Miracle-dz/UniFAR-FTUs huggingface dataset:
Compressed Learning in MCA Architectures to Tolerate Malicious Noise

It is shown that compressed learning tolerates adversarial attacks effectively and that classification accuracy is impacted minimally when the compression ratio is selected appropriately. An approach to select the compression ratio is presented. It is also shown that compressed learning is at least as tolerant to adversarial noise as the more power consuming compressive sensing method. Tolerance to adversarial attacks increases when the compressed learning-based neural network architecture is implemented on circuits that use Memristive Crossbar Arrays (MCAs). This paper shows that implementation on an MCA-based analog hardware circuit tolerates adversarial attacks more effectively than a hybrid MCA-based architecture while improving on latency and power consumption.
Modeling Dropwise Condensation underneath Unidirectional Wettability Graded Surfaces

The dropwise condensation underneath a horizontal super-hydrophobic surface having unidirectional wettability gradient is modeled with implication to enhance the rate of condensation. The mathematical model includes nucleation, growth by vapor condensation and coalescence, and drop instability arising from force imbalances at the three-phase contact line. The wettability graded surfaces, formed by a variable surface energy coating, allow the micro-drop of condensate to slide from the hydrophobic to the hydrophilic region without the aid of gravity. The resulting decrease in the drop sliding size shifts the drop size distribution to smaller radii. Furthermore, this decrease in sliding size enhances the heat transfer rate during dropwise condensation. Simulation data has been compared with condensation patterns for a horizontal surface and inclined surface, both with zero wettability gradients. Results obtained show that a wettability graded surface can effectively control the condensation process by decreasing the cycle time of nucleation, growth and removal.
Novel ceramic composites produced from coal discards with potential application in the building and construction sectors

In response to the enormous amounts of coal discard generated during coal mining and preparation, the development of an efficient and sustainable strategic use of this resource is essential. Furthermore, the rising urban population over the next decades is confronted with the depletion of quality raw materials for building components. To this end, this study reports new information on the morphology, water absorption, and flexural strength properties of ceramic composites produced from three different coal discards and polysiloxane pre-ceramic polymer (PCP) resin. In addition, test results relating to the continuous operating temperature, chemical resistance, and efflorescence potential of the composites are presented. The results show that the water absorption and flexural strength of the coal composites, up to 1.94% and 36.46 MPa respectively, exceed the requirements for ceramic and clay roof tiles. The continuous operating temperature of composites is found to be more thermally stable than conventional roofing tiles (concrete and ceramic) between ambient temperature and 600°C. In addition, the excellent chemical resistance of the composites (94.43%-99.98%) compared to conventional roofing tiles (67.82%-99.97%) eliminates the need for additional external coatings. The interesting results documented so far suggest that this technique could be used to produce low-temperature application building products such as bricks, panels, roofing tiles, etc. This new recycling technique offers an excellent opportunity to eliminate enormous volumes of coal discard and to advance the circular economy in the coal industry.
Star formation in the ultraluminous infrared galaxy F00183-7111

We report the detection of molecular CO(1-0) gas in F00183-7111, one of the most extreme Ultra-Luminous Infrared Galaxies known, with the Australia Telescope Compact Array. We measure a redshift of 0.3292 for F00183-7111 from the CO(1-0) line and estimate the mass of the molecular gas in 00183 to be 1 $\times$ 10$^{10}$ M$_{\odot}$. We find that F00183-7111 is predominately powered by the AGN and only $\sim$14 per cent of the total luminosity is contributed by star-formation (SFR $\sim$220 M$_{\odot}$ yr$^{-1}$). We also present an optical image of F00183-7111, which shows an extension to the East. We searched for star-formation in this extension using radio continuum observations but do not detect any. This suggests that the star-formation is likely to be predominately nuclear. These observations provide additional support for a model in which the radio emission from ULIRGs is powered by an intense burst of star-formation and by a radio-loud AGN embedded in its nucleus, both triggered by a merger of gas-rich galaxies.
EFFECT OF ENTREPRENEURIAL RISK PERCEPTION ON ENTREPRENEURIAL INTENTION WITH THE MEDIATING ROLE OF PERCEIVED BEHAVIORAL CONTROL

