Miracle-dz/UniFAR-FTUs huggingface dataset:
Peran Penyuluh Dalam Keberdayaan Petani Padi Sawah di Desa Belading Kecamatan Sabak Auh Kabupaten Siak

Petani bisa mengoptimalkan hasil pertaniannya dan meningkatkan usahataninya diperlukan peran penyuluh untuk menyampaikan edukasi serta bimbingan pada petani supaya petani bisa menggarap lahan dan menghasilkan hasil pertanian yang optimal sehingga petani bisa sukses dalam usaha taninya. Untuk meningkatkan usaha taninya petani membutuhkan peran penyuluh pertanian. Penyuluh pertanian adalah agen perubahan yg langsung berhubungan dengan petani. Fungsi utama penyuluh mengubah sikap petani melalui pendidikan non formal sehinga petani mempunyai kehidupan yg lebih baik secara berkelanjut, penyuluh melakukan perubahan sikap petani, sehingga mereka dapat memperbaiki cara bercocok tanamnya, lebih beruntung usaha taninya serta lebih layak hidupnya dan menjadi petani yang berdaya. Penelitian ini bertujuan untuk menganalisis pengaruh peran penyuluh terhadap keberdayaan petani. Penelitian ini dilaksanakan di Desa Belading Kecamatan Sabak Auh Kabupaten Siak. Responden dalam penelitian ini adalah petani padi sawah yang bergabung dengan kelompok tani sebanyak 50 sampel. Untuk menjawab tujuan penelitian ini menggunakan analisis regresi linier berganda. Hasil penelitian menunjukkan bahwah peran penyuluh berpengaruh nyata terhadap keberdayaan petani padi sawah di Desa Belading baik secara simultan maupun secara parsial.
A icE-Bs2022KotaKinabalu Social Media and Entrepreneurial Skill Acquisition: Millennials in Malaysia

The advantage of today's millennials is that the amount of information at their fingertips is almost unlimited. They may be particularly capable of looking for opportunities in the new economic environment of the era of epidemics. However, the study on social media's influence on the development of entrepreneurial skills among millennials has received little attention thus far. In addressing this gap, this study explores the influence of social media as perceived entrepreneurial skills learned by millennials. This study also emphasizes social media usage and the consequences of environmental degradation.
Quality of life assessment and its correlation with disease activity in rheumatoid arthritis patients

Background: Rheumatoid arthritis (RA) is a chronic autoimmune disease of unknown etiology that leads to synovial membrane inflammation & destruction of the synovial joints. Quality of life (QoL) is a multidimensional concept that is used to describe the individuals’ perceptions, satisfaction, and evaluation of different areas of their own lives. Objective: to assess the impact of rheumatoid arthritis on the quality of life of the patients & its correlation with disease activity & functional impairment. Materials and methods: The study was carried out on 60 RA patients. All patients were subjected to complete clinical examination & laboratory assessment. Disease activity had been assessed through Disease Activity Score 28 (DAS 28). Functional assessment by HAQ-DI (Health Assessment Questionnaire - Disability Index) was done. Quality of life assessment by: World Health Organization Quality of Life BREF (WHO QoL BREF) and Rheumatoid Arthritis Quality of Life (RAQoL). Sleep quality was assessed by PSQI. Results: There was significant negative correlation between QoL assessed by (WHO QoL BREF) & DAS. There was significant positive correlation between QoL assessed by RAQoL & DAS (P < 0.001), quality of sleep assessed by (PSQI) & DAS.
AN INTEGRAL CONDITION FOR CORE-COLLAPSE SUPERNOVA EXPLOSIONS

