Total Density Distribution Research Articles

Effect of moving walkway arrangement on unidirectional crowd flow characteristics

As moving walkways (MWs) are being used in larger airport terminals, train stations and so on, there is growing concern about their impact on the crowd movement. Some existing applications have shown that these passenger conveyors are not always capable of providing a better level of service, therefore, it is necessary to examine the effect of MWs on crowd dynamics thoroughly. In this work, we first construct more realistic numerical experimental scenarios and utilize a macroscopic continuum pedestrian model to simulate crowd movement in long corridors with the MWs under various conditions, including demand level, operation speed, position, landing area, and layout. Then, based on the comparison of experiment results such as total travel time, density distribution, queue size, and total crowd pressure, we analyze the effect of MWs on unidirectional crowd dynamics. From the results, we prove that the presence of a landing area between two segments of MWs can help to split the flow in the main direction and enhance the safety of crowd movement. Moreover, according to our research, compared to increasing the operation speed, modifying the position and layout of MWs is more effective and cost-saving in improving traffic efficiency. In summary, this paper investigates the effect of MWs and provides a better understanding to organizers when designing pedestrian conveyor systems.

Using Three-Dimensional Information to Predict and Interpret the Facial Selectivities of Nucleophilic Additions to Cyclic Ketones.

In this study, we devised a new method to predict facial selectivity by quantifying steric and orbital factors for the nucleophile approaching both π-plane faces. Using this method, we quantified the total electron density and frontier orbital distributions of 163 cyclic ketones with various structures and quantitatively explained the surface selectivity of 323 reactions with eight nucleophiles (BH3, LiAlH4, NaBH4, LiAl(OMe)3H, MeLi, MeMgI, PhLi, and PnMgI). Importance analysis showed a large orbital effect for BH3, LiAlH4, and NaBH4 and the dominance of the steric effect for LiAl(OMe)3H, MeLi, MeMgI, PhLi, and PhMgI. Our method analyzes three-dimensional features based on Gaussian cube files, which can be easily obtained using mainstream computational chemistry software packages, and this approach should prove useful for predicting the rates and facial selectivity of other reactions.

Dust around Massive Stars Is Agnostic to Galactic Environment: New Insights from PHAT/BEAST

Resolving the environments of massive stars is crucial for understanding their formation mechanisms and their impact on galaxy evolution. An important open question is whether massive stars found in diffuse regions outside spiral arms formed in situ or migrated there after forming in denser environments. To address this question, we use multiresolution measurements of extinction in the Andromeda galaxy (M31) to probe the interstellar medium surrounding massive stars across galactic environments. We construct a catalog of 42,107 main-sequence massive star candidates (M ≥ 8 M ⊙) using resolved stellar photometry from the Panchromatic Hubble Andromeda Treasury (PHAT) program, plus stellar and dust model fits from the Bayesian Extinction and Stellar Tool (BEAST). We quantify galactic environments by computing surrounding stellar densities of massive stars using kernel density estimation. We then compare high-resolution line-of-sight extinction estimates from the BEAST with 25 pc resolution dust maps from PHAT, measuring the total column density distribution of extinction. Our key finding is that, although the average total column density of dust increases with the density of massive stars, the average line-of-sight extinction toward massive stars remains constant across all environments. This suggests that massive stars have a uniform amount of dust in their immediate environment, regardless of their location in the galaxy. One possible explanation for these findings is that small molecular clouds are still capable of forming massive stars, even if they are not resolvable at 25 pc. These results indicate that massive stars are forming in the sparse regions of M31, as opposed to migrating there.

Phonon Transport Characteristics of Nano-Silicon Thin Films Irradiated by Ultrafast Laser under Dispersion Relation

The gray model simplifies calculations by ignoring phonon polarization, but sacrifices a certain level of computational accuracy. In effect, the frequency and wavevector of phonons form complex polarization patterns, which means their propagation modes and vibrational directions have different influences. Therefore, based on the phonon dispersion relations in silicon, the lattice Boltzmann method is used to analyze the phonon transport characteristics in nano-silicon films under ultrafast laser excitation. The results show that the total energy density distribution obtained by superimposing acoustic and optical branches exhibits multiple wave-like behaviors. Among them, the acoustic branch has excellent transfer capability, dominating the rate at which the total energy density reaches a steady state distribution, while the optical branch has stronger heat capacity characteristics, with a greater impact on the peak value of the total energy density. When the heat transfer approaches a steady state, the longitudinal optical branch surprisingly contributes up to 52.73%. This indicates that the often-neglected optical phonons should also receive sufficient attention. Additionally, compared to the results of the gray model, it is found that the dispersion model is preferred when more attention is paid to the propagation characteristics during phonon transport.

