Miracle-dz/UniFAR-FTUs huggingface dataset:
THE OUTFLOWS ACCELERATED BY THE MAGNETIC FIELDS AND RADIATION FORCE OF ACCRETION DISKS

The inner region of a luminous accretion disk is radiation-pressure-dominated. We estimate the surface temperature of a radiation-pressure-dominated accretion disk, , which is significantly lower than that of a gas-pressure-dominated disk, Θ ∼ (H/r)2. This means that the outflow can be launched magnetically from the photosphere of the radiation-pressure-dominated disk only if the effective potential barrier along the magnetic field line is extremely shallow or no potential barrier is present. For the latter case, the slow sonic point in the outflow will probably be in the disk, which leads to a slow circular dense flow above the disk. This implies that hot gas (probably in the corona) is necessary for launching an outflow from the radiation-pressure-dominated disk, which provides a natural explanation for the observational evidence that the relativistic jets are related to hot plasma in some X-ray binaries and active galactic nuclei. We investigate the outflows accelerated from the hot corona above the disk by the magnetic field and radiation force of the accretion disk. We find that with the help of the radiation force, the mass loss rate in the outflow is high, which leads to a slow outflow. This may be why the jets in radio-loud narrow-line Seyfert galaxies are in general mildly relativistic compared with those in blazars.
Ngân sách tối thiểu phát hiện thông tin sai lệch trên mạng xã hội trực tuyến, đảm bảo đạt ít nhất một ngưỡng cho trước

Phát hiện nguồn phát tán thông tin sai lệch trên mạng xã hội trực tuyến đóng vai trò quan trọng trong việc hạnchế hành vi sai trái trên mạng. Các nghiên cứu gần đây cho thấy, phương pháp đặt máy giám sát có thể phát hiện nguồn thông tin sai lệch. Tuy nhiên, không thể đặt máy giám sát đối với tất cả người dùng mạng vì ngân sách hạn chế. Trong bài báo này, một mạng xã hội được biểu diễn bởi đồ thị có hướng, mỗi người dùng là một nút trên đồ thị và phát tán thông tin trên đồ thị theo mô hình Bậc độc lập. Trên mô hình này, giả sử biết trước tập nút nghi ngờ sẽ phát tán thông tin sai lệch, chúng tôi đề xuất tìm tập nút nhỏ nhất để đặt giám sát sao cho số nút bị phát hiện đạt ít nhất một ngưỡng cho trước. Ba thuật toán xấp xỉ được đề xuất, bao gồm: Tham lam, phát hiện thông tin sai lệch dựa trên tập mẫu phát hiện và phát hiện thông tin sai lệch dựa trên tập mẫu phát hiện quan trọng. Các thử nghiệm được thực hiện trên bộ dữ liệu của mạng xã hội thực cho thấy các thuật toán của chúng tôi đề xuất vượt trội hơn các thuật toán khác cả về hiệu suất và thời gian thực hiện.
SPECTRAL LAGS AND THE LAG–LUMINOSITY RELATION: AN INVESTIGATION WITH SWIFT BAT GAMMA-RAY BURSTS

Spectral lag, the time difference between the arrival of high-energy and low-energy photons, is a common feature in gamma-ray bursts (GRBs). Norris et al. reported a correlation between the spectral lag and the isotropic peak luminosity of GRBs based on a limited sample. More recently, a number of authors have provided further support for this correlation using arbitrary energy bands of various instruments. In this paper, we report on a systematic extraction of spectral lags based on the largest Swift sample to date of 31 GRBs with measured redshifts. We extracted the spectral lags for all combinations of the standard Swift hard X-ray energy bands: 15–25 keV, 25–50 keV, 50–100 keV, and 100–200 keV and plotted the time dilation corrected lag as a function of isotropic peak luminosity. The mean value of the correlation coefficient for various channel combinations is −0.68 with a chance probability of ∼0.7 × 10−3. In addition, the mean value of the power-law index is 1.4 ± 0.3. Hence, our study lends support to the existence of a lag–luminosity correlation, albeit with large scatter.
Scattered light images of spiral arms in marginally gravitationally unstable discs with an embedded planet