This article evaluated the multidimensional nature of entrepreneurial risk perceptions in an entrepreneurial setting and its effects on entrepreneurial intensions. Furthermore, mediation effects of perceived behavior control were also analyzed. Results of the study confirm multidimensional and domain specific nature of entrepreneurial risk perceptions. It also confirms the direct effects of positive and negative risk perceptions on entrepreneurial intentions. Lastly, through the lens of theory of planned behavior, entrepreneurial risk perceptions significantly effects perceived behavior control, which in turn has a significant effect on the entrepreneurial intensions.
PAGaN II: The Evolution of AGN Jets on Sub-Parsec Scales

We report first results from KVN and VERA Array (KaVA) VLBI observations obtained in the frame of our Plasma-physics of Active Galactic Nuclei (PAGaN) project. We observed eight selected AGN at 22 and 43 GHz in single polarization (LCP) between March 2014 and April 2015. Each source was observed for 6 to 8 hours per observing run to maximize the $uv$ coverage. We obtained a total of 15 deep high-resolution images permitting the identification of individual circular Gaussian jet components and three spectral index maps of BL Lac, 3C 111 and 3C 345 from simultaneous dual-frequency observations. The spectral index maps show trends in agreement with general expectations -- flat core and steep jets -- while the actual value of the spectral index for jets shows indications for a dependence on AGN type. We analyzed the kinematics of jet components of BL Lac and 3C 111, detecting superluminal proper motions with maximum apparent speeds of about $5c$. This constrains the lower limits of the intrinsic component velocities to $\sim0.98c$ and the upper limits of the angle between jet and line of sight to $\sim$20$\deg$. In agreement with global jet expansion, jet components show systematically larger diameters $d$ at larger core distances $r$, following the global relation $d\approx0.2r$, albeit within substantial scatter.
Quality work in higher education: a multi-stakeholder study

Abstract Quality in higher education has been at the top of the political agenda for years, motivating discussion of how to define quality and how standards and assessment can promote quality. However, the literature tends to overlook the processes and practices constituting ‘every-day’ quality. To improve quality, it is important to know how quality is perceived and enacted by the key stakeholders, namely the students, teachers, administrative staff and managers. Informed by the findings of a survey, this article aims to identify and compare the local practices of quality work at higher education institutions in Denmark. The analysis reveals that students, teachers and managers across sectors to a large extent share views on quality work highlighting practices that help develop students’ academic skills, the ability to apply these to practice and the continuous development of teaching practices. Some differences are however also apparent, for example, concerning employability orientation in higher education.
Inferring past refugia and range dynamics through the integration of fossil, niche modelling and genomic data

Reconstructing species' glacial refugial history and demographic changes over time has greatly relied on comparing inferences from multiple methods while not sufficiently acknowledging their limitations. Here, we aim to integrate as fully as possible complementary methods in ecology, genomics and palaeobiology to improve the reconstruction of species biogeographical history.
Resilience: Key Factors Associated With Resilience of Older People in Botswana

This study aims to determine key factors that predict resilience in older people. A cross-sectional design and quantitative methods were used for this study. Four districts were selected in Botswana using cluster random sampling. Data on resilience from 378 older adults aged 60 years+ [Mean Age (SD) = 71.1(9.0)] was collected using snowballing technique. Data on socio-demographics, protective and risk factors were also collected from urban and rural areas. CHAID (Chi-squared Automatic Interaction Detection) analysis was used to predict the strengths of the relationships among resilience and all predictor variables because the data were skewed. Five major predictor variables reached significance to be included in the model: depression, QOL, social impairment, education, and whether participants paid for services or accessed free services, along with high self-esteem (p < .001), security, and self-efficacy (p < .05). The presence of depression symptoms (χ2 = 23.7, p = .001, df = 1) and self-esteem (χ2 = 39.6, p < .001) had the greatest influence on resilience. Older people with no depression symptoms but had low QOL still had social impairment (χ2 = 3.9, p < .05). Older people with no depression symptoms had moderate to high QOL but had low resilience as a result of paying for services (χ2 = 7.4, p < .02). Both protective and risk factors had a significant influence on resilience. Knowledge about the predictors of resilience in older people may assist stakeholders devise effective intervention, especially now with COVID-19 ravaging the country. Additionally, policies and programs inclined to assist older people may be established and implemented.
ANALYZING BEHAVIORAL INTENTION OF E-WALLET USAGE IN FOOD AND BEVERAGE AT MICRO SMALL AND MEDIUM ENTERPRISES (MSME) IN MANADO

