Miracle-dz/UniFAR-FTUs huggingface dataset:
Research on the Impact of Smart Home Service Innovation on Consumers' Willingness to Use from the Perspective of Privacy Concerns

In order to explore the influence mechanism of smart home service innovation on consumers' willingness to use, this paper constructs a chain mediation model of smart home service innovation on consumers' willingness to use through perceived intrusiveness and perceived value, and explores the moderating role of privacy concerns in the model. The results show that :(1) Smart home service innovation has a significant positive impact on consumers' willingness to use; (2) Perceived value and perceived intrusiveness played a partially mediating role in the positive impact of smart home service innovation on consumers' willingness to use, respectively; (3) Perceived intrusiveness and perceived value play a chain-mediated role in the positive impact of smart home service innovation on consumers' willingness to use; (4) Privacy concerns moderated the two partial mediating pathways, that is, the stronger the privacy concerns, the weaker the positive mediating effect of perceived value, and the stronger the negative mediating effect of perceived intrusive. This paper explores the mechanism of the impact of smart home service innovation on consumers' willingness to use from the perspective of privacy concerns, which is a supplement and enrichment to previous studies, and also provides valuable ideas for the physical retail industry to properly handle consumers' privacy and improve consumers' willingness to use.
Antibacterial polymeric micelles based on kojic acid/acrylic acid/chitosan

Abstract In the present study, antibacterial micelles based on poly [5-(benzyloxy)-4-oxo-4H-pyran-2-yl] methyl acrylate/polyacrylic acid/chitosan(PBOPMA-PAA-Cs) terpolymer with suspended kojic acid groups was synthesized. For this purpose, first, protected kojic acid (BOP) was prepared by reaction of 5-hydroxy-2-hydroxymethyl-4 H-pyran-4-one with benzyl chloride. Subsequently, [5-(benzyloxy)-4-oxo-4H-pyran-2-yl] methyl acrylate(BOPMA) was prepared by esterification reaction between protected kojic acid hydroxyl groups and carboxylic groups related to acrylic acid. The initiator, [5-(benzyloxy)-4-oxo-4H-pyran-2-yl] methyl-2-bromo-2-methylpropanoate (BOPBr), was synthesized via acyl nucleophilic substitution. Polymerization of BOPMA by ATRP polymerization using initiator (BOPBr) was performed. The PBOPMA-PAA copolymer was prepared by free radical polymerization. In the final step, PBOPMA-PAA-Cs terpolymer was prepared by esterification reaction of the N-phthaloylated chitosan hydroxyl group with the carboxylic acid groups of the PBOPMA-PAA copolymer. Micelles with a size of 20 ± 5 nm were prepared from amphiphilic terpolymers and their morphology and size were evaluated by TEM and DLS, respectively. The structure, thermal stability, and morphology of synthesized compounds were confirmed by FT-IR, 1H-NMR, TGA, and SEM. Furthermore, in the study of antibacterial properties against gram-positive and negative bacteria, PBPMA, PBPMA-PAA, and PBPMA-PAA-Cs behaved differently, however, all three had good antibacterial properties compared to gentamicin and ampicillin. Graphical Abstract
Comparison between bone height changes around the splinted and non-splinted OT bridge system implants in edentulous mandibles rehabilitated with all-on four full arch prosthesies a randomized clinical trial

Objectives: the aim of this study was to compare the difference in marginal bone loss around the splinted and non-splinted implants supported on OT bridge system in full arch implant mandibular restoration using the All-On -Four concept. Materials and methods: This study was conducted on 12 completely edentulous patients having 48 implants. All patients were treated with a mandibular implant supported fixed restoration. Four implants were placed interforaminally for each patient and restored with immediately loaded restoration following the All-On-Four concept. Comparison was made between the splinted implants and non-splinted implants of immediately loaded temporary conversion prosthesis using OT bridge system regarding the marginal bone loss (MBL) using digital periapical radiograph at base line and after 3 months. Results: The marginal bone loss around both groups splinted and non-splinted implants after 3 months of immediate loading was similar with no statistically significant difference. Conclusion: Both techniques are considered as reliable methods for immediate loading of a full arch screw retained implant restoration with no preference of one approach regarding marginal bone loss around implants.
Star Formation with Adaptive Mesh Refinement Radiation Hydrodynamics

