Miracle-dz/UniFAR-FTUs huggingface dataset:
ASTROMETRY WITH THE HUBBLE SPACE TELESCOPE: TRIGONOMETRIC PARALLAXES OF SELECTED HYADS

We present absolute parallaxes and proper motions for seven members of the Hyades open cluster, pre-selected to lie in the core of the cluster. Our data come from archival astrometric data from fine guidance sensor (FGS) 3 and newer data for three Hyads from FGS 1r, both white-light interferometers on the Hubble Space Telescope (HST). We obtain member parallaxes from six individual FGS fields and use the field containing van Altena 622 and van Altena 627 (= HIP 21138) as an example. Proper motions, spectral classifications, and VJHK photometry of the stars comprising the astrometric reference frames provide spectrophotometric estimates of reference star absolute parallaxes. Introducing these into our model as observations with error, we determine absolute parallaxes for each Hyad. The parallax of vA 627 is significantly improved by including a perturbation orbit for this previously known spectroscopic binary, now an astrometric binary. Compared to our original (1997) determinations, a combination of new data, updated calibration, and improved analysis lowered the individual parallax errors by an average factor of 4.5. Comparing parallaxes of the four stars contained in the Hipparcos catalog, we obtain an average factor of 11 times improvement with the HST. With these new results, we also have better agreement with Hipparcos for the four stars in common. These new parallaxes provide an average distance for these seven members, 〈D〉 = 47.5 pc, for the core, a ±1σ dispersion depth of 3.6 pc, and a minimum depth from individual components of 16.0 ± 0.9 pc. Absolute magnitudes for each member are compared to established main sequences with excellent agreement. We obtain a weighted average distance modulus for the core of the Hyades of m − M = 3.376 ± 0.01, a value close to the previous Hipparcos values, m − M = 3.33 ± 0.02.
Gamification in Engineering Education: Exploring Students' Performance, Motivation, and Engagement

Gamification has become a popular approach to support teaching and learning in Higher Education. A significant bag of research has demonstrated its benefits, such as engagement, motivation, and learning performance. However, it has been argued that the success of a gamification application does not occur automatically without a good design process. This paper presents the design and implementation of Easy-Newton, a gamified application to help students practice physics-related concepts in a Higher Education context. The application includes gamification elements such as scores, levels, badges, and progress over the different topics and chapters. A total of 4 teachers and 261 students have utilized Easy-Newton in different stages of the design and implementation processes. We report the evaluation of Easy-Newton in terms of students' perceived motivation, engagement, and academic performance. For students' motivation, 84% of students (n = 163) reported a good experience using Easy-Newton. Concerning engagement, 88% of students (n = 261) completed at least one hard level from one topic, and 71% of students finished a complete chapter. As for the academic performance, there was no strong correlation between the usage (time a student spent) of Easy-Newton and its GPA, suggesting that more complex exercises, similar to the ones proposed in exams, should also be considered in the application.
KINEMATIC AND ENERGETIC PROPERTIES OF THE 2012 MARCH 12 POLAR CORONAL MASS EJECTION

We report on the energetics of the 2012 March 12 polar coronal mass ejection (CME) originating from a southern latitude of ∼60°. The polar CME is similar to low-latitude (LL) CMEs in almost all respects: three-part morphology; post-eruption arcade (PEA), CME, and filament kinematics; CME mass and kinetic energy; and the relative thermal energy content of the PEA. From polarized brightness images, we estimate the CME mass, which is close to the average mass of LL CMEs. The CME kinetic energy (3.3 × 1030 erg) is also typical of the general population of CMEs. From photospheric magnetograms, we estimate the free energy (1.8 × 1031 erg) in the polar crown source region, which we find is sufficient to power the CME and the PEA. About 19% of the free energy went into the CME kinetic energy. We compute the thermal energy content of the PEA (2.3 × 1029 erg) and find it to be a small fraction (6.8%) of the CME kinetic energy. This fraction is remarkably similar to that in active region CMEs associated with major flares. We also show that the 2012 March 12 is one among scores of polar CMEs observed during the maximum phase of cycle 24. The cycle 24 polar crown prominence eruptions have the same rate of association with CMEs as those from LLs. This investigation supports the view that all CMEs are magnetically propelled from closed field regions, irrespective of their location on the Sun (polar crown filament regions, quiescent filament regions, or active regions).
Uncovering selective excitations using the resonant profile of indirect inelastic x-ray scattering in correlated materials: observing two-magnon scattering and relation to the dynamical structure factor