The surface mass density of the Milky Way: does the traditional KZ approach work in the context of new surveys?

ABSTRACT We revisit the classical KZ problem – determination of the vertical force and implied total mass density distribution of the Milky Way disc – for a wide range of Galactocentric radius and vertical height using chemically selected thin and thick disc samples based on Apache Point Observatory Galactic Evolution Experiment spectroscopy combined with the Gaia astrometry. We derived the velocity dispersion profiles in Galactic cylindrical coordinates, and solved the Jeans equation for the two samples separately. The result is surprising that the total surface mass density as a function of vertical height as derived for these two chemically distinguished populations is different. The discrepancies are larger in the inner compared to the outer Galaxy, with the density calculated from thick disc being larger, independent of the Galactic radius. Furthermore, while there is an overall good agreement between the total mass density derived for the thick disc population and the standard halo model for vertical heights larger than 1 kpc, close to the mid-plane the mass density observed using the thick disc population is larger than that predicted from the standard halo model. We explore various implications of these discrepancies, and speculate their sources, including problems associated with the assumed density laws, velocity dispersion profiles, and the Galactic rotation curve, potential non-equilibrium of the Galactic disc, or a failure of the Navarro-Frenk-White (NFW) dark matter halo profile for the Milky Way. We conclude that the growing detail in hand on the chemodynamical distributions of Milky Way stars challenges traditional analytical treatments of the KZ problem.

Statistical analysis of discrete dislocation dynamics simulations: initial structures, cross-slip and microstructure evolution

Over the past decades, discrete dislocation dynamics simulations have been shown to reliably predict the evolution of dislocation microstructures for micrometer-sized metallic samples. Such simulations provide insight into the governing deformation mechanisms and the interplay between different physical phenomena such as dislocation reactions or cross-slip. This work is focused on a detailed analysis of the influence of the cross-slip on the evolution of dislocation systems. A tailored data mining strategy using the ‘discrete-to-continuous (D2C) framework’ allows to quantify differences and to quantitatively compare dislocation structures. We analyze the quantitative effects of the cross-slip on the microstructure in the course of a tensile test and a subsequent relaxation to present the role of cross-slip in the microstructure evolution. The precision of the extracted quantitative information using D2C strongly depends on the resolution of the domain averaging. We also analyze how the resolution of the averaging influences the distribution of total dislocation density and curvature fields of the specimen. Our analyzes are important approaches for interpreting the resulting structures calculated by dislocation dynamics simulations.

Study on the effect of different sandwich materials on the impact resistance of laminated glass

In this paper, four types of laminated glass with various sandwich materials, polyvinyl butyral (PVB), polyurethane (PU), ethylene vinyl acetate (EVA), and SentryGlas® Plus (SGP), were selected to obtain the impact mechanical parameters and crack space development of laminated glass under different impact velocities by using light gas gun flyer plate variable velocity impact combined with CT scan-3D reconstruction technique. The findings demonstrated that different impact velocities had various demands on the elastic modulus of the sandwich material, showing the impact resistance demands of low velocity-high flexibility and high velocity-high rigidity. From the full-dimensional crack characterization under the medium-velocity impact, it could be seen that the comprehensive characteristics of the sandwich material viscosity, ductility, and rigidity led to different total volume, density, and spatial distribution complexity of cracks. This research provides important practical value and technical support for the selection and improvement of laminated glass.