Abstract I provide a pedagogic review of adaptive mesh refinement (AMR) radiation hydrodynamics (RHD) methods and codes used in simulations of star formation, at a level suitable for researchers who are not computational experts. I begin with a brief overview of the types of RHD processes that are most important to star formation, and then I formally introduce the equations of RHD and the approximations one uses to render them computationally tractable. I discuss strategies for solving these approximate equations on adaptive grids, with particular emphasis on identifying the main advantages and disadvantages of various approximations and numerical approaches. Finally, I conclude by discussing areas ripe for improvement.
A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018 M⊙ (assuming κ850 = 1.7 cm2 g−1). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼8500 K, luminosity of log(L/L⊙) = 5.32, and a relatively high mass-loss rate of 1.0 × 10−5 M⊙ yr−1. The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼8 M⊙ is comparable to its nebular mass of ∼5.5 M⊙ (from an assumed gas-to-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region.
Adsorption of SO2 air pollutant gas molecule on the pure and Al-doped graphene nano sheet: A DFT study

The interaction of pure graphene nano sheet and Al-doped graphene nano sheet with SO2 pollutant gas molecules was examined by density functional theory (DFT). Adsorption energies and the transferred Mulliken charge were calculated. Doping Al on the graphene improved adsorption and electronic properties of graphene. Dos plots and HOMO-LUMO band gaps showed that pure graphene and Al-doped were semiconductor materials. The results revealed that sensitivity of graphene-based materials was enhanced by doping Al on the surface of pure graphene. Thus, Al-doped graphene was found to be a better detector of SO2 gas molecules.
A modified fuzzy C‐means algorithm using scale control spatial information for MRI image segmentation in the presence of noise

The fuzzy C‐means (FCM) algorithm does not fully utilize the spatial information for image segmentation and is sensitive to the presence of noise and intensity inhomogeneity in magnetic resonance imaging (MRI) images. The underlying reason is that using a single fuzzy membership function the FCM algorithm cannot properly represent pattern associations to all clusters. In this paper, we present a modified FCM (mFCM) algorithm by incorporating scale control spatial information for segmentation of MRI images in the presence of high levels of noise and intensity inhomogeneity. The algorithm utilizes scale controlled spatial information from the neighbourhood of each pixel under consideration in the form of a probability function. Using this probability function, a local membership function is introduced for each pixel. Finally, new clustering centre and weighted joint membership functions are introduced based on the local membership and global membership functions. The resulting mFCM algorithm is robust to the noise and intensity inhomogeneity in MRI image data and thereby improves the segmentation results. The experimental results on a synthetic image, four volumes of simulated and one volume of real‐patient MRI brain images show that the mFCM algorithm outperforms k‐means, FCM and some other recently proposed FCM‐based algorithms for image segmentation in terms of qualitative and quantitative studies such as cluster validity functions, segmentation accuracy and tissue segmentation accuracy. Copyright © 2015 John Wiley & Sons, Ltd.
A Wavelet-Based Compressive Deep Learning Scheme for Inverse Scattering Problems

Recently, physics-assisted deep learning schemes (DLSs) have demonstrated the state-of-the-art performance for solving inverse scattering problems (ISPs). However, most learning approaches typically require a high-computational overhead and a big memory footprint, which prohibits further applications. In this work, a wavelet-based compressive scheme (WCS) is proposed in solving ISPs, where the multisubspace information is explored by wavelet bases and branched between each encoder and decoder path. It is shown that the proposed WCS can be simply adapted to commonly used DLSs, such as the back-propagation scheme (BPS) and the dominant current scheme (DCS), to reduce the computational and storage load. Specifically, benefiting from compressive and multiresolution properties of wavelet and with the help of the factorized convolution method, more than 99.7% trainable weights are reduced in both illustrated back-propagation (BP)-WCS and dominant current (DC)-WCS, whereas the performance deterioration is limited around 1% in terms of traditional BPS and DCS. Extensive numerical and experimental tests are conducted for quantitative validations. Comparisons are also made among UNet, a well-known compressive method (Mobile-UNet), and the proposed method. It is expected that the suggested compression technique would find its applications on deep learning-based electromagnetic inverse problems under source-limited scenarios.
Making programming part of teachers' everyday life – Programming affordances and constraints for K-12 mathematics and technology

PurposeThe conducted examination of programming affordances and constraints had the purpose of adding knowledge and value that facilitate the on-going national curricula revision; knowledge that also could be of general interest outside the Swedish K-12 context.Design/methodology/approachWith a qualitative approach, the study was conducted as a document analysis where submitted lesson plans were the base for a directed content analysis.FindingsThis study presents findings on how the involvement of programming in mathematics and technology have potential to foster engagement and motivation among students. Findings also indicate that the implementation of programming can develop important general skills that go beyond the boundaries of mathematics and technology. Moreover, the identified constraints could be valuable to improve the on-going curriculum development for K-12 mathematics and technology.Research limitations/implicationsThis qualitative study was conducted on a relatively small number of teachers where the majority has taken the courses on a voluntary basis. An important complement would be to conduct a larger quantitative study with data from a more general sample of K-12 teachers.Practical implicationsResults and discussions provide guidance for K-12 teachers and other stakeholders who want to introduce programming as a complementary tool in teaching and learning activities.Social implicationsThe study has a contribution to the on-going implementation of the Swedish national curricula for K-12 mathematics and technology.Originality/valueDuring the last years, many studies have been published on teacher training in programming, and how the training can be improved. This study goes beyond the actual teacher training and examine aspects teachers translate to theirs daily work after completing the training.
The Type Ia supernovae rate with Subaru/XMM-Newton Deep Survey

