Miracle-dz/UniFAR-FTUs huggingface dataset:
Post-1-Newtonian equations of motion for systems of arbitrarily structured bodies

We give a surface-integral derivation of post-1-Newtonian translational equations of motion for a system of arbitrarily structured bodies, including the coupling to all the bodies' mass and current multipole moments. The derivation requires only that the post-1-Newtonian vacuum field equations are satisfied in weak field regions between the bodies; the bodies' internal gravity can be arbitrarily strong. In particular, black holes are not excluded. The derivation extends previous results due to Damour, Soffel, and Xu (DSX) for weakly self-gravitating bodies in which the post-1-Newtonian field equations are satisfied everywhere. The derivation consists of a number of steps: (i) The definition of each body's current and mass multipole moments and center-of-mass world line in terms of the behavior of the metric in a weak field region surrounding the body. (ii) The definition for each body of a set of gravitoelectric and gravitomagnetic tidal moments that act on that body, again in terms of the behavior of the metric in a weak field region surrounding the body. For the special case of weakly self-gravitating bodies, our definitions of these multipole and tidal moments agree with definitions given previously by DSX. (iii) The derivation of a formula, for any given body, of themore » second time derivative of its mass dipole moment in terms of its other multipole and tidal moments and their time derivatives. This formula was obtained previously by DSX for weakly self-gravitating bodies. (iv) A derivation of the relation between the tidal moments acting on each body and the multipole moments and center-of-mass world lines of all the other bodies. A formalism to compute this relation was developed by DSX; we simplify their formalism and compute the relation explicitly. (v) The deduction from the previous steps of the explicit translational equations of motion, whose form has not been previously derived. « less
The Role of Campus Food Pantries in the Food Security Safety Net: On-Going or Emergency Use at a Midwest Campus Pantry

Food pantries are an integral part of the food security safety net and were designed to distribute emergency food to alleviate short-term hunger. Given many rely on assistance long-term, food pantries may no longer meet the nutritional needs of the typical food pantry user. Less is known about the extent college students use campus food pantries and whether they seek ongoing food support. A comprehensive analysis of food pantry use, including reach, awareness, and student satisfaction was conducted using a cross-sectional campus survey, a student satisfaction survey, and observational data from pantry logs collected from August 2020 to May 2022. During the first year of operation, 20.6% of students were aware of the pantry, 3.1% of students were reached, and student satisfaction was high. About half of users visited once, while 15.4% visited 8 or more times during an academic year. On average, students that visited more had a larger span of use (6.5 months), visited more frequently (2 weeks between visits), and were more likely to be graduate students and older. While most students used the pantry in the short-term, chronic use of the pantry increased from year 1 to year 2. This suggests need may be growing and additional policies or programs are warranted to support students with chronic food needs.
Oscillatory nonlinear electron flow in a Pierce diode

Uniform density electron beam flow in a one‐dimensional Pierce diode is alternately stable and unstable as the diode width is increased. Each stability transition corresponds to an equilibrium bifurcation involving either a static nonuniform equilibrium or a steady oscillatory configuration. The static equilibria, although nonlinear, are evaluated analytically and their stability properties derived. Details of the oscillatory solutions are determined numerically from integral equations relating the transit time of electrons in the diode to the electric field at the entrance plane. As the diode width is reduced, each oscillatory solution undergoes a sequence of subharmonic bifurcations, culminating in a chaotic strange attractor. The chaotic attractor itself terminates in a crisis after a further reduction of the diode width. Unlike other electron beam nonlinear oscillations (e.g., virtual cathodes), no particle reflections are required. This behavior has intrinsic interest as a possible model for beam turbulence in more complex geometries. In addition, it may find application in microwave generation.
Stochastic Models of Transport Flows