The Star Formation–Gas Density Relation in Four Galactic GMCs: Effects of Stellar Feedback

We present maps of four Galactic giant molecular clouds (GMCs) in the J = 2-1 emission of both CO and 13CO. We use an LTE analysis to derive maps of the CO excitation temperature and column density and the distribution of total molecular gas column density, Σgas. The depletion of CO by freeze-out onto cold dust grains is accounted for by an approximation to the results of Lewis et al., which were derived from far-IR observations with Herschel. The surface density of young stellar objects (YSOs) is obtained from published catalogs. The mean YSO surface density exhibits a power-law dependence on Σgas, with exponents in the range 0.9–1.9. Gas column density probability distribution functions show power-law tails extending to high column densities. The distributions of sonic Mach number, M S , are sharply peaked at MS ∼ 5–8 for 3 GMCs; a fourth has a broad distribution up to M S = 30, possibly a result of feedback effects from multiple OB stars. An analysis following the methodology of Pokhrel et al. finds that our sample of GMCs shows power-law relations that are somewhat shallower than those found by Pokhrel et al. for the star formation rate versus 〈Σgas〉 and versus 〈Σgas〉/t ff in a different sample of clouds. We discuss possible differences in the two samples of star-forming clouds and the effects of stellar feedback on the relation between gas density and star formation rate.

Differential perivascular microglial activation in the deep white matter in vascular dementia developed post-stroke.

With the hypothesis that perivascular microglia are involved as neuroinflammatory components of the gliovascular unit contributing to white matter hyperintensities on MRI and pathophysiology, we assessed their status in stroke survivors who develop dementia. Immunohistochemical and immunofluorescent methods were used to assess the distribution and quantification of total and perivascular microglial cell densities in 68 brains focusing on the frontal lobe WM and overlying neocortex in post-stroke dementia (PSD), post-stroke non-dementia (PSND) and similar age control subjects. We primarily used CD68 as a marker of phagocytic microglia, as well as other markers of microglia including Iba-1 and TMEM119, and the myeloid cell marker TREM2 to assess dementia-specific changes. We first noted greater total densities of CD68+ and TREM2+ cells per mm2 in the frontal WM compared to the overlying cortex across the stroke cases and controls (p=0.001). PSD subjects showed increased percentage of activated perivascular CD68+ cells distinct from ramified or primed microglia in the WM (p < 0.05). However, there was no apparent change in perivascular TREM2+ cells. Total densities of TREM2+ cells were only ~10% of CD68+ cells but there was high degree of overlap (>70%) between them in both the WM and the cortex. CD68 and Iba-1 or CD68 and TMEM119 markers were colocalised by ~55%. Within the deep WM, ~30% of CD68+ cells were co-localised with fragments of degraded myelin basic protein. Among fragmented CD68+ cells in adjacent WM of PSD subjects, >80% of the cells expressed cleaved caspase-3. Our observations suggest although the overall repertoire of perivascular microglial cells is not changed in the parenchyma, PSD subjects accrue more perivascular-activated CD68+ microglia rather than TREM2+ cells. This implies there is a subset of CD68+ cells, which are responsible for the differential response in perivascular inflammation within the gliovascular unit of the deep WM.

Evaluation of brushless DC motor structure design for the electric impact using 3-D finite element analysis

In this article, an analytical model is deployed to optimize and design an interior permanent magnet brushless DC motor (IPMBLDC motor) when compared to theoretical structure of IPMBLDC. In this motor, assume air-gap of magnet assembly, distribution of flux density coefficient, selection of functional point in the permanent magnet, Torque density, and permanent magnet dimension compares with air-gap were deployed in an ideal design model. An equivalent circuit of magnetic field was improved and compare with the total flux density distribution and the torque density efficiency is based on initial ideal design factors. In finite element of MAXWELL 3D method, an electromagnetic field is investigated and used to verify an advanced equivalent circuit of magnetic field and improve the IPMBLDC motor factors. Finally, simulation results of IPMBLDC motor are verify and compare with ideal factors of IPMBLDC motor.