Scattered light images of transition discs in the near-infrared often show non-axisymmetric structures in the form of wide-open spiral arms in addition to their characteristic low-opacity inner gap region. We study self-gravitating discs and investigate the influence of gravitational instability on the shape and contrast of spiral arms induced by planet-disc interactions. Two-dimensional non-isothermal hydrodynamical simulations including viscous heating and a cooling prescription are combined with three-dimensional dust continuum radiative transfer models for direct comparison to observations. We find that the resulting contrast between the spirals and the surrounding disc in scattered light is by far higher for pressure scale height variations, i.e. thermal perturbations, than for pure surface density variations. Self-gravity effects suppress any vortex modes and tend to reduce the opening angle of planet-induced spirals, making them more tightly wound. If the disc is only marginally gravitationally stable with a Toomre parameter around unity, an embedded massive planet (planet-to-star mass ratio of $10^{-2}$) can trigger gravitational instability in the outer disc. The spirals created by this instability and the density waves launched by the planet can overlap resulting in large-scale, more open spiral arms in the outer disc. The contrast of these spirals is well above the detection limit of current telescopes.
THE INFRARED PROPERTIES OF EMBEDDED SUPER STAR CLUSTERS: PREDICTIONS FROM THREE-DIMENSIONAL RADIATIVE TRANSFER MODELS

With high-resolution infrared data becoming available that can probe the formation of high-mass stellar clusters for the first time, appropriate models that make testable predictions of these objects are necessary. We utilize a three-dimensional radiative transfer code, including a hierarchically clumped dusty envelope, to study the earliest stages of super star cluster (SSC) evolution. We explore a range of parameter space in geometric sequences that mimic the hypothesized evolution of an embedded SSC. The inclusion of a hierarchically clumped medium can make the envelope porous, in accordance with previous models and supporting observational evidence. The infrared luminosity inferred from observations can differ by a factor of two from the true value in the clumpiest envelopes depending on the viewing angle. The infrared spectral energy distribution also varies with viewing angle for clumpy envelopes, creating a range in possible observable infrared colors and magnitudes, silicate feature depths, and dust continua. General observable features of cluster evolution differ between envelopes that are relatively opaque or transparent to mid-infrared photons. For optically thick envelopes, evolution is marked by a gradual decline of the 9.8 μm silicate absorption feature depth and a corresponding increase in the visual/ultraviolet flux. For the optically thin envelopes, clusters typically begin with a strong hot dust component and silicates in emission, and these features gradually fade until the mid-infrared polycyclic aromatic hydrocarbon features are predominant. For the models with a smooth dust distribution, the Spitzer MIPS or Herschel PACS [70]−[160] color is a good probe of the stellar mass relative to the total mass or star formation efficiency (SFE). Likewise, the IRAC/MIPS [3.6]−[24] color can be used to constrain the Rin and Rout values of the envelope. However, clumpiness confuses the general trends seen in the smooth dust distribution models, making it harder to determine a unique set of envelope properties. Nevertheless, good diagnostic colors were found for each of the input parameters: again, the [70]−[160] color can be used to separate models with different SFEs; the Spitzer IRAC/MIPS [8.0]−[24] color is able to constrain Rin and Rout values; and the IRAC [3.6]−[5.8] color is sensitive to the fraction of the dust distributed in clumps. Finally, in a comparison of this model set to IRAS data of ultracompact H ii regions, we find good agreement, suggesting that these models are physically relevant, and will provide useful diagnostic ability for data sets of resolved, embedded SSCs with the advent of high-resolution infrared telescopes like James Webb Space Telescope.
A HUBBLE SPACE TELESCOPE SEARCH FOR A SUB-EARTH-SIZED EXOPLANET IN THE GJ 436 SYSTEM

