Miracle-dz/UniFAR-FTUs huggingface dataset:
Modified Newton's law, braneworlds, and the gravitational quantum well

Most of the theories involving extra dimensions assume that only the gravitational interaction can propagate in them. In such approaches, called braneworld models, the effective, four-dimensional, Newton's law is modified at short as well as at large distances. Usually, the deformation of Newton's law at large distances is parametrized by a Yukawa potential, which arises mainly from theories with compactified extra dimensions. In many other models however, the extra dimensions are infinite. These approaches lead to a large distance power-law deformation of the gravitational Newtonian potential VN(r), namely V(r) = (1 + kb/rb)VN(r), which is less studied in the literature. We investigate here the dynamics of a particle in a gravitational quantum well with such a power-law deformation. The effects of the deformation on the energy spectrum are discussed. We also compare our modified spectrum to the results obtained with the GRANIT experiment, where the effects of the Earth's gravitational field on quantum states of ultra-cold neutrons moving above a mirror are studied. This comparison leads to upper bounds on b and kb.
Interconnecting Power-Electronic Buck Converter Modules in a Novel High-Power Test Bench for MVDC Circuit Breakers

Advances in medium voltage direct current (MVDC) technologies and the penetration of extended MVDC systems are still significantly hindered by the lack of adequate direct current (DC) switching equipment. The fundamentally different fault current behavior in case of a DC fault, compared to faults in alternating current (AC) systems, with regard to the characteristics and development of fault currents and their interruption make dedicated test procedures necessary. One testing approach is the application of a power-electronic buck converter (PEBC) to simulate relevant stresses on DC switching equipment during a DC fault current interruption. Since the associated requirements, especially regarding current ratings of several kiloamperes, cannot be fulfilled by using a singular PEBC, a modularization becomes necessary. However, particularly in high-power applications, the interconnection of several PEBC modules poses significant challenges. In this article, a demonstrator PEBC-based high-power test circuit for the provision of relevant testing parameters is presented. The underlying challenges and respective solutions with regard to the interconnection of, in total, 120 individual PEBC modules are discussed. It can be shown that the harmonization of connection busbar inductances is the main contributor towards a stable and safe test circuit operation.
Transposable Elements as a Source of Novel Repetitive DNA in the Eukaryote Genome

The impact of transposable elements (TEs) on the evolution of the eukaryote genome has been observed in a number of biological processes, such as the recruitment of the host’s gene expression network or the rearrangement of genome structure. However, TEs may also provide a substrate for the emergence of novel repetitive elements, which contribute to the generation of new genomic components during the course of the evolutionary process. In this review, we examine published descriptions of TEs that give rise to tandem sequences in an attempt to comprehend the relationship between TEs and the emergence of de novo satellite DNA families in eukaryotic organisms. We evaluated the intragenomic behavior of the TEs, the role of their molecular structure, and the chromosomal distribution of the paralogous copies that generate arrays of repeats as a substrate for the emergence of new repetitive elements in the genome. We highlight the involvement and importance of TEs in the eukaryote genome and its remodeling processes.
The second ROSAT PSPC survey of M 31 and the complete ROSAT PSPC source list

This paper reports the results of the analysis of the second ROSAT PSPC survey of M 31 performed in summer 1992. We compare our results with those of the rst survey, already published in Supper et al. (1997). Within the10: 7d eg 2 eld of view, 396 individual X-ray sources are detected in the second survey data, of which 164 are new detections. When combined with the rst survey, this result in a total of 560 X-ray sources in the eld of M 31. Their (0.1 keV{2.0 keV) fluxes range from 7 10 15 erg cm 2 s 1 to 7:6 10 12 erg cm 2 s 1 , and of these 560 sources, 55 are tentatively identied with foreground stars, 33 with globular clusters, 16 with supernova remnants, and 10 with radio sources and galaxies (including M 32). A comparison with the results of the Einstein M 31 survey reveals 491 newly detected sources, 11 long term variable sources, and 7 possible transient sources. Comparing the two ROSAT surveys, we come up with 34 long term variable sources and 8 transient candidates. For the M 31 sources, the observed luminosities range from 4 10 35 erg s 1 to 4 10 38 erg s 1 . The total (0.1 keV{2.0 keV) luminosity of M 31 is (3:4 0:3) 10 39 erg s 1 , distributed approximately equally between the bulge and disk. Within the bulge region, the luminosity of a possible diuse component combined with faint sources below the detection threshold is (2:0 0:5) 10 38 erg s 1 . An explanation in terms of hot gaseous emission leads to a maximum total gas mass of (1:0 0:3) 10 6 M.
An FPTAS for the Single Machine Minimum Total Weighted Tardiness Problem With a Fixed Number of Distinct Due Dates