On the polytropic Bondi accretion in two-component galaxy models with a central massive BH

ABSTRACT In many investigations involving accretion on a central point mass, ranging from observational studies to cosmological simulations, including semi-analytical modelling, the classical Bondi accretion theory is the standard tool widely adopted. Previous works generalized the theory to include the effects of the gravitational field of the galaxy hosting a central black hole and of electron scattering in the optically thin limit. Here, we apply this extended Bondi problem, in the general polytropic case, to a class of new two-component galaxy models recently presented. In these models, a Jaffe stellar density profile is embedded in a dark matter halo such that the total density distribution follows a r−3 profile at large radii; the stellar dynamical quantities can be expressed in a fully analytical way. The hydrodynamical properties of the flow are set by imposing that the gas temperature at infinity is proportional to the virial temperature of the stellar component. The isothermal and adiabatic (monoatomic) cases can be solved analytically; in the other cases, we explore the accretion solution numerically. As non-adiabatic accretion inevitably leads to an exchange of heat with the ambient, we also discuss some important thermodynamical properties of the polytropic Bondi accretion and provide the expressions needed to compute the amount of heat exchanged with the environment as a function of radius. The results can be useful for the subgrid treatment of accretion in numerical simulations, as well as for the interpretation of observational data.

An initial assessment of the distribution of total Flash Rate Density (FRD) in Brazil from GOES-16 Geostationary Lightning Mapper (GLM) observations

Brazil is one of the regions in the world where lightning most occurs. With the launch of the Geostationary Environmental Operational Satellite – 16 (GOES-16), it was possible, for the first time, to carry out an almost uniform resolution mapping, in near real time, of total lightning with a field of view that covers most of the western hemisphere. The objective of this study was to evaluate the initial spatio-temporal distribution of the Total Lightning Flash Rate Density (FRD) for all of Brazil, and to determine lightning hotspots in cities in five regions, the South, the Southeast, the Midwest, the Northeast, and the North. Total lightning flash data from the Geostationary Lightning Mapper (GLM) sensor on board the GOES-16 were evaluated for a three-years period (from 2018 to 2020). The greatest FRD (about 30 fl km−2 season−1) occurred during the hot season (between spring and summer), mostly in the late afternoon (12–18 Local Hour, LH), in the northwest-southeastern portion of the country (AM, PA, MT, GO and TO), in the southeastern of RJ and closer to the Brazil-Argentina border (MS, PR, SC and RS). The lowest FRD values were observed along coastal regions, extending from the north of RJ to AP, and for the north of RO and PA. São Félix do Xingu city in Pará came in first (131 fl km−2 year−1) in the national ranking for lightning hotspots, showing well-defined monthly and daytime cycles with maximums at 14 LH.

Miniaturized peptidomimetics and nano-vesiculation in endothelin types through probable nano-disk formation and structure property relationships of endothelins’ fragments

Abstract Endothelins (ETs), which are multi-functional-peptides with potential for antagonist-based-therapy in various physiological-malfunctionings, including cardiovascular, nephrological, oncologic, and diabetic conditions, may produce newer chemical entities and drug leads. The present study deals with molecular-modeling of the ETs’ sub-types, ET-I, II, and III to find the structure property-relationship (SPR) of the ETs, and individual fragments derived from the ET sub-type ET-I. The ETs peptidic tails’ amino acid (AA) sequence’s structural differences and similarities, various dissected fragments of the ET-I, and SPR comparison with the sarafotoxin-6b (SRT-6b), a structurally-related snake-venom, showed points of dissimilarities for their structural specifications, geometric disposition, and physico-chemical properties. The generation of miniaturized (shortened sequence) peptides towards offering peptidomimetic compounds of near- and far-values compared SPR with estimations for log P, hydration energy, and other molecular and quantitative structure activity relationship (QSAR) were based on random and ordered-fragments derived from the original ET-I AA’s sequence, and sequential distance changes in the original ET-I sequence’s chain of 1–21 AA. The feasibility of alternate and bond length parameters-based possible cysteine–cysteine cyclizations, sequence homology, AA’s positional demarcation, and presence/absence of cysteines, homology-based basic non-cysteine and cysteines-AA based cyclization, total structure and fragments end-to-end cyclizations, and geometrical analogy-based miniaturized sequence of the shorter AAs from the original ET-I sequence, together with mutated replacements with naturally constituent AAs of the ETs, and SRT-6 sequences were utilized. The major findings of the fragmented sequences, and sequences at par with the original ETs to provide structures similar to the size, volume and with molecular and electronic properties of electrostatic potential and total charge density distribution, crucial factors in receptor bindings were investigated. The SPRs, molecular properties, and QSAR values were estimated to compare and validate the findings with the known homologous compounds, ET-I, and its known and potent antagonists. The study resulted in leads of smaller and larger sizes of peptide-based compounds which may have prospects as potent antagonist and in future needs their bioactivity evaluations after the synthesis. Moreover, approach to plausible vesiculation of the ETs, and the involved processes and structural requirements, together with the molecular interactions in settling a nano-vesicle of the peptidic structure with a possible mechanism is also suggested.

