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This paper introduces several models for different piezoelectric composites with the modeling process and mechanism. In order to characterize the uniformity and stability, the volume density of particles and fibers changed with volume is studied. The models generated by ANSYS finite analysis are showed, which the codes are produced by the models.

We highlight the impact of cluster-mass-dependent evolutionary rates upon the evolution of the cluster mass function during violent relaxation, that is, while clusters dynamically respond to the expulsion of their residual star-forming gas. Mass-dependent evolutionary rates arise when the mean volume density of cluster-forming regions is mass-dependent. In that case, even if the initial conditions are such that the cluster mass function at the end of violent relaxation has the same shape as the embedded-cluster mass function (i.e. infant weight-loss is mass-independent), the shape of the cluster mass function does change transiently {\it during} violent relaxation. In contrast, for cluster-forming regions of constant mean volume density, the cluster mass function shape is preserved all through violent relaxation since all clusters then evolve at the same mass-independent rate. On the scale of individual clusters, we model the evolution of the ratio between the dynamical mass and luminous mass of a cluster after gas expulsion. Specifically, we map the radial dependence of the time-scale for a star cluster to return to equilibrium. We stress that fields-of-view a few pc in size only, typical of compact clusters with rapid evolutionary rates, are likely to reveal cluster regions which have returned to equilibrium even if the cluster experienced a major gas expulsion episode a few Myr earlier. We provide models with the aperture and time expressed in units of the initial half-mass radius and initial crossing-time, respectively, so that our results can be applied to clusters with initial densities, sizes, and apertures different from ours.

The proposed paper investigates the influence of a coherence degree of superposing mutually orthogonal linearly−polarized waves on the peculiarities of nanosize range particle motion in the inhomogeneously polarized optical field and field of the averaged values of the Poynting vector. In this case the depth of the energy volume density modulation essentially depends on the degree of coherence of interacting waves. The way of monitoring particles of the Rayleigh light scattering mechanism in the energy inhomogeneous optical field is proposed for investigation. The increase of spin flows influence on optical fields studying is analyzed. The possibility of controlling particles of different properties and characteristics becomes possible due to the intrinsic optical flows action.

The interaction of two mutually orthogonal linearly polarized waves in the incidence plane, where the modulation of polarization and the modulation of the energy volume density occur simultaneously in the observation plane is considered. The spatial modulation of polarization in the observation plane forms the spatial modulation of the energy volume density, which changes the velocity of the particle’s motion according to the coherence characteristics of superposing fields and the resulting optical force that causes the motion of tested particles of micrometer range size. Peculiarities of particle’s motion in a spatial periodically modulated polarized field are determined by coherent properties of interacting optical fields.

Background Spontaneously hypertensive rats (SHR) serve as a model of genetic hypertension. Adverse remodeling of a coronary artery has been reported in SHR. This model is used to study new therapies in regression vascular remodeling. However, no data are available that show remodeling of the intramyocardial branch of the obtuse marginal artery in 10-month-old SHR. This study was designed to assess remodeling (changes in vascular structure and fibrosis) of this coronary artery. Methods and results The study was performed on 10-month-old male SHR ( n =7) and normotensive control Wistar Kyoto rats (WKY) ( n =7). Using histology, we show that the external diameter, lumen diameter, wall width, and cross-sectional area of the intramyocardial artery were significantly greater in SHR than in WKY. The wall-to-lumen ratio was similar in SHR and WKY. The collagen volume density of the intramyocardial artery in SHR was significantly greater than in WKY. Conclusions Our results show hypertrophic outward remodeling in the intramyocardial branch of the obtuse marginal artery of the left ventricle in SHR. This artery can serve as a new vascular bed from adult SHR to study novel therapies in regression coronary artery remodeling.