Resonant inelastic x-ray scattering (RIXS) is a spectroscopic technique that has been widely used to study various elementary excitations in correlated and other condensed matter systems. For strongly correlated materials, besides boosting the overall signal the dependence of the resonant profile on incident photon energy is still not fully understood. Previous endeavors in connecting indirect RIXS, such as Cu K-edge where scattering takes place only via the core–hole created as an intermediate state, with the charge dynamical structure factor S(q,ω) neglected complicated dependence on the intermediate state configuration. To resolve this issue, we performed an exact diagonalization study of the RIXS cross-section using the single-band Hubbard model by fully addressing the intermediate state contribution. Our results are relevant to indirect RIXS in correlated materials, such as high-Tc cuprates. We demonstrate that RIXS spectra can be reduced to S(q,ω) when there is no screening channel for the core–hole potential in the intermediate state. We also show that two-magnon excitations are highlighted at the resonant photon energy when the core–hole potential in the corresponding intermediate state is poorly screened. Our results demonstrate that different elementary excitations can be emphasized at different intermediate states, such that selecting the exact incident energy is critical when trying to capture a particular elementary excitation.
Prediction of Brain Stroke using Machine Learning with Relief Algorithm

Stroke is one of the leading factors of fatality in people today. Numerous conditions, including stress, high blood pressure, cholesterol, obesity, type 2 diabetes, and dyslipidemia illnesses, may all contribute to stroke. By measuring the recorded values of the patients for about 31 features, such as heart rate, cholesterol level, blood pressure, heart rate, diabetes, metabolic syndrome, haemoglobin, steatosis, fibrosis, hepatocellular carcinoma, Body Mass Index (BMI) and so on. The proposed system uses machine learning to predict strokes in patients. The patient data is used to anticipate their health conditions and so as to save their lives. To anticipate strokes, comparing machine learning techniques K-Nearest Neighbour(KNN), Decision Tree (DT), Random Forest (RF), Support Vector Machine (SVM), and Logistic Regression (LR) are used. The relief algorithm is used to select the necessary attributes. An ensemble model comprising SVM, RF, and KNN gives better accuracy compared to base models.
The host galaxy of the z = 2.4 radio-loud AGN MRC 0406−244 as seen by HST

We present multicolour Hubble Space Telescope images of the powerful z=2.4 radio galaxy MRC 0406-244 and model its complex morphology with several components including a host galaxy, a point source, and extended nebular and continuum emission. We suggest that the main progenitor of this radio galaxy was a normal, albeit massive (M ~10^{11} solar masses), star-forming galaxy. The optical stellar disc of the host galaxy is smooth and well described by a S\'ersic profile, which argues against a recent major merger, however there is also a point-source component which may be the remnant of a minor merger. The half-light radius of the optical disc is constrained to lie in the range 3.5 to 8.2kpc, which is of similar size to coeval star forming galaxies. Biconical shells of nebular emission and UV-bright continuum extend out from the host galaxy along the radio jet axis, which is also the minor axis of the host galaxy. The origin of the continuum emission is uncertain, but it is most likely to be young stars or dust-scattered light from the AGN, and it is possible that stars are forming from this material at a rate of 200^{+1420}_{-110} solar masses per year.
A Parameter Study for Modeling Mg ii h and k Emission during Solar Flares

