switched-capacitor converter. In addition, dynamic voltage regulation and voltage gain are improved by integrating the boost converter and switching capacitor cells. The interstage bulk capacitor is no longer needed. An average current control with redistribution of voltage in cells is proposed to obtain voltage lift ability of the switching capacitor cells and maintain a high-power factor. To study and verify the proposed converter preliminarily, theoretical analysis and simulation are presented in the paper. Furthermore, a 500 W prototype with two different configurations is built for experimental verification. The proposed converter can reach 95.62% of maximum efficiency, 0.99 of power factor, and 3.55% of THD with 600 V output voltage, simultaneously.

It remains a mystery when our Milky Way first formed a stellar disk component that survived and maintained its disk structure from subsequent galaxy mergers. We present a study of the age-dependent structure and star formation rate of the Milky Way’s disk using high-α stars with substantial orbital angular momentum that have precise age determinations. Our results show that the radial scale length is nearly independent of age, whereas the vertical scale height experienced dramatic evolution. A disk-like geometry presents even for populations older than 13 Gyr, with the scale height-to-length ratio dropping below 0.5 for populations younger than 12.5 Gyr. We dub the oldest population that has maintained a disk geometry—apparently formed over 13 Gyr ago—PanGu. With an estimated present-day stellar mass of approximately 2 × 109 M⊙, PanGu is presumed to be a major stellar component of our Galaxy in the earliest epoch. The total present-day stellar mass of the whole high-α disk is 2 × 1010 M⊙, which was mostly formed during a distinct star formation rate peak of 11 M⊙ per year around 11 Gyr ago. A comparison with Milky Way analogues in the TNG50 simulations implies that our Galaxy has experienced an exceptionally quiescent dynamical history, even before the Gaia–Enceladus merger. The Milky Way contains an extremely long-lived stellar disk component that formed, according to this study, more than 13 billion years ago. Such longevity is due to the exceptionally quiescent dynamical history of the Galaxy.

After skin tissue trauma, wound infections caused by bacteria posed a great threat to skin repair. However, resistance to antibiotics, the current treatment of choice for bacterial infections, greatly affected the efficiency of anti-infection and wound healing. Therefore, there has been a critical need for the development of novel antimicrobial materials and advanced therapeutic methods to aid in skin repair. In this paper, rGO-PDA@ZIF-8 nanofillers were prepared by coating graphene oxide (GO) with dopamine (DA), followed by in situ growth of zeolite imidazolate framework-8 (ZIF-8). Using polyvinyl alcohol (PVA) and chitosan quaternary ammonium salt (CS) as matrix materials, along with polyethylene glycol (PEG) as a pore-forming agent, and rGO-PDA@ZIF-8 as an antimicrobial nano-filler, we successfully prepared rGO-PDA@ZIF-8/PVA/CS composite hydrogels with a directional macroporous structure using bidirectional freezing method and phase separation technique. This hydrogel exhibited excellent mechanical properties, good solubility and water retention capabilities. In addition, the hydrogel demonstrated excellent biocompatibility. Most notably, it not only exhibited excellent bactericidal effect against E. coli and S. aureus (99.1 % and 99.0 %, respectively) under the synergistic effect of intrinsic antibacterial activity and photothermal antibacterial, but also exhibited the ability to promote wound healing, making it a promising candidate for wound healing applications.

Roofs occupy a great proportion of urban impervious surfaces, and the implementation of eco-roof construction in urban areas is beneficial to alleviate the ecological and environmental problems caused by rapid urbanization. In this study, different eco-roofs (i.e., 68.6%-90.7%, and 39.8%-54.5%, respectively. However, all the eco-roofs were sources of NO-3-N, DCr, DFe, and DNi. The blue roof was a sink of DCu (with a pollutant load reduction rate of 21.9%) and did not affect the cumulative load of PO3-4-P in runoff. However, the green roof and blue-green roof were the sources of PO3-4-P and DCu. The RQI value of the blue roof was the highest, followed by that of the blue-green roof and green roof. The RQI value of the green roof was significantly lower than that of the blue and blue-green roofs (P<0.05). These results indicated that the runoff quality of the blue roof was the best, whereas that of the green roof was the worst. Adding a storage layer to the green roofs could significantly improve the runoff quality. The results of this study provide scientific references for the selection and design of eco-roof facilities.

A novel single-phase hybrid switching capacitor APFC converter is proposed in this paper. By integrating the boost APFC converter with the switching capacitor converter, the active switch number is reduced, the voltage gain is increased with a high power factor. The dynamic voltage regulation is also improved with no need for the large capacitor. Besides, in order to achieve APFC and the boost capability of switching capacitor cells simultaneously, this paper proposes an average-current control with mode dispatching method. The theoretical analysis of this converter is studied and verified preliminarily through simulation. A 500W with 85-265V AC input and 600V DC output voltage prototype is built to evaluate experimentally. The efficiency of the proposed converter is around 95.33% with a power factor above 0.99.

[目的]绿色屋顶具有滞留雨水、削减和延缓洪峰等径流调控功能,但植物根系对其径流调控功能的影响尚不清楚.本研究旨在揭示植物根系对绿色屋顶径流调控功能的影响,为绿色屋顶植物配置和管理提供科学支撑.[方法]基于在北京城区搭建的 3种不同根系特征植物(佛甲草、大花马齿苋、八宝景天)和无植被覆盖(对照)绿色屋顶的降雨产流和基质含水量动态变化监测,测定植物根长密度和根径等根系特征,定量分析植物根系对绿色屋顶径流调控功能的影响.[结果]含根系绿色屋顶基质的平均雨水滞蓄量比对照绿色屋顶高 2.1～4.1 mm,但平均产流时间较对照绿色屋顶提前6～10 min,平均峰现时间提前 9～26 min.在总根长密度相近的情况下,根茎较粗的八宝景天绿色屋顶的径流调控功能优于根茎较细的大花马齿苋绿色屋顶.佛甲草绿色屋顶的总根长密度和平均根径最大,其雨水初损占比最低,最易产流,且随着降雨量的增大,其径流调控效益相对其他两种植物的绿色屋顶下降更明显.[结论]植物根系可提高绿色屋顶基质的滞蓄能力,但会导致绿色屋顶产流提前;同时根系的径级分布也会影响绿色屋顶的径流调控功能.