The detection of small planets orbiting nearby stars is an important step toward the identification of Earth twins. In previous work using the Spitzer Space Telescope, we found evidence to support at least one sub-Earth-sized exoplanet orbiting the nearby mid-M dwarf star GJ 436. As a follow up, here we used the Hubble Space Telescope (HST) to investigate the existence of one of these candidate planets, UCF-1.01, by searching for two transit signals as it passed in front of its host star. Interpretation of the data hinges critically on correctly modeling and removing the Wide Field Camera 3 (WFC3) instrument systematics from the light curves. Building on previous HST work, we demonstrate that WFC3 analyses need to explore the use of a quadratic function to fit a visit-long time-dependent systematic. This is important for establishing absolute transit and eclipse depths in the white light curves of all transiting systems. The work presented here exemplifies this point by putatively detecting the primary transit of UCF-1.01 with the use of a linear trend. However, using a quadratic trend, we achieve a better fit to the white light curves and a reduced transit depth that is inconsistent with previous Spitzer measurements. Furthermore, quadratic trends with or without a transit model component produce comparable fits to the available data. Using extant WFC3 transit light curves for GJ 436b, we further validate the quadratic model component by achieving photon-limited model fit residuals and consistent transit depths over multiple epochs. We conclude that, when we fit for a quadratic trend, our new data contradict the prediction of a sub-Earth-sized planet orbiting GJ 436 with the size, period, and ephemeris posited from the Spitzer data by a margin of 3. 1σ.
El tamizado de ideas en el proceso de creación de nuevos productos

El lanzamiento de un nuevo producto es una de las decisiones más complejas y arriesgadas que se toman en la empresa, no sólo a nivel comercial. Una de las fases que se contempla en este proceso es el del tamizado o cribado de ideas que, a pesar de su importancia, no ha sido tratado, a nuestro juico, con la suficiente profundidad respecto a otras fases de los modelos de procesos de creación, desarrollo y lanzamiento de nuevos productos. Con este trabajo se pretende profundizar en esta fase del proceso, hasta llegar a unas conclusiones sobre los avances que se pueden hacer en este tema.
The Information and Communication Technology (ICT) Literacy of Local Community in Tourism Village of Karo Regency, Indonesia

This research was motivated by an indication of low ICT literacy in rural communities, especially villages that have great tourism potential, which makes it difficult for villages to be part of the information society and to use information and communication technology as one of the tools to promote tourism in the region. This study was designed to determine the ICT literacy levels of Tongging tourist Village, Karo Regency. ICT literacy was determined by measuring computer literacy, internet literacy, information literacy, and digital literacy. The study was conducted by survey method with a quantitative approach. The result showed that computer literacy, the internet, information and digital literacy of local community in Tongging Village mostly in level. Therefore, the ICT-Literacy level of people in Tongging village were also in level 3, where most individual has a standard knowledge of ICT that they needed, and consistently use that standard as a reference in everyday activities.
Localized deformation of a Cu46.25Zr45.25Al7.5Er1 bulk metallic glass

Using the cavity model and the concept of the plastic-hardening modulus, a simple relationship was established between the size of an indent and the size of a semi-spherical-shell softening zone. Indentation experiments of a Cu46.25Zr45. 25Al7.5Er1 bulk-metallic glass (BMG) were performed over a range of indentation loads from 500 to 4000 mN, using a Vickers indenter. The indentation hardness decreased slightly with the increase in the indentation load from 5.21 GPa at an indentation load of 500 mN to 4.66 GPa at an indentation load of 4000 mN. The evolution of shear bands underneath the indentation was studied using an interface-bonded BMG sample. Shear bands of a semi-spherical-shell shape and a line-shape were observed underneath the indentation. The dependence of the size of the shear-banding zone on the size of the indent was examined, which qualitatively supported the analytical model. The inter-banding spacing decreased with the increase in the indentation load, associated with the release of the stored strain energy.
Transient Weak-Lensing by Cosmological Dark Matter Microhaloes

We study the time variation of the apparent flux of cosmological point sources due to the transient weak lensing by dark matter microhaloes. Assuming a transverse motion of microhaloes with respect to our line of sight, we derive the correspondence between the temporal power spectrum of the weak lensing magnification, and the spatial power spectrum of density on small scales. Considering different approximations for the small scale structure of dark matter, we predict the apparent magnitude of cosmological point sources to vary by as much as $10^{-4}-10^{-3}$, due to this effect, within a period of a few months. This red photometric noise has an almost perfect gaussian statistics, to one part in $\sim 10^4$. We also compare the transient weak lensing power spectrum with the background effects such as the stellar microlensing on cosmological scales. A quasar lensed by a galaxy or cluster like SDSSJ1004+4112 strong lensing system, with multiple images, is a suitable system for this study as: (i) using the time-delay method between different images, we can remove the intrinsic variations of the quasar, and (ii) strong lensing enhances signals from the transient weak lensing. We also require the images to form at large angular separations from the center of the lensing structure, in order to minimize contamination by the stellar microlensing. With long-term monitoring of quasar strong lensing systems with a 10-meter class telescope, we can examine the existence of dark microhaloes as the building blocks of dark matter structures. Failure to detect this signal may either be caused by a breakdown of cold dark matter (CDM) hierarchy on small scales, or rather interpreted as evidence against CDM paradigm, e.g. in favor of modified gravity models.
Dilemmas and problems of being a moral educator