The aim of this article is to obtain ergodicity conditions for the traffic models with one or two consecutive traffic lights. The cars arrival is described by Poisson processes. The traffic lights interswitching times have an arbitrary distribution. The optimization of traffic lights performance is also considered. Existence of steady state for the model with two consecutive traffic lights is established taking into account the cars size.
General Classes of Influence Measures for Multivariate Regression

Abstract Many of the existing measures for influential subsets in univariate ordinary least squares (OLS) regression analysis have natural extensions to the multivariate regression setting. Such measures may be characterized by functions of the submatrices H I of the hat matrix H, where I is an index set of deleted cases, and Q I , the submatrix of Q = E(E T E)−1 E T , where E is the matrix of ordinary residuals. Two classes of measures are considered: f(·)tr[H I Q I (I − H I − Q I ) a (I − H I ) b ] and f(·)det[(I − H I − Q I ) a (I − H I ) b ], where f is a scalar function of the dimensions of matrices and a and b are integers. These characterizations motivate us to consider separable leverage and residual components for multiple-case influence and are shown to have advantages in computing influence measures for subsets. In the recent statistical literature on regression analysis, much attention has been given to problems of detecting observations that, individually or jointly, exert a disproportionate .
New Boundary Element Analysis Of AcousticProblems With The Fictitious Eigenvalue Issue

This paper is concerned with a new approach for avoiding the fictitious eigenfrequency problem to boundary element analysis of three-dimensional acoustic problems governed by Helmholtz equation. It is well known that in solving without any care the external acoustic problem which includes internal sub-domains by means of the boundary integral equation, the solution is disturbed at fictitious eigenfrequencies corresponding to the internal sub-domains. The present paper proposes a new boundary element analysis to circumvent such the fictitious eigenfrequency problem, which is an alternative boundary integral equation approach to the Burton-Miller one. The present approach is implemented, and its validity and effectiveness are demonstrated through numerical computation of typical examples.
Interaction of Bubbles with Vortex Ring Launched into Bubble Plume

This study is concerned with an experimental exploration for the interactions of bubbles with a vortex ring launched vertically upward into a bubble plume. A vortex ring launcher, composed of a cylinder and a piston, is mounted at the bottom of a water tank. Small hydrogen bubbles are released into still water from a cathode, which is wound around the cylinder outlet, by the electrolysis of water. The bubbles rise by the buoyant force and induce a bubble plume. The water in the cylinder is discharged into the bubble plume by the piston, resulting in a laminar vortex ring convecting along the central axis of the plume. Just after the launch of the vortex ring, the bubbles are spirally entrained into the vortex ring with the roll up of the shear layer. The void fraction within the vortex ring increases with the convection of the vortex ring until a certain displacement of the vortex ring, where the reduction occurs. The vortex ring convects with a constant velocity higher than that in still water. The entrained bubbles reduce the strength of the vortex ring.
The impact of eco-innovation, ecotourism policy and social media on sustainable tourism development: evidence from the tourism sector of Indonesia

Tourism growth is a significant factor in the economic development around the globe, and eco-innovation and tourism policies could improve the tourism development and needs the researchers ’ attention. Thus, the present article investigates the impact of eco-product innovation, eco-process innovation, eco-organizational innovation, eco-tourism policies, and social media on sustainable tourism development in Indonesia. This article has used primary data collection methods like questionnaires to collect the data from the selected respondents. The research also applied the smart-PLS to check the association among variables and test the hypotheses. The results revealed that eco-product innovation, eco-process innovation, eco-organizational innovation, eco-tourism policies, and social media have a positive nexus with sustainable tourism growth in Indonesia. This shows that through social media, the tourism firms keep in contact with the stakeholders, can have information, and share their own ideas with them. In this way, they can keep their tourism practice innovative and according to the requirements of stakeholders. This article guides the regulators to develop effective policies that improve sustainable tourism growth using eco-innovation and eco-tourism policies.
Turnaround radius in f(R) model