The existence of Jl. Kol. Burlian - Jl. Tanjung Api Api junction becomes very strategic because it becomes the entrance and exit of Palembang city. The intersection is access to several places such as Sultan Mahmud Badaruddin II Airport, Tanjung Api-Api Port, and the border road to Banyuasin. The position of Jl. Kol. Burlian - Jl. Tanjung Api Api junction which is very strategic cause the long queue of vehicles causing traffic jam. To overcome this the South Sumatra Provincial Government will build a fly over at Jl. Kol. Burlian - Jl. Tanjung Api Api junction. Basically the construction of this fly over as an effort to reduce the volume density of vehicles that accumulate at Jl. Kol. Burlian - Jl. Tanjung Api Api junction. The result of calculation using MKJI method calculation, the delay value before the existing fly over or signal condition is 46 seconds / smp, while the length of delay after the fly over dropped dramatically to 16 seconds / smp. Likewise with the calculation using the VISSIMprogram, the results obtained are not much different from the MKJI method, which is 45.23 seconds / smp for the condition before the fly over, and 15.18 seconds / smp for the condition after the fly over. Thus, the development of an efficient fly over in reducing the length of vehicle delays at Jl. Kol. Burlian - Jl. Tanjung Api Api junction, so it is expected to overcome the congestion that always occurs at the intersection.

We establish the connection between the Magellanic Clouds (MCs) and the dwarf galaxy candidates discovered in the Dark Energy Survey (DES) by building a dynamical model of the MC satellite populations, based on an extensive suite of tailor-made numerical simulations. Our model takes into account the response of the Galaxy to the MCs infall, the dynamical friction experienced by the MCs and the disruption of the MC satellites by their hosts. The simulation suite samples over the uncertainties in the MC's proper motions, the masses of the MW and the Clouds themselves and allows for flexibility in the intrinsic volume density distribution of the MC satellites. As a result, we can accurately reproduce the DES satellites' observed positions and kinematics. Assuming that Milky Way (MW) dwarfs follow the distribution of subhaloes in $\Lambda$CDM, we further demonstrate that, of 14 observed satellites, the MW halo contributes fewer than 4 (8) of these with 68% (95%) confidence and that 7 (12) DES dwarfs have probabilities greater than 0.7 (0.5) of belonging to the LMC. Marginalising over the entire suite, we constrain the total number of the Magellanic satellites at ~70, the mass of the LMC around $10^{11}M_\odot$ and show that the Clouds have likely endured only one Galactic pericentric passage so far. Finally, we give predictions for the line-of-sight velocities and the proper motions of the satellites discovered in the vicinity of the LMC., Comment: 23 pages, 17 figures, submitted to MNRAS, comments are welcome

The present study aimed to evaluate primary stability (PS) and osseointegration of dental implants in polylactide [70/30 poly(l-lactide-co-d, l-lactide); (PLDLA)] modified bone in 30 Goettingen minipigs. Each animal received three implants per jaw quadrant. In a split-mouth design, one side of the maxilla and mandible was randomly allocated to the experimental treatment (PLDLA applied into the drill hole before implantation), while the contralateral sides served as intraindividual controls (no PLDLA applied). The required insertion torque and the implant stability quotient (ISQ) were measured during implantation. ISQ, volume density (VD) of new bone formation (NBF), and the bone-implant contact (BIC) were evaluated at the end of the observation period (1, 3, 6, 12, and 24 months, respectively) in six animals each. Across all study groups, the PLDLA treatment resulted in a) a comparable insertion torque, b) an equivalent ISQ, c) a reduced BIC, and d) a reduced VD of NBF, as opposed to the untreated controls. In conclusion, the PLDLA treatment did not affect the PS, but rather led to an impaired osseointegration, which was particularly strong in the compact mandibular bone, and decreased in the spongious maxillary bone. PLDLA induced anchoring in spongious bone should be evaluated in further investigations.