We present measurements of the rates of high-redshift Type Ia supernovae derived from the Subaru/XMM-Newton Deep Survey (SXDS). We carried out repeated deep imaging observations with Suprime-Cam on the Subaru Telescope, and detected 1040 variable objects over 0.918 deg(2) in the Subaru/XMM-Newton Deep Field. From the imaging observations, light curves in the observed i band are constructed for all objects, and we fit the observed light curves with template light curves. Out of the 1040 variable objects detected by the SXDS, 39 objects over the redshift range 0.2 <z <1.4 are classified as Type Ia supernovae using the light curves. These are among the most distant SN Ia rate measurements to date. We find that the Type Ia supernova rates increase up to z similar to 0.8 and may then flatten at higher redshift. The rates can be fitted by a simple power law, r(V)(z) = r(0)(1 + z)(alpha) with r(0) = 0.20(0.16)(+0.52)(stat.)(0.07)(+0.26)(syst.) x 10(-4) yr(-1) Mpc(-3), and alpha = 2.04(-1.96)(+1.84) (stat.)(-0.86)(+2.11)(syst.).
Understanding the large-distance behavior of transverse-momentum-dependent parton densities and the Collins-Soper evolution kernel

There is considerable controversy about the size and importance of non-perturbative contributions to the evolution of transverse momentum dependent (TMD) parton distribution functions. Standard fits to relatively high-energy Drell-Yan data give evolution that when taken to lower Q is too rapid to be consistent with recent data in semi-inclusive deeply inelastic scattering. Some authors provide very different forms for TMD evolution, even arguing that non-perturbative contributions at large transverse distance bT are not needed or are irrelevant. Here, we systematically analyze the issues, both perturbative and non-perturbative. We make a motivated proposal for the parameterization of the non-perturbative part of the TMD evolution kernel that could give consistency: with the variety of apparently conflicting data, with theoretical perturbative calculations where they are applicable, and with general theoretical non-perturbative constraints on correlation functions at large distances. We propose and use a scheme- and scale-independent function A(bT) that gives a tool to compare and diagnose different proposals for TMD evolution. We also advocate for phenomenological studies of A(bT) as a probe of TMD evolution. The results are important generally for applications of TMD factorization. In particular, they are important to making predictions for proposed polarized Drell- Yan experiments to measure the Siversmore » function. « less
Stable probability laws modeling random propagation times of waves crossing different media

In a communication scheme, there exist points at the transmitter and at the receiver where the wave is reduced to a finite set of functions of time which describe amplitudes and phases. For instance, the information is summarized in electrical cables which preceed or follow antennas. In many cases, a random propagation time is sufficient to explain changes induced by the medium. In this paper we study models based on stable probability laws which explain power spectra due to propagation of different kinds of waves in different media, for instance, acoustics in quiet or turbulent atmosphere, ultrasonics in liquids or tissues, or electromagnetic waves in free space or in cables. Physical examples show that a sub-class of probability laws appears in accordance with the causality property of linear filters.
Dynamic Analysis of Collision Between Two Floating Bodies Considering Hydrodynamic Loads

This paper presents a simulation model for coupled simulation of external and internal mechanics of two colliding floating bodies. The model employs a rigid body motion solver, which calculates the hydrostatic restoring, wave radiation forces and solves the 6-DOF motion components in time domain. Rigid body solver is coupled with the structural analysis code Abaqus/Explicit using a user-defined load subroutine. The load subroutine is verified by comparing the benchmark analysis results for heave motion of a sphere. A case study is presented considering a simple box-shaped ship hit by a floating object with a wedge-shaped bow. Simulations are run by considering hydrodynamic loads on the struck ship. The importance of roll restoring and added mass effects are highlighted.
THE STAR FORMATION MASS SEQUENCE OUT TO z = 2.5

