Miracle-dz/UniFAR-FTUs huggingface dataset:
Role of carbon nanotube diameter on thermal interfacial resistance through the analysis of vibrational mismatch: A Molecular Dynamics approach

Carbon nanotube (CNT) have been known to increase the heat transfer at the solid-liquid interfaces, but have a limitation due to the interfacial thermal resistance. Vibrational mismatch at the interface leads to this interfacial thermal resistance, which plays an important role in energy transfer at the boundary. Negligible work has been reported on the influence of CNT diameter on the resistance through the vibrational mismatch study. Molecular dynamics simulations have been performed to investigate the effect of CNT diameter on interfacial resistance between carbon nanotube (CNT) and water molecules. This work is an effort to understand the heat transfer phenomenon at the interface by quantifying the vibrational mismatch. Analysis of the vibrational spectra of CNT and water molecules is done to study the effect of CNT diameter on interfacial resistance. Starting with the initial configuration, and equilibrating the system of CNT and water molecules at 300 K and 1 atm, the CNT temperature is raised to 700 K by velocity rescaling. This system is now allowed to relax as a micro-canonical ensemble. Based on the lumped capacitance analysis, the time constant of the CNT temperature response is determined, which is then used to compute the interfacial thermal resistance. The interfacial thermal resistance is observed to be relatively higher for the larger diameter nanotube. This is attributed to the higher vibrational mismatch existing for larger diameter CNT as a result of low overlapping region between vibrational density states of CNT and water molecules. For smaller diameter CNT, the interfacial thermal resistance is low which results in the efficient heat transfer at the interface thus, emphasizing the indispensable role of larger diameter CNTs in the cooling applications.
Enhancement in Frequency Response Capability of Grid Connected Photovoltaic System

Due to various serious environmental concerns, it is strongly recommended to produce electricity using large-scale photovoltaic (PV) plants. However, such PV sources must provide frequency support similar to conventional synchronous generators. In this paper, frequency regulation is enabled through deloaded PV. Deloaded PV keeps part of its available power as reserve which can be utilized during frequency disturbances. In order to deal with varying operating conditions such as load/solar insolation change and to utilize PV units with different ratings, a fuzzy-based adaptive deloading control is proposed in this work. It is established that proposed fuzzy-based scheme reduce the oscillations and overshoot in frequency response during the dynamic operating conditions. Moreover, the proposed control enables the PV units to operate as dispatchable sources similar to conventional generators. The extensive simulation results are presented in support of the proposed controller.
STRUCTURE AND DYNAMICS OF MODEL SYSTEMS: FROM FERROFLUIDS TO BRAIN MEMBRANES

Soft condensed matter systems are a very diverse and challenging subject to study. To understand the complex macro-properties of such systems one approach is to characterize the microscopic structure and dynamics. A powerful technique for determining micro and nanoscale properties is scattering of radiation sources. Light, electron and neutron scattering techniques provide insight into the complicated molecular structures and the processes happening on these small scales. We have used neutron and x-ray scattering techniques to determine structural and dynamical information from two different types of soft condensed matter systems. The microscopic nature of a cobalt magnetic fluid was studied using neutron scattering, and the structure and dynamics of molecules within lipid bilayers was studied with the use of both neutron and x-ray scattering. Under strong magnetic fields, our cobalt fluid’s small magnetic particles formed short chains, which we observed using neutron scattering. In the lipid bilayer systems which were studied we determined the positional orientation of cholesterol, Aspirin, and ethanol molecules, observed the effect of temperature on some of these systems, characterized domains and dynamics, and recreated the molecular structures of Alzheimer’s protein in a brain-like membrane.
Feedback and the structure of simulated galaxies at redshift z=2