We present a catalogue of dense cores in a $\sim 4^\circ\times2^\circ$ field of the Taurus star-forming region, inclusive of the L1495 cloud, derived from Herschel SPIRE and PACS observations in the 70 $\mu$m, 160 $\mu$m, 250 $\mu$m, 350 $\mu$m, and 500 $\mu$m continuum bands. Estimates of mean dust temperature and total mass are derived using modified blackbody fits to the spectral energy distributions. We detect 525 starless cores of which $\sim10$-20% are gravitationally bound and therefore presumably prestellar. Our census of unbound objects is $\sim85$% complete for $M>0.015\,M_\odot$ in low density regions ($A_V\stackrel{0.1\,M_\odot$ overall. The prestellar core mass function (CMF) is consistent with lognormal form, resembling the stellar system initial mass function, as has been reported previously. All of the inferred prestellar cores lie on filamentary structures whose column densities exceed the expected threshold for filamentary collapse, in agreement with previous reports. Unlike the prestellar CMF, the unbound starless CMF is not lognormal, but instead is consistent with a power-law form below $0.3\,M_\odot$ and shows no evidence for a low-mass turnover. It resembles previously reported mass distributions for CO clumps at low masses ($M\stackrel{, Comment: 17 pages, 12 figures. Accepted for publication in MNRAS

Methodology for analysis of meso-structure effects on longer-scale mechanical response of concrete is developed. Efficient algorithms for particle generation and packing are proposed to represent 3D meso-structures as collections of discrete features distributed randomly in a continuous phase. Specialised to concrete, the continuous phase represents mortar, while the features are aggregates and voids. Intra- and inter-phase cohesive zones are used for failure initiation and crack propagation. A Monte Carlo approach is proposed to analyse the effects of meso-structure geometrical (volume density, size distribution and shape of features) and physical (strength and energy of cohesive zones) properties, whereas a number of model realisations with identical properties are used for statistical analysis. The results present the relative significance of each meso-structure parameter for the emergent load capacity (tensile strength), damage evolution via micro-crack coalescence and macro-crack patterns, and failure energy density (toughness) of concrete. The proposed methodology is an effective tool for meso-structure optimisation in the design of concrete structures with prescribed requirements for strength and toughness.

With a goal toward deriving the physical conditions in external galaxies, we have conducted a survey and subsequent high spatial resolution imaging of formaldehyde (H2CO) and ammonia (NH3) emission and absorption in a sample of starburst galaxies. In this article we present the results from a subset of this survey which focuses on high spatial resolution measurements of volume density- and kinetic temperature-sensitive transitions of the H2CO molecule. The volume density structure toward the nuclear region of NGC 253 has been derived from θ ≃ 4 arcsec NRAO Very Large Array (VLA) measurements of the 110 - 111 and 211 - 212 K-doublet transitions of H2CO. The kinetic temperature structure toward NGC 253 and NGC 4945 has been derived from θ ≃ 0.5 - 1.0 arcsec measurements of the H2CO 3K-1K+1 - 2K-1K+1 (near 218 GHz) and 5K-1K+1 - 4K-1K+1 (near 365 GHz) transitions acquired using the Atacama Large Millimeter/submillimeter Array (ALMA). These measurements have allowed us to characterize the dense gas and kinetic temperature structure within these star forming galaxies, which is a first step toward associating dense star-forming gas and the heating processes at work within galaxies.

Background. This study examines the impact of one-time direct application of haemostatic agent zeolite–bentonite powder to wounded skin on the healing process in rats. Materials and Methods. 24 male Sprague-Dawley rats were randomly allocated into two groups (n=12): (1) the rats whose wounds were washed only with sterile normal saline (NS-treated) and (2) those treated with zeolite–bentonite compound (ZEO-treated). The wound was circular, full-thickness, and 2 cm in diameter. At the end of the 12th day, six animals from each group were randomly selected and terminated. The remaining rats were terminated after 21 days. Just after scarification, skin samples were excised and sent for stereological evaluation. Results. The results showed a significant difference between the two groups regarding the length density of the blood vessels and diameter of the large and small vessels on the 12th day after the wound was inflicted. Besides, volume density of both the dermis and collagen bundles was reduced by 25% in the ZEO-treated rats in comparison to the NS-treated animals after 21 days. Conclusions. One-time topical usage of zeolite–bentonite haemostatic powder on an animal skin wound might negatively affect the healing process through vasoconstriction and inhibition of neoangiogenesis.