We derive an integral condition for core-collapse supernova (CCSN) explosions and use it to construct a new diagnostic of explodability. The fundamental challenge in CCSN theory is to explain how a stalled accretion shock revives to explode a star. In this manuscript, we assume that the shock revival is initiated by the delayed-neutrino mechanism and derive an integral condition for spherically symmetric shock expansion, vs > 0. One of the most useful one-dimensional explosion conditions is the neutrino luminosity and mass-accretion rate ( L ν –  ˙ ) critical curve. Below this curve, steady-state stalled solutions exist, but above this curve, there are no stalled solutions. Burrows & Goshy suggested that the solutions above this curve are dynamic and explosive. In this manuscript, we take one step closer to proving this supposition; we show that all steady solutions above this curve have vs > 0. Assuming that these steady vs > 0 solutions correspond to explosion, we present a new dimensionless integral condition for explosion, Ψ > 0. Ψ roughly describes the balance between pressure and gravity, and we show that this parameter is equivalent to the τ condition used to infer the L ν –  ˙ critical curve. The illuminating difference is that there is a direct relationship between Ψ and vs. Below the critical curve, Ψ may be negative, positive, and zero, which corresponds to receding, expanding, and stalled-shock solutions. At the critical curve, the minimum Ψ solution is zero; above the critical curve, Ψmin > 0, and all steady solutions have vs > 0. Using one-dimensional simulations, we confirm our primary assumptions and verify that Ψmin > 0 is a reliable and accurate explosion diagnostic.
A DEEP X-RAY VIEW OF THE BARE AGN ARK 120. I. REVEALING THE SOFT X-RAY LINE EMISSION

The Seyfert 1 galaxy Ark 120 is a prototype example of the so-called class of bare nucleus active galactic nuclei (AGNs), whereby there is no known evidence for the presence of ionized gas along the direct line of sight. Here deep (>400 ks exposure), high-resolution X-ray spectroscopy of Ark 120 is presented from XMM-Newton observations that were carried out in 2014 March, together with simultaneous Chandra/High Energy Transmission Grating exposures. The high-resolution spectra confirmed the lack of intrinsic absorbing gas associated with Ark 120, with the only X-ray absorption present originating from the interstellar medium (ISM) of our own Galaxy, with a possible slight enhancement of the oxygen abundance required with respect to the expected ISM values in the solar neighborhood. However, the presence of several soft X-ray emission lines are revealed for the first time in the XMM-Newton RGS spectrum, associated with the AGN and arising from the He- and H-like ions of N, O, Ne, and Mg. The He-like line profiles of N, O, and Ne appear velocity broadened, with typical FWHMs of ∼5000 km s−1, whereas the H-like profiles are unresolved. From the clean measurement of the He-like triplets, we deduce that the broad lines arise from a gas of density ne ∼ 1011 cm−3, while the photoionization calculations infer that the emitting gas covers at least 10% of 4π steradian. Thus the broad soft X-ray profiles appear coincident with an X-ray component of the optical–UV broad-line region on sub-parsec scales, whereas the narrow profiles originate on larger parsec scales, perhaps coincident with the AGN narrow-line region. The observations show that Ark 120 is not intrinsically bare and substantial X-ray-emitting gas exists out of our direct line of sight toward this AGN.
GRAVITY WAVES ON HOT EXTRASOLAR PLANETS. I. PROPAGATION AND INTERACTION WITH THE BACKGROUND

We study the effects of gravity waves, or g-modes, on hot extrasolar planets. These planets are expected to possess stably stratified atmospheres, which support gravity waves. In this paper, we review the derivation of the equation that governs the linear dynamics of gravity waves and describe its application to a hot extrasolar planet, using HD 209458 b as a generic example. We find that gravity waves can exhibit a wide range of behaviors, even for a single atmospheric profile. The waves can significantly accelerate or decelerate the background mean flow, depending on the difference between the wave phase and mean flow speeds. In addition, the waves can provide significant heating (∼102 to ∼103 K per planetary rotation), especially to the region of the atmosphere above about 10 scale heights from the excitation region. Furthermore, by propagating horizontally, gravity waves provide a mechanism for transporting momentum and heat from the dayside of a tidally locked planet to its nightside. We discuss work that needs to be undertaken to incorporate these effects in current atmosphere models of extrasolar planets.
Large size scatter of passively evolving lensed galaxies at z ~ 2 in CLASH.