A New Type of Tri-Input TFET with T-Shaped Channel Structure Exhibiting Three-Input Majority Logic Behavior

In this paper, we propose a new type of tri-input tunneling field-effect transistor (Ti-TFET) that can compactly realize the “Majority-Not” logic function with a single transistor. It features an ingenious T-shaped channel and three independent-biasing gates deposited and patterned on its left, right, and upper sides, which greatly enhance the electrostatic control ability between any two gates of all the three gates on the device channel and thus increase its turn-on current. The total current density and energy band distribution in different biasing conditions are analyzed in detail by TCAD simulations. The turn-on current, leakage current, and ratio of turn-on/off current are optimized by choosing appropriate work function and body thickness. TCAD simulation results verify the expected characteristics of the proposed Ti-TFETs in different working states. Ti-TFETs can flexibly be used to implement a logic circuit with a compact style and thus reduce the number of transistors and stack height of the circuits. It provides a new technique to reduce the chip area and power consumption by saving the number of transistors.

Tip Charge Dependence of Three-Dimensional AFM Mapping of Concentrated Ionic Solutions.

A molecular scale understanding of the organization and structure of a liquid near a solid surface is currently a major challenge in surface science. It has implications across different fields from electrochemistry and energy storage to molecular biology. Three-dimensional AFM generates atomically resolved maps of solid-liquid interfaces. The imaging mechanism behind those maps is under debate, in particular, for concentrated ionic solutions. Theory predicts that the observed contrast should depend on the tip's charged state. Here, by using neutrally, negatively, and positively charged tips, we demonstrate that the 3D maps depend on the tip's polarization. A neutral tip will explore the total particle density distribution (water and ions) while a charged tip will reveal the charge density distribution. The experimental data reproduce the key findings of the theory.

Control of chirality, bond flexing and anharmonicity in an electric field

AbstractWe located “hidden” S‐character chirality in formally achiral glycine using a vector‐based interpretation of the total electronic charge density distribution. We induced the formation of stereoisomers in glycine by the application of an electric field. Control of chirality was indicated from the proportionate response to a non‐structurally distorting electric field. The bond‐flexing was determined to be a measure of bond strain, which could be a factor of three lower or higher, depending on the direction of the electric field, than in the absence of the electric field. The bond‐anharmonicity was found to be approximately independent of the electric field. We also compared the formally achiral glycine with the chiral molecules alanine and lactic acid, quantifying the preferences for the S and R stereoisomers. The proportional response of the chiral discrimination to the magnitude and direction of the applied electric field indicated use of the chirality discrimination as a molecular similarity measure.

Tensor force and deformation in even-even nuclei

The variational principle is used to build a model which describes open shell nuclei with ground state deformations. Hartree-Fock equations are solved by using single particle wave functions whose radial parts depend on the projection of the angular momentum on the quantization axis. Pairing effects are taken into account by solving Bardeen-Cooper-Schrieffer equations in each step of the minimisation procedure. The Gogny D1S finite-range interaction and an extension of it that includes tensor terms are consistently used in both parts of our calculations. The model is applied to study a set of isotopes with 34 protons and of isotones with 34 neutrons. Total energies, density distributions, their radii and single particle energies are analysed and the results of our calculations are compared with the available experimental data. We focused our attention on the effects of the deformation and of the tensor force on these observables. Our model describes open shell nuclei from a peculiar perspective and opens the possibility of future theoretical developments.