In this work, we aim to characterise high-mass clumps with infall motions. We selected 327 clumps from the Millimetre Astronomy Legacy Team 90-GHz (MALT90) survey, and identified 100 infall candidates. Combined with the results of He et al. (2015), we obtained a sample of 732 high-mass clumps, including 231 massive infall candidates and 501 clumps where infall is not detected. Objects in our sample were classified as pre-stellar, proto-stellar, HII or photo-dissociation region (PDR). The detection rates of the infall candidates in the pre-stellar, proto-stellar, HII and PDR stages are 41.2%, 36.6%, 30.6% and 12.7%, respectively. The infall candidates have a higher H$_{2}$ column density and volume density compared with the clumps where infall is not detected at every stage. For the infall candidates, the median values of the infall rates at the pre-stellar, proto-stellar, HII and PDR stages are 2.6$\times$10$^{-3}$, 7.0$\times$10$^{-3}$, 6.5$\times$10$^{-3}$ and 5.5$\times$10$^{-3}$ M$_\odot$ yr$^{-1}$, respectively. These values indicate that infall candidates at later evolutionary stages are still accumulating material efficiently. It is interesting to find that both infall candidates and clumps where infall is not detected show a clear trend of increasing mass from the pre-stellar to proto-stellar, and to the HII stages. The power indices of the clump mass function (ClMF) are 2.04$\pm$0.16 and 2.17$\pm$0.31 for the infall candidates and clumps where infall is not detected, respectively, which agree well with the power index of the stellar initial mass function (2.35) and the cold Planck cores (2.0)., Comment: 26 pages, 26 figures, accepted for publication on MNRAS

The deep, wide-area (~800-900 arcmin**2) near-infrared/WFC3/IR + Spitzer/IRAC observations over the CANDELS fields have been a remarkable resource for constraining the bright end of high redshift UV luminosity functions (LFs). However, the lack of HST 1.05-micron observations over the CANDELS fields has made it difficult to identify z~9-10 sources robustly, since such data are needed to confirm the presence of an abrupt Lyman break at 1.2 microns. We report here on the successful identification of many such z~9-10 sources from a new HST program (z9-CANDELS) that targets the highest-probability z~9-10 galaxy candidates with observations at 1.05 microns, to search for a robust Lyman-break at 1.2 microns. The potential z~9-10 candidates are preselected from the full HST, Spitzer/IRAC S-CANDELS observations, and the deepest-available ground-based optical+near-infrared observations. We identified 15 credible z~9-10 galaxies over the CANDELS fields. Nine of these galaxies lie at z~9 and 5 are new identifications. Our targeted follow-up strategy has proven to be very efficient in making use of scarce HST time to secure a reliable sample of z~9-10 galaxies. Through extensive simulations, we replicate the selection process for our sample (both the preselection and follow-up) and use it to improve current estimates for the volume density of bright z~9 and z~10 galaxies. The volume densities we find are 5(-2)(+3)x and 8(-3)(+9)x lower, respectively, than found at z~8. When compared with the best-fit evolution (i.e., dlog_{10} rho(UV)/dz=-0.29+/-0.02) in the UV luminosities densities from z~8 to z~4 integrated to 0.3L*(z=3) (-20 mag), these luminosity densities are 2.6(-0.9)(+1.5)x and 2.2(-1.1)(+2.0)x lower, respectively, than the extrapolated trends. Our new results are broadly consistent with the "accelerated evolution" scenario at z>8, as seen in many theoretical models., 23 pages, 15 figures, 7 tables, updated to match the version in press, including some minor textual corrections identified at the proof stage