Kinesiology is the science of human movement. Within the United States, kinesiology encompasses different sub-disciplines of human movement, e.g., exercise physiology, biomechanics, sport psychology, and philosophy, as well as, the professions of teaching, leading, and training. This paper addresses one issue, the lack of moral education in the preparation of kinesiology pre-professionals. Moral education is imperative for kinesiology students to address issues of right and wrong as well as engage in higher order reasoning however, many problems exist in applying moral education to kinesiology. First, even though 37 states have some sort of requirement that moral education is a part of the general public education curriculum, apparently, no direct teaching of moral values exists in public elementary, middle, and high schools. Students arrive at the university with no background. Second, direct teaching of moral values is nonexistent because: teachers and college instructors are not content experts in moral education, consumer-based education drives and affects students’ value of education, and the fallacious argument that ethics should only be taught to the young. Third, moral pedagogy is seldom applied. All of which directly affects kinesiology students in making decisions of right and wrong in a service profession. Therefore, the purpose of this narrative philosophical paper is twofold: to discuss the problems and dilemmas incorporating moral education in kinesiology curriculum and discuss three specific solutions, the: a) creation of moral development courses, b) use of writing intensive courses, and c) development of courses in pedagogy. A narrative philosophical approach discusses theory and supports with real life examples.
Preoperative Omega-6/Omega-3 Fatty Acid Ratio Could Predict Postoperative Outcomes in Patients with Surgically Resected Non-Small-Cell Lung Cancer

Introduction: The aim of this study was to determine whether preoperative nutritional status and inflammatory status, specifically polyunsaturated acids and the omega 6/3 ratio, would affect postoperative outcomes and complications in patients with lung cancer undergoing lung resection. Methods: This prospective observational study included 68 patients with early-stage non-small-cell lung cancer who were candidates for radical surgery. A complete nutritional assessment was performed. The primary study variable was postoperative complications and mortality in the first 30 days. Descriptive, bivariate, and logistic regression analyses were carried out. Results: A total of 50 men (73.53%) and 18 women (26.47%) underwent surgery, with a median age of 64.2 (±9.74) years. The mean omega 6/3 ratio was 17.39 (±9.45). A complication occurred in 39.7% of the study sample (n = 27), the most common being persistent air leak in 23.53% (n = 16). After performing the bivariate analysis, the only variable that remained significant was the omega 6/3 ratio; we observed that it had a prognostic value for persistent air leak (p = 0.001) independent of age, sex, comorbidity, preoperative respiratory function, and approach or type of surgery. The remaining nutritional and inflammatory markers did not have a statistically significant association (p > 0.05) with postoperative complications. However, this significance was not maintained in the multivariate analysis by a small margin (p = 0.052; 95% CI: 0.77–1.41). Conclusions: Omega 6/3 ratio may be a prognostic factor for air leak, independent of the patient’s clinical and pathological characteristics.
LARGE-SCALE FILAMENTARY STRUCTURES AROUND THE VIRGO CLUSTER REVISITED

We revisit the filamentary structures of galaxies around the Virgo cluster, exploiting a larger data set, based on the HyperLeda database, than previous studies. In particular, this includes a large number of low-luminosity galaxies, resulting in better sampled individual structures. We confirm seven known structures in the distance range 4 h−1 Mpc < SGY < 16 h−1 Mpc, now identified as filaments, where SGY is the axis of the supergalactic coordinate system roughly along the line of sight. The Hubble diagram of the filament galaxies suggests they are infalling toward the main body of the Virgo cluster. We propose that the collinear distribution of giant elliptical galaxies along the fundamental axis of the Virgo cluster is smoothly connected to two of these filaments (Leo II A and B). Behind the Virgo cluster (16 h−1 Mpc < SGY < 27 h−1 Mpc), we also identify a new filament elongated toward the NGC 5353/4 group (“NGC 5353/4 filament”) and confirm a sheet that includes galaxies from the W and M clouds of the Virgo cluster (“W–M sheet”). In the Hubble diagram, the NGC 5353/4 filament galaxies show infall toward the NGC 5353/4 group, whereas the W–M sheet galaxies do not show hints of gravitational influence from the Virgo cluster. The filamentary structures identified can now be used to better understand the generic role of filaments in the build-up of galaxy clusters at z ≈ 0.
Quantum criticality and novel phases: Summary and outlook