We study the star formation rate (SFR)–stellar mass (M⋆) relation in a self-consistent manner from 0 < z < 2.5 with 22,816 star-forming galaxies selected from the NEWFIRM Medium-Band Survey. We find a significant nonlinear slope of the relation, SFR∝M0.6⋆, and a constant observed scatter of 0.34 dex, independent of redshift and M⋆. However, if we select only blue galaxies we find a linear relation SFR∝M⋆, similar to previous results at z = 0 by Peng et al. This selection excludes red, dusty, star-forming galaxies with higher masses, which brings down the slope. By selecting on LIR/LUV (a proxy for dust obscuration) and the rest-frame U − V colors, we show that star-forming galaxies fall in three distinct regions of the log(SFR)–log(M⋆) plane: (1) actively star-forming galaxies with “normal” dust obscuration and associated colors (54% for log (M⋆) > 10 at 1 < z < 1.5), (2) red star-forming galaxies with low levels of dust obscuration and low-specific SFRs (11%), and (3) dusty, blue star-forming galaxies with high-specific SFRs (7%). The remaining 28% comprises quiescent galaxies. Galaxies on the “normal” star formation sequence show strong trends of increasing dust attenuation with stellar mass and a decreasing specific SFR, with an observed scatter of 0.25 dex. The dusty, blue galaxies reside in the upper envelope of the star formation sequence with remarkably similar spectral shapes at all masses, suggesting that the same physical process is dominating the stellar light. The red, low-dust star-forming galaxies may be in the process of shutting off and migrating to the quiescent population.
Jet vetoes for Higgs boson production at future hadron colliders

We study Higgs boson production in exclusive jet bins at possible future 33 and 100 TeV proton-proton colliders. We compare the cross sections obtained using fixed-order perturbation theory with those obtained by also resuming large logarithms induced by the jet-binning in the gluon-fusion and associated production channels. The central values obtained by the best-available fixed-order predictions differ by $10-20\%$ from those obtained after including resummation over the majority of phase-space regions considered. Additionally, including the resummation dramatically reduces the residual scale variation in these regions, often by a factor of two or more. We further show that in several new kinematic regimes that can be explored at these high-energy machines, the inclusion of resummation improvement is mandatory.
Structure formation constraints on Sommerfeld-enhanced dark matter annihilation

We study the growth of cosmic structure in a ΛCDM universe under the assumption that dark matter self-annihilates with an averaged cross section times relative velocity that grows with the scale factor, an increase known as Sommerfeld-enhancement. Such an evolution is expected in models in which a light force carrier in the dark sector enhances the annihilation cross section of dark matter particles, and has been invoked, for instance, to explain anomalies in cosmic ray spectra reported in the past. In order to make our results as general as possible, we assume that dark matter annihilates into a relativistic species that only interacts gravitationally with the standard model. This assumption also allows us to test whether the additional relativistic species mildly favored by cosmic-microwave background data could originate from dark matter annihilation. We do not find evidence for Sommerfeld-enhanced dark matter annihilation and derive the corresponding upper limits on the annihilation cross-section.
NUMERICAL STUDY OF THE VISHNIAC INSTABILITY IN SUPERNOVA REMNANTS

The Vishniac instability is thought to explain the complex structure of radiative supernova remnants in their Pressure-Driven Thin Shell (PDTS) phase after a blast wave (BW) has propagated from a central explosion. In this paper, the propagation of the BW and the evolution of the PDTS stage are studied numerically with the two-dimensional (2D) code HYDRO-MUSCL for a finite-thickness shell expanding in the interstellar medium (ISM). Special attention is paid to the adiabatic index, γ, and three distinct values are taken for the cavity (γ1), the shell (γ2), and the ISM (γ3) with the condition γ2 < γ1, γ3. This low value of γ2 accounts for the high density in the shell achieved by a strong radiative cooling. Once the spherical background flow is obtained, the evolution of a 2D-axisymmetric perturbation is computed from the linear to the nonlinear regime. The overstable mechanism, previously demonstrated theoretically by E. T. Vishniac in 1983, is recovered numerically in the linear stage and is expected to produce and enhance anisotropies and clumps on the shock front, leading to the disruption of the shell in the nonlinear phase. The period of the increasing oscillations and the growth rate of the instability are derived from several points of view (the position of the perturbed shock front, mass fluxes along the shell, and density maps), and the most unstable mode differing from the value given by Vishniac is computed. In addition, the influence of several parameters (the Mach number, amplitude and wavelength of the perturbation, and adiabatic index) is examined and for wavelengths that are large enough compared to the shell thickness, the same conclusion arises: in the late stage of the evolution of the radiative supernova remnant, the instability is dampened and the angular initial deformation of the shock front is smoothed while the mass density becomes uniform with the angle. As a result, our model shows that the supernova remnant returns to a stable evolution and the Vishniac instability does not lead to the fragmentation of the shock as predicted by the theory.