We investigate the turnaround radius in the spherical collapse model, both in General Relativity and in modified gravity, in particular f(R) scenarios. The phases of spherical collapse are marked by the non-linear density contrast in the instant of turnaround δt, and by the linear density contrast in the moment of collapse, δc. We find that the effective mass of the extra scalar degree of freedom which arises in modified gravity models has an impact on δt of up to ∼16%, and that δc can increase by ∼2.3%, for structures with mass of ≃ 1013 h−1 M⊙ at z≃ 0. We also compute the turnaround radius, Rt, which in modified gravity models can increase by up to ∼ 6%.
On the use of the Kodama vector field in spherically symmetric dynamical problems

It is shown that by making use of the Kodama vector field, as a preferred time evolution vector field, in spherically symmetric dynamical systems unexpected simplifications arise. In particular, the evolution equations relevant for the case of a massless scalar field minimally coupled to gravity are investigated. The simplest form of these equations in the ‘canonical gauge’ is known to possess the character of a mixed first-order elliptic–hyperbolic system. The advantages related to the use of the Kodama vector field are twofold although they show up simultaneously. First, it is found that the true degrees of freedom separate. Second, a subset of the field equations possessing the form of a first-order symmetric hyperbolic system for these preferred degrees of freedom is singled out. It is also demonstrated, in the appendix, that the above results generalize straightforwardly to the case of a generic self-interacting scalar field.
An exact integral equation for solitary waves (with new numerical results for some ‘internal’ properties)

A novel exact within potential flow integral equation for the solitary wave profile, ns(x), is presented and numerically solved utilizing a parametric form for the profile and ‘tailored quadrature’ methods. We believe the profiles and properties of such waves, so obtained, to be the most accurate (to date). From the profiles, certain internal properties of interest, such as the shapes and properties of internal streamlines, internal velocities and pressures, that appear to be hitherto unevaluated in the literature, are here presented. In the outskirts, it is shown that the Stokes form for the exponential decay, ns(x) ~ e-μx/h, of the surface profile is also valid for all streamlines. The amplitude of this exponential decay is numerically obtained for all solitary wave surface profiles. The analagous decay amplitude of an internal streamline is shown to be related to the surface profile amplitude via a simple quadrature. Like several other properties of solitary waves, it is found that the surface profile outskirts decay amplitude, as well as the pressure on the canal bed directly underneath the crest, are largest for waves of lesser height than the ‘maximum’ wave.
Rise of the first supermassive stars

We use high resolution adaptive mesh refinement simulations to model the formation of massive metal-free stars in the early Universe. By applying Lyman-Werner (LW) backgrounds of 100 J$_{21}$ and 1000 J$_{21}$ respectively we construct environments conducive to the formation of massive stars. We find that only in the case of the higher LW backgrounds are super-critical accretion rates realised that are necessary for super-massive star (SMS) formation. Mild fragmentation is observed for both backgrounds. Violent dynamical interactions between the stars that form in the more massive halo formed (1000 J$_{21}$ background) results in the eventual expulsion of the two most massive stars from the halo. In the smaller mass halo (100 J$_{21}$ background) mergers of stars occur before any multibody interactions and a single massive Pop III star is left at the centre of the halo at the end of our simulation. Feedback from the very massive Pop III stars is not effective in generating a large HII region with ionising photons absorbed within a few thousand AU of the star. In all cases a massive black hole seed is the expected final fate of the most massive objects. The seed of the massive Pop III star which remained at the centre of the less massive halo experiences steady accretion rates of almost $10^{-2}$ M$_{\odot}$/yr and if these rates continue could potentially experience super-Eddington accretion rates in the immediate aftermath of collapsing into a black hole.
Brachiaria humidicola Cultivation Enhances Soil Nitrous Oxide Emissions from Tropical Grassland by Promoting the Denitrification Potential: A 15N Tracing Study