The purpose of this research is to find out the performance expectation, effort expectation, social influence, perceived risk, dan perceived cost on behavioral intention for E-wallet usage by MSMEs in Manado. This research is conducted by using quantitative method using questionnaires as data collection method. Owners/the person in charge of the micro, small and medium enterprises in Manado use e-wallet that can be informants about these issues. Researchers determine the minimum sample to be 100 respondents. The requirements in selecting the samples, Owners/people in charge of MSME that use e-wallet in transactions. In this study, the primary data collected is data obtained by submitting questionnaire. The result of this research showed that performance expectation has a negative and significant influence on behavior intention to use e-wallet in food and beverage MSME in Manado City, effort expectation and social influence have a positive and significant influence on behavior intention to use e-wallet in food and beverage MSME in Manado City, perceived risk and perceived cost have a negative and not significant influence on behavior intention to use e-wallet in food and beverage MSME in Manado City, and performance expectation, effort expectation, social influence, perceived risk, and perceived cost, simultaneously has a positive and significant influence on behavior intention to use e-wallet in food and beverage MSME in Manado City. It is recommended that MSME owner or management must consider the importance of variables in this research, as well as its importance in order to optimize the business activities. MSME owner also should consider focusing on the variables that have a significant influence in usage of e-wallet to improve the business activities. Keywords: E-Wallet, MSME, Entrepreneurship.
EVIDENCE FOR CLUSTER TO CLUSTER VARIATIONS IN LOW-MASS STELLAR ROTATIONAL EVOLUTION

The concordance model for angular momentum evolution postulates that star-forming regions and clusters are an evolutionary sequence that can be modeled with assumptions about protostar–disk coupling, angular momentum loss from magnetized winds that saturates in a mass-dependent fashion at high rotation rates, and core-envelope decoupling for solar analogs. We test this approach by combining established data with the large h Per data set from the MONITOR project and new low-mass Pleiades data. We confirm prior results that young low-mass stars can be used to test star–disk coupling and angular momentum loss independent of the treatment of internal angular momentum transport. For slow rotators, we confirm the need for star–disk interactions to evolve the ONC to older systems, using h Per (age 13 Myr) as our natural post-disk case. There is no evidence for extremely long-lived disks as an alternative to core-envelope decoupling. However, our wind models cannot evolve rapid rotators from h Per to older systems consistently, and we find that this result is robust with respect to the choice of angular momentum loss prescription. We outline two possible solutions: either there is cosmic variance in the distribution of stellar rotation rates in different clusters or there are substantially enhanced torques in low-mass rapid rotators. We favor the former explanation and discuss observational tests that could be used to distinguish them. If the distribution of initial conditions depends on environment, models that test parameters by assuming a universal underlying distribution of initial conditions will need to be re-evaluated.
Cosmological attractor inflation from the RG-improved Higgs sector of finite gauge theory

The possibility to construct an inflationary scenario for renormalization-group improved potentials corresponding to the Higgs sector of finite gauge models is investigated. Taking into account quantum corrections to the renormalization-group potential which sums all leading logs of perturbation theory is essential for a successful realization of the inflationary scenario, with very reasonable parameter values. The inflationary models thus obtained are seen to be in good agreement with the most recent and accurate observational data. More specifically, the values of the relevant inflationary parameters, ns and r, are close to the corresponding ones in the R2 and Higgs-driven inflation scenarios. It is shown that the model here constructed and Higgs-driven inflation belong to the same class of cosmological attractors.
Dwarf nova outbursts with magnetorotational turbulence