This thesis provides a Fully Polynomial Time Approximation Scheme (FPTAS) for the minimum total weighted tardiness (TWT) problem with a constant number ofdistinct due dates. Given a sequence of jobs on a single machine, each with a weight, processing time, and a due date, the tardiness of a job is the amount of time that its completion time goes beyond its due date. The TWT problem is to find a schedule of the given jobs such that the total weighted tardiness is minimized. This problem is NP-hard even when the number of distinct due dates is fixed. In this thesis, we present a dynamic programming algorithm for the TWT problem with a constant number of distinct due dates first and then adopt a rounding scheme to obtain an FPTAS. Three major points that we make in this algoritlun are: we observe a series of structural properties of optimal schedules so that we shrink the state space of the DP; we make use of preemption (i.e. allowing the processing of a job to be interrupted and restarted later) for the design of the DP; the rounding scheme that we adopt guarantees that a factor 1 + E of the optimal solution is generated and the algorithm runs within a polynomial time of the problem size.
Dosimetric evaluation of cardiac and left anterior descending artery dose in patients with left-sided breast cancer treated by different techniques of hypofractionated adjuvant radiotherapy after breast conservative surgery

The aims: to dosimetrically evaluate the dose to the heart and left anterior descending artery in left-sided early breast cases using different techniques. Materials and methods: Prospective observational/analytical study done in cases of left-sided BCS referred for adjuvant RT in 54 patients. Patients who underwent left-sided BCS (breast conservative surgery), patients aged between 18- and 75 years performance status ECOG 0-2, histological confirmed DCIS, Invasive Breast Cancer-Stage 1, 2, 3, patients without any evidence of metastatic disease Irrespective of hormonal receptor and HER-2 neu status are included in the study. Results: All the 3 parameters for LAD showed the highest doses with 3DCRT and lowest with VMAT. Thus our study favoured VMAT (p<0.01) as the planning technique to achieve the least doses of LAD. However, for the heart, there was no statistically significant difference between 3DCRT and IMRT (p=0.349) for the average mean dose (Gy). On the other hand, there was a statistically significant difference between 3DCRT Vs VMAT and IMRT Vs VMAT (95 % CI, p<0.01), again favouring VMAT as the choice of planning technique. The average heart max dose(Gy) and average heart V20(%) showed statistically significant benefits with VMAT (p<0.01). There was a statistically significant benefit (p<0.000) with VMAT for both LV parameters. At the same time, there was a statistically significant benefit in terms of ipsilateral lung dose with VMAT(p<0.000), the dose to the right lung, right breast and favoured 3DCRT (p<0.01). PTV95 % (Gy) by 3DCRT, IMRT, and VMAT in our study is 41.01, 41.96, and 41.76, respectively. Though the difference between the 3 techniques seems meagre, there was a statistically significant difference (p<0.012) favouring IMRT. Conclusion: We conclude that using the VMAT technique in radiotherapy for left-sided breast cancer can significantly reduce radiation doses to the heart and LAD, potentially reducing cardiac risk. For all patients, the cardiac doses are considerably decreased for all dose levels without compromising the dose coverage to PTV, which is an advantage over IMRT and 3DCRT
Weak lensing statistics as a probe of Omega and power spectrum

The possibility of detecting weak lensing effects from deep wide field imaging surveys has open new means of probing the large-scale structures of the Universe and measuring cosmological parameters. In this paper we present a systematic study of the expected dependence of the low order moments of the filtered gravitational local convergence with the power spectrum of the density fluctuations and with the cosmological parameters Omega_0 and Lambda. The results show a significant dependence with all these parameters. Though we note that this degeneracy could be partially raised by considering two populations of sources, at different redshifts, computing the third moment is more promising since it is expected, in the quasi-linear regime and for Gaussian initial conditions, to be only $\Omega_0$ dependent (with a slight degeneracy with Lambda) when it is correctly expressed in terms of the second moment. More precisely we show that the variance of the convergence varies approximately as P(k) Omega_0^{1.5} z_s^{1.5}, whereas the skewness varies as Omega_0^{-0.8} z_s^{-1.35}, where P(k) is the projected power spectrum and z_s the redshift of sources. Thus, used jointly they can provide both P(k) and Omega_0. However, the dependence with the redshift of sources is large and could be a major concern for a practical implementation. We have estimated the errors expected for these parameters in realistic scenario and sketched what would be the observational requirements for doing such measurements. A more detailed study of an observational strategy is left for a second paper.
Probing the weak wind phenomenon in Galactic O-type giants