In a systematic search over 11 cluster fields from Cluster Lensing And Supernova survey with Hubble (CLASH) we identify ten passively evolving massive galaxies at redshift z~2.We derive the stellar properties of these galaxies using HST WFC3/ACS multiband data, together with Spitzer IRAC observations. We also deduce the optical rest-frame effective radius of these high redshift objects. The derived stellar masses and measured effective radii have been corrected by the lensing magnification factors, which are estimated by simply adopting the spherical NFW model for the foreground cluster lens. The observed near-IR images, obtained by HST WFC3 camera with high spatial resolution and lensed by the foreground clusters, enable us to study the structures of such systems. Nine out of ten galaxies have on average three times smaller effective radius than local ETGs of similar stellar masses, in agreement with previous works at redshift 1.5 < z < 2.5. Combined with literature data for z~2, we find that the mass-normalized effective radius scales with redshift as re/M^0.56 \propto (1 + z)^{-1.13}. We confirm that their size distribution shows a large scatter: from normal size to ~5 times smaller compared to local ETGs with similar stellar masses. The 1-{\sigma} scatter {\sigma}_{logre} of the size distribution is 0.22 and 0.34 at z~1.6 and z~2.1,respectively.The observed large size scatter has to be carefully taken into account in galaxy evolution model predictions.
Factors controlling SOC stability in colluvial soils under contrasting climate and soil weathering conditions

Although agricultural colluvial soils are important storage for soil organic carbon (SOC), the mechanisms underlying colluvial (cumulative soils) SOC stability have received little attention so far. In this study, we aim to understand to what extent the main controls on colluvial SOC stability differ from those observed in non‐colluvial soils. Paired soil profiles (non‐colluvial versus colluvial) were collected from five sites which differ in climate, soil geochemical background and cultivation history. Topsoil (0–10 cm) and subsoil (30–50 cm) were analysed for SOC fractions, mineral composition, potential soil respiration and radiocarbon content. Our analysis showed that for non‐colluvial soils, climate, cultivation history and weathering degree have significant effects on potential soil respiration. In contrast, for colluvial soils, the most influential factor for potential soil respiration was the rate of accretion and this was independent of climatic and geochemical context. Furthermore, accretion rates indirectly affected potential soil respiration by interacting with the degree of weathering of deposited soil. This changed the mineral matrix of colluvial soil settings and thereby may enhance soil mineral‐related SOC stabilisation mechanisms. Together, these results suggest that the dominant controls on SOC stability in colluvial soils differ from those in non‐colluvial soils, and the soil accretion rate is the most important control on colluvial SOC stability in agricultural systems.
SVMs using geometric algebra for 3D computer vision

This paper shows the analysis of support multivector machines using the coordinate-free system of Clifford or geometric algebra. Real-, complex- and quaternion-valued neural networks are simple particular cases of the geometric algebra multidimensional neural networks and that they can be generated using support multivector machines. Particularly, the generation of RBF for neurocomputing in geometric algebra is easier using the SMVM, which allows to find the optimal parameters automatically. The use of SVM in the geometric algebra framework expands its sphere of applicability for multidimensional learning. As illustration we present the estimation of 3D rigid motion and 3D pose of rigid objects using visual information captured by a trinocular head.
A SEMI-EMPIRICAL MASS-LOSS RATE IN SHORT-PERIOD CATACLYSMIC VARIABLES

The mass-loss rate of donor stars in cataclysmic variables (CVs) is of paramount importance in the evolution of short-period CVs. Observed donors are oversized in comparison with those of isolated single stars of the same mass, which is thought to be a consequence of the mass loss. Using the empirical mass–radius relation of CVs and the homologous approximation for changes in effective temperature T2, orbital period P, and luminosity of the donor with the stellar radius, we find the semi-empirical mass-loss rate of CVs as a function of P. The derived is at ∼10−9.5–10−10 M☉ yr−1 and weakly depends on P when P>90 minutes, while it declines very rapidly toward the minimum period when P < 90 minutes, emulating the P–T2 relation. Due to strong deviation from thermal equilibrium caused by the mass loss, the semi-empirical is significantly different from and has a less-pronounced turnaround behavior with P than suggested by previous numerical models. The semi-empirical P– relation is consistent with the angular momentum loss due to gravitational wave emission and strongly suggests that CV secondaries with 0.075 M☉ < M2 < 0.2 M☉ are less than 2 Gyr old. When applied to selected eclipsing CVs, our semi-empirical mass-loss rates are in good agreement with the accretion rates derived from the effective temperatures T1 of white dwarfs, suggesting that can be used to reliably infer T2 from T1. Based on the semi-empirical , SDSS 1501 and 1433 systems that were previously identified as post-bounce CVs have yet to reach the minimal period.
Sviluppo di un metodo per confrontare l'analisi del cammino markerless e l'analisi del cammino marker-based in ambiente acquatico