Biological nitrification inhibition (BNI) in the tropical grass Brachiaria humidicola could reduce net nitrification rates and nitrous oxide (N2O) emissions in soil. To determine the effect on gross nitrogen (N) transformation processes and N2O emissions, an incubation experiment was carried out using 15N tracing of soil samples collected following 2 years of cultivation with high-BNI Brachiaria and native non-BNI grass Eremochloa ophiuroide. Brachiaria enhanced the soil ammonium (NH4+) supply by increasing gross mineralization of recalcitrant organic N and the net release of soil-adsorbed NH4+, while reducing the NH4+ immobilization rate. Compared with Eremochloa, Brachiaria decreased soil gross nitrification by 37.5% and N2O production via autotrophic nitrification by 14.7%. In contrast, Brachiaria cultivation significantly increased soil N2O emissions from 90.42 μg N2O-N kg−1 under Eremochloa cultivation to 144.31 μg N2O-N kg−1 during the 16-day incubation (p < 0.05). This was primarily due to a 59.6% increase in N2O production during denitrification via enhanced soil organic C, notably labile organic C, which exceeded the mitigated N2O production rate during nitrification. The contribution of denitrification to emitted N2O also increased from 9.7% under Eremochloa cultivation to 47.1% in the Brachiaria soil. These findings confirmed that Brachiaria reduces soil gross nitrification and N2O production via autotrophic nitrification while efficiently stimulating denitrification, thereby increasing soil N2O emissions.
Broad-line Type Ic supernova SN 2014ad

We present optical and ultraviolet photometry, and low resolution optical spectroscopy of the broad-line type Ic supernova SN 2014ad in the galaxy PGC 37625 (Mrk 1309), covering the evolution of the supernova during $-$5 to +87 d with respect to the date of maximum in $B$-band. A late phase spectrum obtained at +340 d is also presented. With an absolute $V$ band magnitude at peak of $M_{V}$ = $-$18.86 $\pm$ 0.23 mag, SN 2014ad is fainter than Gamma Ray Burst (GRB) associated supernovae, and brighter than most of the normal and broad-line type Ic supernovae without an associated GRB. The spectral evolution indicates the expansion velocity of the ejecta, as measured using the Si\,{\sc ii} line, to be as high as $\sim$ 33500 km\,s$^{-1}$ around maximum, while during the post-maximum phase it settles down at $\sim$ 15000 km\,s$^{-1}$. The expansion velocity of SN 2014ad is higher than all other well observed broad-line type Ic supernovae except the GRB associated SN 2010bh. The explosion parameters, determined by applying the Arnett's analytical light curve model to the observed bolometric light curve, indicate that it was an energetic explosion with a kinetic energy of $\sim$ (1 $\pm$ 0.3)$\times$10$^{52}$ ergs, a total ejected mass of $\sim$ (3.3 $\pm$ 0.8) M$_\odot$, and $\sim$ 0.24 M$_\odot$ of $^{56}$Ni was synthesized in the explosion. The metallicity of the host galaxy near the supernova region is estimated to be $\sim$ 0.5 Z$_\odot$.
Pathways of care and attitudes toward psychotropics in patients with depressive disorders and psychotic disorders

Objectives: Delay in institution of appropriate mental healthcare is closely linked with attitudes, stigma, and availability of services, which further directs the help seeking pathways. This study was aimed to assess the pathway of care and attitudes toward psychotropic medications among patients with depressive disorder and psychotic disorders. Materials and Methods: Eighty outpatients with depressive disorder and 40 patients with psychotic disorder were assessed in a tertiary care center for pathways to care and attitude toward psychotropics through Attitude toward Psychotropic Medications Questionnaire and Drug attitude inventory-10. Results: The psychiatrist remained the most common first treatment contact (46% in depression and 62% in psychosis). Greater number of patients in psychotic disorder group had first treatment contact with faith healers or exorcist (17.5%), compared to depressive disorder (6.2%). Patients in depressive group had more favorable attitude toward psychotropics compared to psychosis group. Majority of patients had favorable attitude toward psychotropic medications, but they also had substantial misconceptions about side effects, utility, and need of taking lesser than prescribed doses. Conclusions: Although majority of patients had favorable attitude, they also had substantial misconceptions about medications. These issues need to be addressed for better delivery of comprehensive mental healthcare.
On Extending the Mass-Metallicity Relation of Galaxies by 2.5 Decades in Stellar Mass