This conference summary and outlook provides a personal overview of the topics and themes of the August 2009 Dresden meeting on quantum criticality and novel phases. The dichotomy between the local moment and the itinerant views of magnetism is revisited and refreshed in new materials, new probes, and new theoretical ideas. New universality and apparent zero temperature phases of matter move us beyond the old ideas of quantum criticality. This is accompanied by alternative pairing interactions and as yet unidentified phases developing in the vicinity of quantum critical points. In discussing novel order, the magnetic analogs of superconductivity are considered as candidate states for the hidden order that sometimes develops in the vicinity of quantum critical points in metallic systems. These analogs can be thought of as “pairing” in the particle–hole channel and are tabulated. This analogy is used to outline a framework to study the relation between ferromagnetic fluctuations and the propensity of a metal to nematic type phases – which at weak coupling correspond to Pomeranchuk instabilities. This question can be related to the fundamental relations of Fermi liquid theory.
Predicted Constraints on Cosmic String Tension from Planck and Future CMB Polarization Measurements

We perform a Fisher matrix calculation of the predicted uncertainties on estimates of the cosmic string tension Gmu from upcoming observational data (namely, cosmic microwave background power spectra from the Planck satellite and an idealized future polarization experiment). We employ simulations that are more general than others commonly used in the literature, leaving the mean velocity of strings, correlation length of the string network, and "wiggliness" (which parametrizes smaller-scale structure along the strings) as free parameters that can be observationally measured. In a new code, StringFast, we implement a method for efficient computation of the C_l spectra induced by a network of strings, which is fast enough to be used in Markov Chain Monte Carlo analyses of future data. Performing a calculation with the string parameters left free results in projected constraints on Gmu that are larger than those obtained by fixing their values a priori, typically by a factor of ~2-7. We also find that if Gmu is equal to the current observational maximum, Planck will be able to make a confident detection of strings. However, if Gmu is two orders of magnitude smaller, even a perfect, lensing-free measurement of polarization power spectra will not be able to detect a nonzero string tension at better than 2 sigma confidence.
An End-to-End Cardiac Arrhythmia Recognition Method with an Effective DenseNet Model on Imbalanced Datasets Using ECG Signal

Electrocardiography (ECG) is a well-known noninvasive technique in medical science that provides information about the heart's rhythm and current conditions. Automatic ECG arrhythmia diagnosis relieves doctors' workload and improves diagnosis effectiveness and efficiency. This study proposes an automatic end-to-end 2D CNN (two-dimensional convolution neural networks) deep learning method with an effective DenseNet model for addressing arrhythmias recognition. To begin, the proposed model is trained and evaluated on the 97720 and 141404 beat images extracted from the Massachusetts Institute of Technology-Beth Israel Hospital (MIT-BIH) arrhythmia and St. Petersburg Institute of Cardiological Technics (INCART) datasets (both are imbalanced class datasets) using a stratified 5-fold evaluation strategy. The data is classified into four groups: N (normal), V (ventricular ectopic), S (supraventricular ectopic), and F (fusion), based on the Association for the Advancement of Medical Instrumentation® (AAMI). The experimental results show that the proposed model outperforms state-of-the-art models for recognizing arrhythmias, with the accuracy of 99.80% and 99.63%, precision of 98.34% and 98.94%, and F1-score of 98.91% and 98.91% on the MIT-BIH arrhythmia and INCART datasets, respectively. Using a transfer learning mechanism, the proposed model is also evaluated with only five individuals of supraventricular MIT-BIH arrhythmia and five individuals of European ST-T datasets (both of which are also class imbalanced) and achieved satisfactory results. So, the proposed model is more generalized and could be a prosperous solution for arrhythmias recognition from class imbalance datasets in real-life applications.