The phenomenological Disc Instability Model has been successful in reproducing the observed light curves of dwarf nova outbursts by invoking an enhanced Shakura-Sunyaev $\alpha$ parameter $\sim0.1-0.2$ in outburst compared to a low value $\sim0.01$ in quiescence. Recent thermodynamically consistent simulations of magnetorotational (MRI) turbulence with appropriate opacities and equation of state for dwarf nova accretion discs have found that thermal convection enhances $\alpha$ in discs in outburst, but only near the hydrogen ionization transition. At higher temperatures, convection no longer exists and $\alpha$ returns to the low value comparable to that in quiescence. In order to check whether this enhancement near the hydrogen ionization transition is sufficient to reproduce observed light curves, we incorporate this MRI-based variation in $\alpha$ into the Disc Instability Model, as well as simulation-based models of turbulent dissipation and convective transport. These MRI-based models can successfully reproduce observed outburst and quiescence durations, as well as outburst amplitudes, albeit with different parameters from the standard Disc Instability Models. The MRI-based model lightcurves exhibit reflares in the decay from outburst, which are not generally observed in dwarf novae. However, we highlight the problematic aspects of the quiescence physics in the Disc Instability Model and MRI simulations that are responsible for this behavior.
Probing parton dynamics of QCD matter with Ω and Φ production

Author(s): Adamczyk, L; Adkins, JK; Agakishiev, G; Aggarwal, MM; Ahammed, Z; Alekseev, I; Aparin, A; Arkhipkin, D; Aschenauer, EC; Attri, A; Averichev, GS; Bai, X; Bairathi, V; Bellwied, R; Bhasin, A; Bhati, AK; Bhattarai, P; Bielcik, J; Bielcikova, J; Bland, LC; Bordyuzhin, IG; Bouchet, J; Brandenburg, JD; Brandin, AV; Bunzarov, I; Butterworth, J; Caines, H; Calderon De La Barca Sanchez, M; Campbell, JM; Cebra, D; Chakaberia, I; Chaloupka, P; Chang, Z; Chatterjee, A; Chattopadhyay, S; Chen, JH; Chen, X; Cheng, J; Cherney, M; Christie, W; Contin, G; Crawford, HJ; Das, S; De Silva, LC; Debbe, RR; Dedovich, TG; Deng, J; Derevschikov, AA; Di Ruzza, B; Didenko, L; Dilks, C; Dong, X; Drachenberg, JL; Draper, JE; Du, CM; Dunkelberger, LE; Dunlop, JC; Efimov, LG; Engelage, J; Eppley, G; Esha, R; Evdokimov, O; Eyser, O; Fatemi, R; Fazio, S; Federic, P; Fedorisin, J; Feng, Z; Filip, P; Fisyak, Y; Flores, CE; Fulek, L; Gagliardi, CA; Garand, D; Geurts, F; Gibson, A; Girard, M; Greiner, L; Grosnick, D; Gunarathne, DS; Guo, Y; Gupta, S; Gupta, A; Guryn, W; Hamad, AI | Abstract: © 2016 American Physical Society. We present measurements of Ω and φ production at midrapidity from Au+Au collisions at nucleon-nucleon center-of-mass energies sNN=7.7, 11.5, 19.6, 27, and 39 GeV by the STAR experiment at the BNL Relativistic Heavy Ion Collider (RHIC). Motivated by the coalescence formation mechanism for these strange hadrons, we study the ratios of N(Ω-+Ω#x0002B;)/[2N(φ)]. These ratios as a function of transverse momentum pT fall on a consistent trend at high collision energies, but start to show deviations in peripheral collisions at sNN=19.6, 27, and 39 GeV, and in central collisions at 11.5 GeV in the intermediate pT region of 2.4-3.6 GeV/c. We further evaluate empirically the strange quark pT distributions at hadronization by studying the Ω/φ ratios scaled by the number of constituent quarks (NCQ). The NCQ-scaled Ω/φ ratios show a suppression of strange quark production in central collisions at 11.5 GeV compared to sNN≥19.6 GeV. The shapes of the presumably thermal strange quark distributions in 0-60% most central collisions at 7.7 GeV show significant deviations from those in 0-10% most central collisions at higher energies. These features suggest that there is likely a change of the underlying strange quark dynamics in the transition from quark matter to hadronic matter at collision energies below 19.6 GeV.
Extreme flux states of NGC 4151 observed with INTEGRAL