We report 4.5 μm luminosities for 27 nearby (D ≲ 5 Mpc) dwarf irregular galaxies measured with the Spitzer Infrared Array Camera. We have constructed the 4.5 μm luminosity-metallicity (L-Z) relation for 25 dwarf galaxies with secure distance and interstellar medium oxygen abundance measurements. The 4.5 μm L-Z relation is 12 + log(O/H) = (5.78 ± 0.21) + (-0.122 ± 0.012)M[4.5], where M[4.5] is the absolute magnitude at 4.5 μm. The dispersion in the near-infrared L-Z relation is smaller than the corresponding dispersion in the optical L-Z relation. The subsequently derived stellar mass-metallicity (M*-Z) relation is 12 + log(O/H) = (5.65 ± 0.23) + (0.298 ± 0.030) log M*, and extends the SDSS M*- Z relation to lower mass by about 2.5 dex. We find that the dispersion in the M*-Z relation is similar over 5 orders of magnitude in stellar mass, and that the relationship between stellar mass and interstellar medium metallicity is similarly tight from high-mass to low-mass systems. We find a larger scatter at low mass in the relation between effective yield and total baryonic mass. In fact, there are a few dwarf galaxies with large yields, which is difficult to explain if galactic winds are ubiquitous in dwarf galaxies. The low scatter in the L-Z and M*-Z relationships are difficult to understand if galactic superwinds or blowout are responsible for the low metallicities at low mass or luminosity. Naively, one would expect an ever increasing scatter at lower masses, which is not observed.
Strong Spatial Clustering of Ultraviolet-selected Galaxies with Magnitude Ks < 20.5 and Redshift z ~ 2

We obtained deep 8. ′5 × 8. ′5 near-infrared (IR) images within four high-redshift survey fields, measured the Ks magnitudes of 300 optically selected galaxies with spectroscopic redshift 1.8 ≲ z ≲ 2.6, and compared the spatial clustering strength of galaxies with Ks < 20.5 and Ks > 20.5. We found at greater than 95% confidence that the brighter galaxies cluster more strongly. The best-fit correlation lengths for the bright and faint samples are 10 ± 3 and 4 ± 0.8 h-1 comoving Mpc, respectively (1 σ), although the unusual density of bright QSOs in one of our survey fields may imply that the result is not representative of the universe as a whole. Neglecting this possibility, the correlation length for the optically selected sample with Ks < 20.5 agrees well with that reported for comparably bright near-IR-selected samples. The differences in correlation length between optically selected and near-IR-selected samples have been presented as evidence that the two techniques find orthogonal populations of high-redshift galaxies. Our results favor a more nuanced view.
Density distribution function of a self-gravitating isothermal compressible turbulent fluid in the context of molecular clouds ensembles – II. Contribution of the turbulent term and the potential of the outer shells

We have set ourselves the task of obtaining the probability distribution function of the mass density of a self-gravitating isothermal compressible turbulent fluid from its physics. We have done this in the context of a new notion: the molecular clouds ensemble. We have applied a new approach that takes into account the fractal nature of the fluid. Using the medium equations, under the assumption of steady state, we show that the total energy per unit mass is an invariant with respect to the fractal scales. As a next step we obtain a nonlinear integral equation for the dimensionless scale Q which is the third root of the integral of the probability distribution function. It is solved approximately up to the leading-order term in the series expansion. We obtain two solutions. They are power-law distributions with different slopes: the first one is -1.5 at low densities, corresponding to a equilibrium between all energies at a given scale, and the second one is -2 at high densities, corresponding to a free fall at small scales.