Aims. Analyses of Galactic late O dwarfs (O8-O9.5V stars) raised the “weak wind problem”: spectroscopic mass-loss rates (Ṁ) are up to two orders of magnitude lower than the theoretical values. We investigated the stellar and wind properties of Galactic late O giants (O8-O9.5III stars). These stars have luminosities log (L⋆ ∕ L⊙) ~ 5.2, which is the critical value (onset of weak winds) proposed in the literature. Methods. We performed a spectroscopic analysis of nine O8-O9.5III stars in the ultraviolet (UV) and optical regions using the model atmosphere code CMFGEN. Results. Stellar luminosities were adopted using calibrations from the literature. Overall, our model spectral energy distributions agree well with the observed ones considering parallaxes from the latest Gaia data release (DR2). The effective temperature derived from the UV region agrees well with the ones from the optical. As expected, the analysis of the Hertzsprung–Russell (HR) diagram shows that our sample is more evolved than late O dwarfs. From the UV region, we found Ṁ ~ 10−8 − 10−9M⊙ yr−1 overall. This is lower by ~0.9 − 2.3 dex than predicted values based on the (global) conservation of energy in the wind. The mass-loss rates predicted from first principles, based on the moving reversing layer theory, agree better with our findings, but it fails to match the spectroscopic Ṁ for the most luminous OB stars. The region of log (L⋆ ∕ L⊙) ~ 5.2 is critical for both sets of predictions in comparison with the spectroscopic mass-loss rates. CMFGEN models with the predicted Ṁ (the former one) fail to reproduce the UV wind lines for all the stars of our sample. We reproduce the observed Hα profiles of four objects with our Ṁ derived from the UV. Hence, low Ṁ values (weak winds) are favored to fit the observations (UV + optical), but discrepancies between the UV and Hα diagnostics remain for some objects. Conclusions. Our results indicate weak winds beyond the O8-9.5V class, since the region of log (L⋆ ∕ L⊙) ~ 5.2 is indeed critical to the weak wind phenomenon. Since O8-O9.5III stars are more evolved than O8-9.5V, evolutionary effects do not seem to play a role in the onset of the weak wind phenomenon. These findings support that the Ṁ (for low luminosity O stars) in use in the majority of modern stellar evolution codes must be severely overestimated up to the end of the H-burning phase. Further investigations must evaluate the consequences of weak winds in terms of physical parameters for massive stars (e.g., angular momentum and CNO surface abundances).
Hurricanes and Anomalous Heat in the Caribbean

Co‐occurring hazards present unparalleled challenges to development and disaster recovery. In this study, we investigate the relationship between anomalous heat in the aftermath of tropical cyclones in the eastern Caribbean between 1991 and 2020. We analyze the spatial patterns of anomalous heat index (HI) values for 53 tropical storms and hurricanes using a Lagrangian analysis framework. Furthermore, we analyze temporal patterns of 205 city‐storms pairings. The spatial patterns displayed distinct and statistically significant areas of anomalously warm conditions regardless of the storm intensity classification. Moreover, all 205 city‐storm events had positive HI anomalies following the storms' passage with a maximum of 5°C. The results show that HI anomalies can be high, have a time lag of days, and be observed in locations not directly impacted by the storm. The results have implications for tropical cyclones preparedness, including suggesting that preparedness include informing the public about heat impacts.
Conservation of spin supercurrents in superconductors

We demonstrate that spin supercurrents are conserved upon transmission through a conventional superconductor, even in the presence of spin-dependent scattering by impurities with magnetic moments or spin-orbit coupling. This is fundamentally different from conventional spin currents, which decay in the presence of such scattering, and has important implications for the usage of superconducting materials in spintronics.
The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies

We use integral-field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence of recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10% of their spectra within the SAMI field of view. These -strong (HDS) galaxies (HDSGs) are rare, making up only ∼2% (25/1220) of galaxies with stellar mass > 10. The HDSGs make up a significant fraction of nonpassive cluster galaxies (15%; 17/115) and a smaller fraction (2.0%; 8/387) of the nonpassive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence of star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the HDS signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R200 of the cluster center and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected phase space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that has entered the central 0.5r200,3D cluster region within the last ∼1 Gyr. In the eight of nine cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram pressure stripping on their first passage through the cluster.
TIME MOTION AND PERFORMANCE ANALYSIS IN TANGO DANCE

The aim of this study was to investigate the movement and choreography characteristics between four different quality groups in tango. Thirty-five dance couples competing in an international competition in the adult category were selected for analysis. The total time and average speed in each direction of movement and the number of changes of direction were compared between four different quality groups. The average speed of the movement and choreography path was 1.14 ± 5.1 m/s and 77.56 ± 11.1 m, respectively. Dancers mostly danced in line of dance (LOD) (M = 10.74 ± 5.2 s), diagonal to the center (DC) (M = 9.96 ± 4.5 s), and diagonal to the wall (DW) (M = 8 ± 3.1s). Although no significant differences were found, the time spent dancing in LOD decreased with the more successful quality group. Significant differences between the quality groups were found in the speed of movement in LOD direction (χ2 = 9.4, df = 3, p = 0.024), which decreased with the more successful quality group. Dancers made an average of 26.31 ± 3.4 changes in direction. Statistical differences were found between the quality groups (χ2 = 7.7, df = 3, p = 0.04). This is the first detailed study in tango analyzing the characteristics of movement and choreography. The quality groups differ in the speed of movement in some directions of movement and in the number of changes of direction. The results presented can help choreographers and coaches to adequately design the physical preparation of the dancers, the structure of the choreography and the technical and tactical requirements.
Two-electron bunching in transport through a quantum dot induced by Kondo correlations