Solar flares show highly unusual spectra in which the thermodynamic conditions of the solar atmosphere are encoded. Current models are unable to fully reproduce the spectroscopic flare observations, especially the single-peaked spectral profiles of the Mg ii h and k lines. We aim to understand the formation of the chromospheric and optically thick Mg ii h and k lines in flares through radiative transfer calculations. We take a flare atmosphere obtained from a simulation with the radiative hydrodynamic code RADYN as input for a radiative transfer modeling with the RH code. By iteratively changing this model atmosphere and varying thermodynamic parameters such as temperature, electron density, and velocity, we study their effects on the emergent intensity spectra. We reproduce the typical single-peaked Mg ii h and k flare spectral shape and approximate the intensity ratios to the subordinate Mg ii lines by increasing either densities, temperatures, or velocities at the line core formation height range. Additionally, by combining unresolved upflows and downflows up to ∼250 km s−1 within one resolution element, we reproduce the widely broadened line wings. While we cannot unambiguously determine which mechanism dominates in flares, future modeling efforts should investigate unresolved components, additional heat dissipation, larger velocities, and higher densities and combine the analysis of multiple spectral lines.
Radio observations of the Galactic Centre and the Coma cluster as a probe of light dark matter self-annihilations and decay

We update our earlier calculations of gamma ray and radio observational constraints on annihilations of dark matter particles lighter than 10 GeV. We predict the synchrotron spectrum as well as the morphology of the radio emission associated with light decaying and annihilating dark matter candidates in both the Coma cluster and the Galactic Centre. Our new results basically confirm our previous findings: synchrotron emission in the very inner part of the Milky Way constrains or even excludes dark matter candidates if the magnetic field is larger than 50 micro Gauss. In fact, our results suggest that light annihilating candidates must have a S-wave suppressed pair annihilation cross section into electrons (or the branching ratio into electron positron must be small). If dark matter is decaying, it must have a life time that is larger than t = 3. 10^{25} s. Therefore, radio emission should always be considered when one proposes a "light" dark matter candidate.
Dispersion measure variations in a sample of 168 pulsars

ABSTRACT We analyse dispersion measure (DM) variations in six years of radio observations ofmore than 160 young pulsars, all gamma ray candidates for the Fermi gamma raytelescope mostly located close to the Galactic plane. DMs were t across 256 MHzof bandwidth for observations centred at 1.4 GHz and across three frequencies {0.7 GHz, 1.4 GHz, and 3.1 GHz { where multifrequency observations were available.Changes in dispersion measure, dDM/dt, were calculated using a weighted linear tacross all epochs of available DMs. DM variations were detected at a 3˙level in 11pulsars, four of which were above 5˙: PSRs J0835 4510, J0908 4913, J1824 1945,and J1833 0827. We nd that after 28 years of gradual decline, the DM of PSRJ0835 4510 is now increasing. The magnitude of variations in three of the four (PSRsJ0835 4510, J0908 4913, and J1833 0827) are above what models would predict foran ISM dominated by Kolmogorov turbulence. We attribute this excess as likely dueto the pulsar’s local environment - the supernova remnants near PSRs J0835 4510and J1833 0827 and the pulsar wind nebula around PSR J0908 4913. Upper limitswere determined for all pulsars without detectable values of dDM/dt, most limits werefound to lie above the levels of variations predicted by ISM theory. We nd our resultsto be consistent with scattering estimates from the NE2001 model along these lines ofsight.Key words: pulsars: general | pulsars: individual: PSR J0835 4510 | pulsars:individual: PSR J0908 4913 | pulsars: individual: PSR J1824 1945 | pulsars: in-dividual: PSR J1833 0827 | ISM: structure
Magnetic absorption of VHE photons in the magnetosphere of the Crab pulsar