Nel presente lavoro di tesi si e sviluppato un metodo per il confronto tra l'analisi del cammino markerless e quella marker-based in acqua. A tal fine si sono estratte le coordinate 3D dei centri articolari e degli angoli articolari dell'arto inferiore di un soggetto acquisiti tramite entrambe le tecniche simultaneamente. I risultati ottenuti possono ritenersi soddisfacenti e risaltano i limiti imposti dall’ambiente acquatico
Existence of Positive Solutions for some Dirichlet Problems with an Asymptotically Homogenous Operator

Existence of positive radially symmetric solutions to a Dirichlet problem of the form −div(A(|Du|)Du) = f(u) in Ω u = 0 on ∂Ω is studied by using blow-up techniques. It is proven here that by choosing the functions sA(s) and f(s) among a certain class called asymptotically homogeneous, the blow-up method still provides the a-priori bounds for positive solutions. Existence is proved then by using degree theory.
Shaping the galaxy stellar mass function with supernova- and AGN-driven winds

Cosmological hydrodynamical simulations of galaxy formation in representative regions of the Universe typically need to resort to subresolution models to follow some of the feedback processes crucial for galaxy formation. Here, we show that an energy-driven outflow model in which the wind velocity decreases and the wind mass loading increases in low-mass galaxies, as suggested by observations, can produce a good match to the low-mass end of the observed galaxy stellar mass function. The high-mass end can be recovered simultaneously if feedback from active galactic nuclei (AGN) and a correction for diffuse stellar light plausibly missed in observations are included. At the same time, our model is in good agreement with the stellar mass functions at redshifts z=1 and z=2, and with the observed redshift evolution of the cosmic star formation rate density. In addition, it accurately reproduces the observed gas to stellar mass ratios and specific star formation rates of galaxies as a function of their stellar mass. This agreement with a diverse set of data marks significant progress in hydrodynamically modelling the formation of a representative galaxy population. It also suggests that the mass flux in real galactic winds should strongly increase towards low-mass galaxies. Without this assumption, an overproduction of galaxies at the faint-end of the galaxy luminosity function seems inevitable in our models.
THE EVOLUTION OF THE MASS–SIZE RELATION TO z = 3.5 FOR UV-BRIGHT GALAXIES AND SUBMILLIMETER GALAXIES IN THE GOODS-NORTH FIELD

We study the evolution of the size–stellar mass relation for a large spectroscopic sample of galaxies in the GOODS-North field up to z ∼ 3.5. The sizes of the galaxies are measured from Ks-band images (corresponding to rest-frame optical/NIR) from the Subaru 8 m telescope. We reproduce earlier results based on photometric redshifts that the sizes of galaxies at a given mass evolve with redshift. Specifically, we compare sizes of UV-bright galaxies at a range of redshifts: Lyman-break galaxies (LBGs) selected through the U-drop technique (z ∼ 2.5–3.5), BM/BX galaxies at z ∼ 1.5–2.5, and GALEX LBGs at low redshift (z ∼ 0.6–1.5). The median sizes of these UV-bright galaxies evolve as (1 + z)−1.11±0.13 between z ∼ 0.5and3.5. The UV-bright galaxies are significantly larger than quiescent galaxies at the same mass and redshift by 0.45 ± 0.09 dex. We also verify the correlation between color and stellar mass density of galaxies to high redshifts. The sizes of submillimeter galaxies in the same field are measured and compared with BM/BX galaxies. We find that the median half-light radius of SMGs is 2.90 ± 0.45 kpc, and there is little difference in their size distribution to the UV-bright star-forming galaxies.
Phenomenological theory of phase transitions in epitaxial Ba x Sr 1 − x TiO 3 thin films