We present a comprehensive spectral analysis of all INTEGRALdata obtained so far for the X-ray‐bright Seyfert galaxy NGC 4151. We also use all contemporaneous data from RXTE, XMM-Newton, Swift and Suzaku. We find a linear correlation between the medium and hardenergy X-ray fluxes measured by INTEGRAL, which indicates an almost constant spectral index over six years. The majority of INTEGRAL observations were made when the source was either at a very bright or very dim hard‐X-ray state. We fin d that thermal Comptonization models applied to the bright state yields the plasma temperature of'50‐70 keV and its optical depth of'1: 3‐2.6, depending on the assumed source geometry. For the dim state, these parameters are in the ranges of'180‐230 keV and'0: 3‐0.7, respectively. The Compton parameter is y'1 for all the spectra, indicating a stable geometry. Using th is result, we can determine the reflection e ffective solid angles associated with the close and distant re processing media as'0: 3�2� and 0: 2�2�, respectively. The plasma energy balance, the weak disc reflection and a comparison of the UV fluxes illuminating the plasma to the observed ones are all consistent with an inner hot accretion surround ed by an outer cold disc. The disc truncation radius can be determined from an approximate equipartition between the observed UV and X-ray emission, and from the fitted disc blackbody mode l, as�15 gravitational radii. Alternatively, our results can be explained by a mildly rela tivistic coronal outflow.
The influence of collimation on the appearance of relativistic jets

Abstract The question of the collimation of relativistic jets is the subject of a lively debate in the community. We numerically compute the apparent velocity and the Doppler factor of a non homokinetic jet using different velocity profile, to study the effect of collimation on the appearance of relativistic jets (apparent velocity and Doppler factor). We argue that if the motion is relativistic, the high superluminal velocity are possible only if the geometrical collimation is smaller than the relativistic beaming angle γ−1. In the opposite case, the apparent image will be dominated by the part of the jet traveling directly towards the observer resulting in no apparent velocity. Furthermore, getting rid of the homokinetic hypothesis yields a complex relation between the observing angle and the Doppler factor, resulting in important consequences for the numerical computation of AGN population and unification scheme model.
High efficiency of collisional Penrose process requires heavy particle production

The center-of-mass energy of two particles can become arbitrarily large if they collide near the event horizon of an extremal Kerr black hole, which is called the Banados-Silk-West (BSW) effect. We consider such a high-energy collision of two particles which started from infinity and follow geodesics in the equatorial plane and investigate the energy extraction from such a high- energy particle collision and the production of particles in the equatorial plane. We analytically show that, on the one hand, if the produced particles are as massive as the colliding particles, the energy-extraction efficiency is bounded by 2.19 approximately. On the other hand, if a very massive particle is produced as a result of the high-energy collision, which has negative energy and necessarily falls into the black hole, the upper limit of the energy-extraction efficiency is increased to (2+ √ 3) 2 ≃ 13.9. Thus, higher efficiency of the energy extraction, which is t ypically as large as
Optical observations of SAX J1808.4−3658 during quiescence

We observed the accreting millisecond pulsar SAX J1808.4-3658 with Gemini-South in g' and i' bands, nearly simultaneous with XMM-Newton observations. A clear periodic flux modulation on the system's orbital period is present, consistent with the varying aspect of the donor star's heated face. We model the contributions of a disc and donor star to these optical bands. To produce the observed modulation amplitudes, we conclude that the donor must be irradiated by an external flux two orders of magnitude greater than provided by the measured X-ray luminosity. A possible explanation for this irradiation is that the radio pulsar mechanism becomes active during the quiescent state as suggested by Burderi et al., with relativistic particles heating the donor's day side face. Our modelling constrains the binary inclination to be 36°-67°. We obtain estimates for the pulsar mass of >2.2 M ⊙ (although this limit is sensitive to the source's distance), consistent with the accelerated neutron star cooling in this system indicated by X-ray observations. We also estimate the donor mass to be 0.07-0.11 M ⊙ , providing further indications that the system underwent non-standard binary evolution to reach its current state.