We report on noise measurements in a quantum dot in the presence of Kondo correlations. Close to the unitary limit, with the conductance reaching $1.8{e}^{2}∕h$, we observed an average backscattered charge of ${e}^{*}\ensuremath{\sim}5e∕3$, while weakly biasing the quantum dot. This result held to bias voltages up to half the Kondo temperature. Away from the unitary limit, the charge was measured to be $e$ as expected. These results confirm and extend theoretical predictions that suggested that two-electron backscattering processes dominate over single-electron backscattering processes near the unitary limit, with an average backscattered charge ${e}^{*}\ensuremath{\sim}5e∕3$.
Entropies des flots magnétiques

Un champ magnetique assez petit sur une variete riemannienne compacte a courbure strictement negative engendre une perturbation Anosov du flot geodesique. Le rapport des entropies topologiques est encadre numeriquement. L'entropie de la mesure de Liouville admet une estimation a la Osserman-Sarnak. Sur une surface, pour un champ magnetique assez petit et regulier, de moyenne nulle, le flot magnetique peut etre reparametre par l'action du lagrangien. Son entropie topologique ne coincide avec celle de la mesure de Liouville que si le champ magnetique est nul et la courbure de Gauss constante, ce qui renforce un theoreme de Katok connu pour le flot geodesique.
On the cosmological variation of the fine-structure constant

A phenomenological and Newtonian model is proposed to explain the recent observed cosmological variation of the fine-structure constant as an effect of the quantum vacuum, assuming a flat universe with cosmological constant Λ in the cases (ΩM,ΩΛ) equal to (0.3,0.7) and (1,0). Because of the fourth Heisenberg relation, the lifetime of the virtual pairs of the zero-point radiation must depend on the gravitational potential Φ, so that the quantum vacuum changes its density and acquires a relative permittivity different from one. Since the matter was more concentrated in the past, the gravitational potential of all the universe was stronger and the optical density of the vacuum higher, the electron charge being then more renormalized and smaller than now. The model predicts that Δα/α is proportional to {ΩM[a(t)−1 − 1] − 2ΩΛ[a(t)2 − 1]}, a(t) being the scale factor. This agrees with the observations.
Anisotropic Adaptivity and Subgrid Scale Modelling for the Solution of the Neutron Transport Equation with an Emphasis on Shielding Applications

This thesis demonstrates advanced new discretisation and adaptive meshing technologies that improve the accuracy and stability of using finite element discretisations applied to the Boltzmann transport equation (BTE). This equation describes the advective transport of neutral particles such as neutrons and photons within a domain. The BTE is difficult to solve, due to its large phase space (three dimensions of space, two of angle and one each of energy and time) and the presence of non-physical oscillations in many situations. This work explores the use of a finite element method that combines the advantages of the two schemes: the discontinuous and continuous Galerkin methods. The new discretisation uses multiscale (subgrid) finite elements that work locally within each element in the finite element mesh in addition to a global, continuous, formulation. The use of higher order functions that describe the variation of the angular flux over each element is also explored using these subgrid finite element schemes. In addition to the spatial discretisation, methods have also been developed to optimise the finite element mesh in order to reduce resulting errors in the solution over the domain, or locally in situations where there is a goal of specific interest (such as a dose in a detector region). The chapters of this thesis have been structured to be submitted individually for journal publication, and are arranged as follows. Chapter 1 introduces the reader to motivation behind the research contained within this thesis. Chapter 2 introduces the forms of the BTE that are used within this thesis. Chapter 3 provides the methods that are used, together with examples, of the validation and verification of the software that was developed as a result of this work, the transport code RADIANT. Chapter 4 introduces the inner element subgrid scale finite element discretisation of the BTE that forms the basis of the discretisations within RADIANT and explores its convergence and computational times on a set of benchmark problems. Chapter 5 develops the error metrics that are used to optimise the mesh in order
Impact of the built, social, and food environment on long‐term weight loss within a behavioral weight loss intervention

Behavioral weight loss interventions can lead to an average weight loss of 5%–10% of initial body weight, however there is wide individual variability in treatment response. Although built, social, and community food environments can have potential direct and indirect influences on body weight (through their influence on physical activity and energy intake), these environmental factors are rarely considered as predictors of variation in weight loss.