We study the properties of simulated high-redshift galaxies using cosmological N-body/gasdynamical runs from the OverWhelmingly Large Simulations (OWLS) project. The runs contrast several feedback implementations of varying effectiveness: from no feedback, to supernova-driven winds to powerful active galactic nucleus (AGN)-driven outflows. These different feedback models result in large variations in the abundance and structural properties of bright galaxies at z = 2. In agreement with earlier work, models with inefficient or no feedback lead to the formation of massive compact galaxies collecting a large fraction (upwards of 50 per cent) of all available baryons in each halo. Increasing the efficiency of feedback reduces the baryonic mass and increases the size of simulated galaxies. A model that includes supernova-driven gas outflows aided by the energetic output of AGNs reduces galaxy masses by roughly a factor of similar to 10 compared with the no-feedback case. Other models give results that straddle these two extremes. Despite the large differences in galaxy formation efficiency, the net specific angular momentum of a galaxy is, on average, roughly half that of its surrounding halo, independent of halo mass (in the range probed) and of the feedback scheme. Feedback thus affects the baryonic mass of a galaxy much more severely than its spin. Feedback induces strong correlations between angular momentum content and galaxy mass that leave their imprint on galaxy scaling relations and morphologies. Encouragingly, we find that galaxy discs are common in moderate-feedback runs, making up typically similar to 50 per cent of all galaxies at the centres of haloes with virial mass exceeding similar to 1011 M-circle dot. The size, stellar masses and circular speeds of simulated galaxies formed in such runs have properties in between those of large star-forming discs and of compact early-type galaxies at z = 2. Once the detailed abundance and structural properties of these rare objects are well established, it may be possible to use them to gauge the overall efficacy of feedback in the formation of high-redshift galaxies.
Fundamentals of Texture Mapping and Image Warping

The applications of texture mapping in computer graphics and image distortion (warping) in image processing share a core of fundamental techniques. We explore two of these techniques, the two-dimensional geometric mappings that arise in the parameterization and projection of textures onto surfaces, and the filters necessary to eliminate aliasing when an image is resampled during texture mapping or warping. With respect to mappings, this work presents a tutorial on three common classes of mapping: the affine, bilinear, and projective. For resampling, this work develops a new theory describing the ideal, space variant intialiazing filter for signals warped and resampled according to an arbitrary mapping. Efficient implementations of the mapping and filtering techniques are discussed and demonstrated.
Measuring Determination of Factors Affecting Firm Value in Agricultural Sector Companies in Indonesia

The purpose of this study is to use a panel data model to examine the factors that impact firm value in agriculture sector enterprises in Indonesia. Management initiatives such as earnings management, tax evasion, and debt strategy all influence business value. According to the findings of this study, all variables studied (earnings management, tax evasion, and debt policy) have an impact on business value. All of these variables have a 79.34 percent impact on the company's valuation, with the remaining 20.46 percent impacted by variables outside of the model. Meanwhile, independent studies show that debt and management strategies have little influence and have a negative link with business value. The study's findings may give more information on what elements may be included in measuring business value, which may have implications for investors, particularly those in agriculture sector companies listed on the stock exchange.
Lectures on Representations of Surface Groups

HAL is a multi-disciplinary open access archive for the deposit and dissemination of scientific research documents, whether they are published or not. The documents may come from teaching and research institutions in France or abroad, or from public or private research centers. L’archive ouverte pluridisciplinaire HAL, est destinée au dépôt et à la diffusion de documents scientifiques de niveau recherche, publiés ou non, émanant des établissements d’enseignement et de recherche français ou étrangers, des laboratoires publics ou privés. Copyright Lectures on Representations of Surface Groups François Labourie
THE K2 ECLIPTIC PLANE INPUT CATALOG (EPIC) AND STELLAR CLASSIFICATIONS OF 138,600 TARGETS IN CAMPAIGNS 1–8