Ab initio study of the structural, electronic, mechanical, dynamical, thermodynamic, linear and nonlinear optical properties of [formula omitted] quaternary alloys

The quaternary alloys BeSiP2xAs2(1−x) with the noncentrosymmetric chalcopyrite structure are studied by means of ab initio density functional theory calculations. The calculations are shown the substitution of Asby P leads to the decrease of the volume of the unit cell and the increase of the energy band gap. Using the Zunger approach, the microscopic origins of the energy band gap bowing are examined in term of volume deformation bVD, charge exchange bCEand structural relaxation bS.The analysis of the total electron density distribution map is shown that the electrons flow from the As, Si and P atoms and accumulate into covalent bonds between the As and Si atoms and between the Si and P atoms. The effect of Pconcentration on the mechanical properties, phonon frequencies and Born effective charges Z∗ of these quaternary alloys are also investigated. The calculated results indicated that these quaternary alloys are mechanical and dynamically stable, have a brittleness character and can be regarded as elastically anisotropic materials. Moreover, the thermodynamic properties of these quaternary alloys including the heat capacity at constant volume CV, the Helmholtz free energy F and entropy S are calculated using the harmonic approximation based on the phonon density of states calculation. Finally, the nonlinear optical coefficient d36 of the quaternary alloys BeSiP2xAs2(1−x) is evaluated and the results confirm that these alloys are remarkable in the nonlinear optics.

Weighing the Galactic disk in sub-regions of the solar neighbourhood using Gaia DR2

Aims. We infer the gravitational potential of the Galactic disk by analysing the phase-space densities of 120 stellar samples in 40 spatially separate sub-regions of the solar neighbourhood, using Gaia’s second data release (DR2), in order to quantify spatially dependent systematic effects that bias this type of measurement. Methods. The gravitational potential was inferred under the assumption of a steady state in the framework of a Bayesian hierarchical model. We performed a joint fit of our stellar tracers’ three-dimensional velocity distribution, while fully accounting for the astrometric uncertainties of all stars as well as dust extinction, and we also masked angular areas of known open clusters. The inferred gravitational potential is compared, post-inference, to a model for the baryonic matter and halo dark matter components. Results. We see an unexpected but clear trend for all 40 spatially separate sub-regions: Compared to the potential derived from the baryonic model, the inferred gravitational potential is significantly steeper close to the Galactic mid-plane (≲60 pc), but flattens such that the two agree well at greater distances (∼400 pc). The inferred potential implies a total matter density distribution that is highly concentrated to the Galactic mid-plane and decays quickly with height. We see a dependence on the Galactic radius that is consistent with a disk scale length of a few kiloparsecs. Apart from this, there are discrepancies between stellar samples, implying spatially dependent systematic effects which are, at least in part, explained by substructures in the phase-space distributions. Conclusions. In terms of the inferred matter density distribution, the very low matter density that is inferred at greater heights (≳300 pc) is inconsistent with the observed scale height and matter distribution of the stellar disk, which cannot be explained by a misunderstood density of cold gas or other hidden mass. Our interpretation is that these results must be biased by a time-varying phase-space structure, possibly a breathing mode, that is large enough to affect all stellar samples in the same manner.

Two-component galaxy models with a central BH – II. The ellipsoidal case

ABSTRACTRecently, two-component spherical galaxy models have been presented, where the stellar profile is described by a Jaffe law, and the total density by another Jaffe law, or by an r−3 law at large radii. We extend these two families to their ellipsoidal axisymmetric counterparts: the JJe and J3e models. The total and stellar density distributions can have different flattenings and scale lengths, and the dark matter halo is defined by difference. First, the analytical conditions required to have a nowhere negative dark matter halo density are derived. The Jeans equations for the stellar component are then solved analytically, in the limit of small flattenings, also in the presence of a central BH. The azimuthal velocity dispersion anisotropy is described by the Satoh k-decomposition. Finally, we present the analytical formulae for velocity fields near the centre and at large radii, together with the various terms entering the virial theorem. The JJe and J3e models can be useful in a number of theoretical applications, e.g. to explore the role of the various parameters (flattening, relative scale lengths, mass ratios, rotational support) in determining the behaviour of the stellar kinematical fields before performing more time-expensive integrations with specific galaxy models, to test codes of stellar dynamics and in numerical simulations of gas flows in galaxies.