A phenomenological thermodynamic theory of ${\text{Ba}}_{x}{\text{Sr}}_{1\ensuremath{-}x}{\text{TiO}}_{3}$ $(\text{BST-}x)$ thin films epitaxially grown on cubic substrates is developed using the Landau-Devonshire approach. The eighth-order thermodynamic potential for ${\text{BaTiO}}_{3}$ (BT) single crystal and modified fourth-order potential for ${\text{SrTiO}}_{3}$ single crystal were used as starting potentials for the end members of the solid solution with the aim to develop potential of $\text{BST-}x$ solid solution valid at high temperatures. Several coefficients of these potentials for BT were changed to obtain reasonable agreement between theory and experimental phase diagram for $\text{BST-}x$ $(xg0.2)$ solid solutions. For low Ba content we constructed the specific phase diagram where five phases converge at the multiphase point (${T}_{N2}=48\text{ }\text{K}$, $x=0.029$) and all transitions are of the second order. The ``concentration-misfit strain'' phase diagrams for $\text{BST-}x$ thin films at room temperature and ``temperature-misfit strain'' phase diagrams for particular concentrations are constructed and discussed. Near ${T}_{N2}$ coupling between polarization and structural order parameter in the epitaxial film is modified considerably and large number of new phases not present in the bulk materials appear on the phase diagram.
Psychological Empowerment and Employee Creativity in Vietnam Telecommunication Enterprises: The Mediating Role of Intrinsic Work Motivation

Employee creativity contributes to increasing the competitiveness of enterprises, especially enterprises with high requirements for innovation such as telecommunication enterprises. This study focuses on understanding the relationship among psychological empowerment, intrinsic work motivation, and employee creativity. By simultaneously using the qualitative method through in-depth interviews and the quantitative method with a large-scale survey of 420 employees of telecommunications businesses, the research results show that psychological empowerment has a significant relationship with intrinsic work motivation and employee creativity, and intrinsic work motivation has a positive effect on employee creativity, at the same time, intrinsic work motivation plays a mediating role in the relationship between psychological empowerment and employee creativity. Based on research results, the author makes implications for managers including focusing on employee empowerment mentality and promoting intrinsic work motivation to enhance employee creativity in Vietnam telecommunication enterprises.
The pulsating hot subdwarf Balloon 090100001: results of the 2005 multisite campaign

We present the results of a multisite photometric campaign on the pulsating B-type hot subdwarf star Balloon090100001 (Bal09). The star is one of the two known hybrid hot subdwarfs with both long- and short-period oscillations, theoretically attributed to g and p modes. The campaign involved eight telescopes with three obtaining UBVR data, four B-band data and one Stromgren uvby photometry. The campaign covered 48 nights, providing a temporal resolution of 0. 36μHz with a detection threshold of about 0.2mmag in B-filter data. Bal09 has the richest pulsation spectrum of any known pulsating subdwarf B star, and our analysis detected 114 frequencies including 97 independent and 17 combination ones. Most of the 24 g-mode frequencies are between 0.1 and 0.4mHz. Of the remaining 73, presumably p modes, 72 group into four distinct regions near 2.8, 3.8, 4.7 and 5.5mHz. The density of frequencies requires that some modes must have degrees l larger than 2. The modes in the 2.8 mHz region have the largest amplitudes. The strongest mode (f1) is most likely radial, while the remaining ones in this region form two nearly symmetric multiplets: a triplet and quintuplet, attributed to rotationally split l = 1 and 2 modes, respectively. We find clear increases of splitting in both multiplets between the 2004 and 2005 observing campaigns, amounting to ~15 per cent on average. The observed splittings imply that the rotational rate in Bal09 depends on stellar latitude and is the fastest on the equator. We also speculate on the possible reasons for the changes of splitting. The only plausible explanation we find is torsional oscillation. This hypothesis, however, needs to be verified in the future by detailed modelling. In this context, it is very important to monitor the splittings on a longer time-scale as their behaviour may help to explain this interesting phenomenon. The amplitudes of almost all terms detected in both 2004 and 2005 were found to vary. This is evident even during one season; for example, amplitudes of modes f8 and fC were found to change by a factor of 2-3 within about 50 d during 2005. We use a small grid of models to constrain the main mode (f1), which most likely represents the radial fundamental pulsation. The groups of p-mode frequencies appear to lie in the vicinity of the consecutive radial overtones, up to the third one. Despite the large number of g-mode frequencies observed, we failed to identify them, most likely because of the disruption of asymptotic behaviour by mode trapping. The observed frequencies were not, however, fully exploited in terms of seismic analysis which should be done in the future with a larger grid of reliable evolutionary models of hot subdwarfs.