The K2 Mission uses the Kepler spacecraft to obtain high-precision photometry over ≈80 day campaigns in the ecliptic plane. The Ecliptic Plane Input Catalog (EPIC) provides coordinates, photometry, and kinematics based on a federation of all-sky catalogs to support target selection and target management for the K2 mission. We describe the construction of the EPIC, as well as modifications and shortcomings of the catalog. Kepler magnitudes (Kp) are shown to be accurate to ≈0.1 mag for the Kepler field, and the EPIC is typically complete to Kp ≈ 17 (Kp ≈ 19 for campaigns covered by Sloan Digital Sky Survey). We furthermore classify 138,600 targets in Campaigns 1–8 (≈88% of the full target sample) using colors, proper motions, spectroscopy, parallaxes, and galactic population synthesis models, with typical uncertainties for G-type stars of ≈3% in , ≈0.3 dex in , ≈40% in radius, ≈10% in mass, and ≈40% in distance. Our results show that stars targeted by K2 are dominated by K–M dwarfs (≈41% of all selected targets), F–G dwarfs (≈36%), and K giants (≈21%), consistent with key K2 science programs to search for transiting exoplanets and galactic archeology studies using oscillating red giants. However, we find significant variation of the fraction of cool dwarfs with galactic latitude, indicating a target selection bias due to interstellar reddening and increased contamination by giant stars near the galactic plane. We discuss possible systematic errors in the derived stellar properties, and differences with published classifications for K2 exoplanet host stars. The EPIC is hosted at the Mikulski Archive for Space Telescopes (MAST): http://archive.stsci. edu/k2/epic/search.php.
The end of star formation in Chamaeleon I? A LABOCA census of starless and protostellar cores

Chamaeleon I is the most active region in terms of star formation in the Chamaeleon molecular cloud complex. Its population of prestellar and protostellar cores is not known and a controversy exists concerning its history of star formation. Our goal is to characterize the earliest stages of star formation in this cloud. We used the bolometer array LABOCA at APEX to map the cloud in dust continuum emission at 870 micron. The detected sources are analysed by carefully taking into account the spatial filtering inherent in the data reduction process. A search for associations with YSOs is performed using Spitzer data and the SIMBAD database. Most of the detected 870 micron emission is distributed in 5 filaments. We identify 59 starless cores, one candidate first hydrostatic core, and 21 sources associated with more evolved YSOs. The starless cores are only found above a visual extinction threshold of 5 mag. They are less dense than those detected in other nearby molecular clouds by a factor of a few on average. The core mass distribution is consistent with the IMF at the high-mass end but is overpopulated at the low-mass end. In addition, at most 17% of the cores have a mass larger than the critical Bonnor-Ebert mass. Both results suggest that a large fraction of the starless cores may not be prestellar. Based on the census of prestellar cores, Class 0 protostars, and more evolved YSOs, we conclude that the star formation rate has decreased with time in this cloud. The low fraction of candidate prestellar cores among the population of starless cores, the small number of Class 0 protostars, the high global star formation efficiency, the decrease of the star formation rate with time, and the low mass per unit length of the detected filaments all suggest that we may be witnessing the end of the star formation process in Cha I {abridged}.
THE RADIO JET INTERACTION IN NGC 5929: DIRECT DETECTION OF SHOCKED GAS

We report on the discovery of kinematic shock signatures associated with a localized radio jet interaction in the merging Seyfert galaxy NGC 5929. We explore the velocity-dependent ionization structure of the gas and find that low-ionization gas at the interaction site is significantly more disturbed than high-ionization gas, which we attribute to a local enhancement of shock ionization due to the influence of the jet. The characteristic width of the broad low-ionization emission is consistent with shock velocities predicted from the ionization conditions of the gas. We interpret the relative prominence of shocks to the high density of gas in the nuclear environment of the galaxy and place some constraints of their importance as feedback mechanisms in Seyferts.
NEW TESTS FOR DISRUPTION MECHANISMS OF STAR CLUSTERS: THE LARGE AND SMALL MAGELLANIC CLOUDS