The detection of the pulsed $\sim 1 $~TeV gamma-ray emission from the Crab pulsar reported by MAGIC and VERITAS collaborations demands a substantial revision of existing models of particle acceleration in the pulsar magnetosphere. In this regard model independent restrictions on the possible production site of the VHE photons become an important issue. In this paper, we consider limitations imposed by the process of conversion of VHE gamma rays into $e^{\pm}$ pairs in the magnetic field of the pulsar magnetosphere. Photons with energies exceeding 1~TeV are effectively absorbed even at large distances from the surface of the neutron star. Our calculations of magnetic absorption in the force-free magnetosphere show that the twisting of the magnetic field due to the pulsar rotation makes the magnetosphere more transparent compared to the dipole magnetosphere. The gamma-ray absorption appears stronger for photons emitted in the direction of rotation than in the opposite direction. There is a small angular cone inside which the magnetosphere is relatively transparent and photons with energy $1.5$~TeV can escape from distances beyond $0.1$~light cylinder radius ($R_{\rm{lc}}$). The emission surface from where photons can be emitted in the observer's direction further restricts the sites of VHE gamma-ray production. For the observation angle $57^{\circ}$ relative to the Crab pulsar axis of rotation and the orthogonal rotation, the emission surface in the open field line region is located as close as $0.4\,R_{\rm{lc}}$ from the stellar surface for a dipole magnetic field, and $0.1\,R_{\rm{lc}}$ for a force-free magnetic field.
Support Vector Machine Classifier based Lung Cancer Recognition: A Fusion Approach

The emergence of computer-aided detection systems emphasized the need of clinical analysis in making decisions regarding human diseases. The evaluation procedure requires special attention since majority of the population have been affected by it resulting in a higher fatality rate. Traditional lung cancer prediction algorithms failed to manage accuracy due to data balance issues and low-quality images that interfere with discriminate features. In this paper, new feature fusion approach used by combining both EfficientNetB7 deep feature and statistical features and ADASYN applied to overcome the problem of data imbalance problem in the dataset. Balance feature set is classified using SVM classifier. Experiments conducted on the IQ-OTHNCCD lung cancer dataset demonstrate that our proposed methods are able to achieve better performance compared with the state of the art. The experimental study showed that the proposed model is efficient in terms of f-measure.
Real- Time Access Control System Based on Temperature Detection and the Correct Use of Face Masks

Nowadays, the COVID-19 pandemic has changed our lives. Some biosecurity measures have been implemented, including the use of face masks and the detection of body temperature; however, there are a lot of outbreaks, and the world cannot overcome this illness. In multiple cases, it is very difficult to measure the temperature and verify the correct use of face masks in everyone. Therefore, this paper proposes a real-time access control system based on body temperature detection and the correct use of face masks. This system uses a Raspberry Pi 4, which integrates temperature measurement using a thermal imager, the detection of the correct use of face masks using Convolutional Neural Networks (CNN), with a model built based on TensorFlow and MobileNetV2 that works on the video obtained from a thermographic camera using OpenCV and the Real Real-Time Streaming Protocol (RSTP). The system includes four modules: body temperature detection, processes, access, and visual interface. As a result, the access control system establishes six classification cases: high temperature and low temperature in faces without a mask, with an incorrectly placed mask, and with a correctly placed mask. The results show a system performance greater than 95% in all cases with a neural network model trained with a learning rate of 10E-4 and 15 epochs.
Energy Band Analysis for Screening Patients Diagnosed with ALS

This paper proposes spectral band analysis of voice signals for the automatic discrimination between patients diagnosed with Amyotrophic Lateral Sclerosis (ALS) and healthy speakers. Tests with repeated cross-validation obtained an average accuracy of 85.2% for a database with all patients diagnosed with Bulbar-type ALS, and with the vowel /a/. This new approach shows results superior to those obtained in the related work where the accuracy has 75%. Using another database with more diversified patients, an average accuracy of 69.4% was obtained with the vowel /a/, and 72.9% with the vowel /i/.
Quantum thermalization of two coupled two-level systems in eigenstate and bare-state representations