The process of atomic-to-molecular (HI-to-H$_2$) gas conversion is fundamental for molecular-cloud formation and star formation. 21 cm observations of the star-forming region W43 revealed extremely high HI column densities, of 120-180 M$_{\odot}$ pc$^{-2}$, a factor of 10-20 larger than predicted by HI-to-H$_2$ transition theories. We analyze the observed HI with an HI-to-H$_2$ transition theoretical model, and show that the theory-observation discrepancy cannot be explained by the intense radiation in W43, nor by variations of the assumed volume density or H$_2$ formation-rate coefficient. We show that the large observed HI columns are naturally explained by several ($9-22$) HI-to-H$_2$ transition layers, superimposed along the sightlines of W43. We discuss other possible interpretations such as a non-steady-state scenario, and inefficient dust absorption. The case of W43 suggests that HI thresholds reported in extra-galactic observations are probably not associated with a single HI-to-H$_2$ transition, but are rather a result of several transition layers (clouds) along the sightlines, beam-diluted with diffuse inter-cloud gas., Comment: 5 pages, 2 figures. ApJ accepted. Comments welcome

The aim of the present study was to investigate the effect of atrazine (6-chloro-N2-ethyl-N4-isopropyl-1,3,5-triazine-2,4-diamine) on the left ventricle myocardium in juvenile/peripubertal male Wistar rats. Atrazine was administered orally at 50 or 200 mg/kg of body weight dose for 28 consecutive days. In order to assess possible structural alterations, tissue sections were examined histologically and then subjected to quantification analysis using stereological methods. The tissue specimens were routinely processed and stained with Mallory trichrome method in order to clearly distinguish muscle cells from the connective tissue components. A toluidine blue staining method was additionally used for the demonstration of mast cells. Statistically significant increase in length density and numerical density of capillaries were found at both the investigated doses of atrazine compared with the control. The increase in surface density and volume density of capillaries found at lower dosage of atrazine was significant in comparison with the control. The extensive mast cell degranulation was noted on the histological examination at both doses of the applied chemical. No significant changes were demonstrated for the stereological parameters of cardiomyocytes. Based on the available published data and the present results, it can be concluded that atrazine promoted angiogenesis in the rat myocardium, which might be partially mediated by mast cells.

An econometric analysis was conducted to assess how tract, policy, and administrative factors of public timber sales influence willingness to pay for stumpage. To do so, we obtained an electronic database containing multiple years of MN DNR timber-sale records. Each record contained information on the timber sale's total appraised volume, species-product composition, tract acres, date of sale, date of sale expiration, method of sale, purchasing firm, and tract location. A total of 4,395 records of MN DNR timber tracts sold from 2001 to 2006 were analyzed. By incorporating physical, ecological, policy, and administrative factors of a timber sale, our model was able to explain approximately 63% of the variation in the natural log of stumpage prices. Sale-specific characteristics found to be significant drivers of stumpage prices are species-product composition, tract location, end-product market conditions, season of sale, harvestable volume density, length of the sale contract, seasonal operating restrictions, total appraised volume, and auction method.

This work aimed to analyze quantitative changes of peritubular cells in testes of aged men. Testicular tissues were obtained from 42 aged men with advanced prostate cancer and 16 young men with biopsy, quantitatively investigated with stereological techniques with quadrate mask grid, measured the parameters volume density (V(V)), numerical density on area (N(A)), and numerical density (N(V)) with grid test points. No significant differences were found in cell ratio, peritubular cell number per tubule, diameter of seminiferous tubules between young and old men (p0.05). Aged men had higher pathologic assignment score than that of young men, which demonstrated more severe pathologic changes (p0.05). Peritubular cell V(V) and pachytene germ cell V(V) increased significantly in old men compared to young men (p0.05). Sertoli cell (SC) number per tubule in two-dimensional was significantly less in aged men than that of young men, p0.01. Peritubular cell N(A), N(V) decreased significantly in aged men compared to young one, p0.05. It is concluded that the stereological data of peritubular cells from three-dimensional level in testes of aged men suggest a significant decrease when compared with young men, indicating age-related changes.