We compare the observed bivariate distribution of masses (M) and ages (τ) of star clusters in the Large Magellanic Cloud (LMC) with the predicted distributions g(M, τ) from three idealized models for the disruption of star clusters: (1) sudden mass-dependent disruption, (2) gradual mass-dependent disruption, and (3) gradual mass-independent disruption. The model with mass-independent disruption provides a good, first-order description of these cluster populations, with g(M, τ) ∝ Mβτγ, β = −1.8 ± 0.2 and γ = −0.8 ± 0.2, at least for clusters with ages τ ≲ 109 yr and masses M ≳ 103M☉ (more specifically, τ ≲ 107(M/102M☉)1.3 yr). This model predicts that the clusters should have a power-law luminosity function, dN/dL ∝ L−1.8, in agreement with observations. The first two models, on the other hand, fare poorly when describing the observations, refuting previous claims that mass-dependent disruption of star clusters is observed in the LMC over the studied M–τ domain. Clusters in the SMC can be described by the same g(M, τ) distribution as for the LMC, but with smaller samples and hence larger uncertainties. The successful g(M, τ) model for clusters in the Magellanic Clouds is virtually the same as the one for clusters in the merging Antennae galaxies, but extends the domain of validity to lower masses and to older ages. This indicates that the dominant disruption processes are similar in these very different galaxies over at least τ ≲ 108 yr and possibly τ ≲ 109 yr. The mass functions for young clusters in the LMC are power laws, while that for ancient globular clusters is peaked. We show that the observed shapes of these mass functions are consistent with expectations from the simple evaporation model presented by McLaughlin & Fall.
Bio-efficacy of Unmanned Aerial Vehicle based spraying to manage pests

An agricultural spraying system for UAV platform was developed at the Department of Farm Machinery and Power Engineering, Punjab Agricultural University, Ludhiana during 2019 to spray pesticides in cotton, rice and moong crops for the control of pests. The developed aerial spraying system was operated at three flying speeds, i.e. S1 (2.0 m/s), S2 (3.0 m/s) and S3 (4.0 m/s) and at three flying heights, i.e. H1 (0.50 m), H2 (0.75 m) and H3 (1.0 m). Whitefly and brown plant hopper (BPH) were the targeted pest and its bio-efficacy data were collected after spray application. Results indicated that flying height and forward speed had significant effect on bio-efficacy in all the three crops. In cotton, whitefly populations varied between 19.00-21.40 per three leaves. The maximum percent, i.e. 84.85% reduction in white fly population was observed at 7 DAS in H1S1 treatment. In rice, BPH population was varied between 6.60-9.47 per hill followed by control 17.20 per hill. Maximum percent reduction in BPH population was observed 67.42% at 7 DAS in H3S1 treatment. In moong, reduction in whitefly population was varied between 4.87-5.80 per plant followed by control (7.00 per plant). After three days of spray, combination of flying heights (H1, H2 and H3) and forward speeds (S1, S2 and S3) were found to be significantly effective in dropping whitefly and BPH population. Increase in flying height and forward speed reduced percentage reduction of pests. Combination of flying heights H1 and H2 and forward speeds S1 and S2 treatments were found significantly effective in controlling pests in all three crops.
Vectorial AdS5/CFT4 duality for spin-one boundary theory

We consider an example of vectorial AdS5/CFT4 duality when the boundary theory is described by free N complex or real Maxwell fields. It is dual to a particular (‘type C’) higher spin theory in AdS5 containing fields in special mixed-symmetry representations. We extend the study of this theory by Beccaria and Tseytlin (2014 Higher spins in AdS 5 ? > at one loop: vacuum energy, boundary conformal anomalies and AdS/CFT arXiv:1410.3273) by deriving the expression for the large N limit of the corresponding singlet-sector partition function on S 1 × S 3 ? > . We find that in both complex U(N) and real O(N) invariant cases the form of the one-particle partition function is as required by the AdS/CFT duality. We also discuss the matching of the Casimir energy on S3 by assuming an integer shift in the bulk theory coupling.
NORMAL GLOBULAR CLUSTER SYSTEMS IN MASSIVE LOW SURFACE BRIGHTNESS GALAXIES