We study analytically the quantum thermalization of two coupled two-level systems (TLSs), which are connected with either two independent heat baths (IHBs) or a common heat bath (CHB). We understand the quantum thermalization in eigenstate and bare-state representations when the coupling between the two TLSs is stronger and weaker than the TLS-bath couplings, respectively. In the IHB case, we find that, when the two IHBs have the same temperatures, the two coupled TLSs in eigenstate representation can be thermalized with the same temperature as those of the IHBs. However, in the case of two IHBs at different temperatures, just when the energy detuning between the two TLSs satisfies a special condition, the two coupled TLSs in eigenstate representation can be thermalized with an immediate temperature between those of the two IHBs. In bare-state representation, we find a counterintuitive phenomenon that, under some conditions, the temperature of the TLS connected with the high-temperature bath is lower than that of the other TLS, which is connected with the low-temperature bath. In the CHB case, the coupled TLSs in eigenstate representation can be thermalized with the same temperature as that of the CHB in nonresonant cases. In bare-state representation, the TLS with a larger energy separation can be thermalized to a thermal equilibrium with a lower temperature. In the resonant case, we find a phenomenon of antithermalization. We also study the steady-state entanglement between the two TLSs in both the IHB and CHB cases.
Redundancy of Transport Subsystem in Providing Reliability of Supply Chain

Extensive development of the theory of logistics has been reflected in numerous publications on its various directions, including the issues of supply chain evaluation, the increased importance of which is noted by many leading experts. At the same time, evaluation becomes more complex by planning levels, by supplier/consumer levels, etc., as the chain itself expands, both at the design stage and in the process of operation. Ensuring reliability is a major supply chain challenge. Reliability of complex systems including a significant number of elements operating under conditions of uncertainty of the external environment becomes especially important. At the same time failures of modern chains of supply are associated with great technical and economic losses. All this causes necessity of the proved and qualitative design and operation of supply chains, development of the full methodology and sufficient methodical apparatus of management of reliability of supply chains which are absent at present. The development of the Arctic zone presupposes the creation and operation of large-scale both in structure and volume of served flows, especially cargo transportation systems, which increases the problem of forming reliable supply chains.
Fool Your Enemies: Enable Cyber Deception and Moving Target Defense for Intrusion Detection in SDN

The adoption of deception technology constructed to throw off stealthy attackers from real assets and gather intelligence about how they operate is gaining ground in the network system. Also, some static honeypots are deployed in the network system to attract adversaries for avoiding them accessing the real targets. This leads to a disclosure of the existence of cyber traps in the network that do not fool skillful attackers. Meanwhile, there are many intrusion detection systems (IDS) lack the abnormal traffic sample to obtain the knowledge of cyberattacks. Hence, it is vital to make honeypots more dynamically and give the material for harvesting useful threat intelligence for detector. Taking advantage of Software Defined Networking (SDN), cyber traps can be easily deployed when an intrusion detector triggers or actively laid in advance to mitigate the impact of adversaries into real assets. Instead of building IDS separately or blocking attacks promptly after an alert issued, in this paper, we utilize the strategy of associating Cyber Deception, and Moving Target Defense (MTD) with IDS in SDN, named FoolYE (Fool your enemies) to slow a network intruder down and leverage the behaviors of adversaries on traps for feeding back detector awareness.
Geomagnetic Earthquake Precursors Improvement Formulation on the basis of SKO (Skopje) and PAG (Intermagnet) Geomagnetic Data

In this paper we show that the simple analysis of the local geomagnetic field behaviour can serve as reliable imminent precursor for regional seismic activity increasing. As the first step the problem was investigated using one- component Dubna fluxgate magnetometer. The result of 2001-2004 Sofia monitoring confirmed many old papers for connection between Earth tide (Sun- Moon tides as earthquakes trigger) and jump (Geomagnetic quake) of daily averaged one minute standart deviation of the geomagnetic field. The second step (2004-present), which included analisys of three-component Danish fluxgate magnetometer data, worked in Skopje Seismological observatory, confirmed the first step result. The analysis of INTERMAGNET data stations around which was happened stronger earthquakes also confirmed our result. The distribution of time difference between the times of such earthquakes and local daily averaged tide vector movement for impending tide extreme confirms our estimate that the increasing seismicity is realized in time window about +/- 2.7 days. The Complex program for researching the possibility for when, where and how earthquakes prediction is proposed as well as the short description of FORTRAN codes for analysis of earthquakes, geomagnetic and tide data, their correlations and visualization.