We present the results of a study of the globular cluster systems of six massive spiral galaxies, originally cataloged as low surface brightness (LSB) but here shown to span a wide range of surface brightness values, including two intermediate to LSB galaxies. We used the Advanced Camera for Surveys on-board Hubble Space Telescope to obtain photometry in the F475W and F775W bands and select sources with photometric and morphological properties consistent with those of globular clusters. A total of 206 candidates were identified in our target galaxies. From a direct comparison with the Galactic globular cluster system we derive specific frequency values for each galaxy that are in the expected range for late-type galaxies. We show that the globular cluster candidates in all galaxies have properties consistent with globular cluster systems of previously studied galaxies in terms of luminosity, sizes and color. We establish the presence of globular clusters in the two intermediate to LSB galaxies in our sample and show that their properties do not have any significant deviation from the behavior observed in the other sample galaxies, implying that these properties do not evolve with the surface brightness of the galaxies. Our results are broadly consistent with a scenario in which low surface brightness galaxies follow roughly the same evolutionary history as normal (i.e. high surface) brightness galaxies except at a much lower rate, but require the presence of an initial period of star formation intense enough to allow the formation of massive star clusters.
Comparison of the Properties of a Random Copolymer and a Molten Blend PA6/PA6.9

This study compares the thermal and mechanical properties of two different materials, obtained via two diverse synthetic pathways. The first one is a mixed blend of PA6/PA6.9, while the second is a random copolymer (PA6.9-ran–PA6, obtained via copolymerization of its monomers, i.e., caprolactam, hexamethylenediamine and azelaic acid). Several tests are carried out according to the aforementioned pathways, varying the relative ratio between the two polymeric building blocks. The role of the synthetized plastic is to be coupled to polyamide material, such as PA6, to confer its better properties. The synthetized random copolymer, besides displaying ease of processability with respect to conventional methods, exhibits interesting features. It has a low melting point (135 °C, PA6.9-ran-PA6 50:50) and therefore it might be used as a hot-melt adhesive in composite material. Owing to its low crystallinity content, the material displays a rubber-like behavior and may be employed to confer elastomeric properties to PA6 matrix, in place of non-amidic material (for example elastomeric polyurethanes). This leads to a further advantage in terms of chemical recyclability of the end-of-life material, since the additive increases the percentage of PA6 in waste material and, consequently, the yield of caprolactam recovery.
Non-linear dense core formation in the dark cloud L1517

We present a solution for the observed core fragmentation of filaments in the Taurus L1517 dark cloud which previously could not be explained. Core fragmentation is a vital step for the formation of stars. Observations suggest a connection to the filamentary structure of the cloud gas, but it remains unclear which process is responsible. We show that the gravitational instability process of an infinite, isothermal cylinder can account for the exhibited fragmentation under the assumption that the perturbation grows on the dominant wavelength. We use numerical simulations with the code RAMSES, estimate observed column densities and line-of-sight velocities, and compare them to the observations. A critical factor for the observed fragmentation is that cores grow by redistributing mass within the filament and thus the density between the cores decreases over the fragmentation process. This often leads to wrong dominant wavelength estimates, as it is strongly dependent on the initial central density. We argue that non-linear effects also play an important role in the evolution of the fragmentation. Once the density perturbation grows above the critical line mass, non-linearity leads to an enhancement of the central core density in comparison to the analytical prediction. Choosing the correct initial conditions with perturbation strengths of around 20 per cent leads to inclination-corrected line-of-sight velocities and central core densities within the observational measurement error in a realistic evolution time.
NEON AND CNO ABUNDANCES FOR EXTREME HELIUM STARS—A NON-LTE ANALYSIS

A non-LTE (NLTE) abundance analysis was carried out for three extreme helium stars (EHes): BD+10° 2179, BD−9° 4395, and LS IV+6° 002, from their optical spectra with NLTE model atmospheres. NLTE TLUSTY model atmospheres were computed with H, He, C, N, O, and Ne treated in NLTE. Model atmosphere parameters were chosen from consideration of fits to observed He i line profiles and ionization equilibria of C and N ions. The program SYNSPEC was then used to determine the NLTE abundances for Ne as well as H, He, C, N, and O. LTE neon abundances from Ne i lines in the EHes: LSE 78, V1920 Cyg, HD 124448, and PV Tel, are derived from published models and an estimate of the NLTE correction applied to obtain the NLTE Ne abundance. We show that the derived abundances of these key elements, including Ne, are well matched with semi-quantitative predictions for the EHe resulting from a cold merger (i.e., no nucleosynthesis during the merger) of an He white dwarf with a C–O white dwarf.