Miracle-dz/UniFAR-FTUs huggingface dataset:
General relativistic simulations of magnetized binary neutron star mergers

Binary neutron stars (NSNS) are expected to be among the leading sources of gravitational waves observable by ground-based laser interferometers and may be the progenitors of short-hard gamma-ray bursts. We present a series of general relativistic NSNS coalescence simulations both for unmagnetized and magnetized stars. We adopt quasiequilibrium initial data for circular, irrotational binaries constructed in the conformal thin-sandwich (CTS) framework. We adopt the BSSN formulation for evolving the metric and a high-resolution shock-capturing scheme to handle the magnetohydrodynamics. Our simulations of unmagnetized binaries agree with the results of Shibata, Taniguchi and Ury\ifmmode \bar{u}\else \={u}\fi{} [M. Shibata, K. Taniguchi, and K. Ury\ifmmode \bar{u}\else \={u}\fi{}, Phys. Rev. D 68, 084020 (2003). ]. In cases in which the mergers result in a prompt collapse to a black hole, we are able to use puncture gauge conditions to extend the evolution and determine the mass of the material that forms a disk. We find that the disk mass is less than 2% of the total mass in all cases studied. We then add a small poloidal magnetic field to the initial configurations and study the subsequent evolution. For cases in which the remnant is a hypermassive neutron star, we see measurable differences in both the amplitude and phase of the gravitational waveforms following the merger. For cases in which the remnant is a black hole surrounded by a disk, the disk mass and the gravitational waveforms are about the same as the unmagnetized cases. Magnetic fields substantially affect the long-term, secular evolution of a hypermassive neutron star (driving ``delayed collapse'') and an accretion disk around a nascent black hole.
Cooperative amplification of energy transfer in plasmonic systems

We study cooperative effects in energy transfer (ET) from an ensemble of donors to an acceptor near a plasmonic nanostructure. We demonstrate that in cooperative regime ET takes place from plasmonic superradiant and subradiant states rather than from individual donors leading to a significant increase of ET efficiency. The cooperative amplification of ET relies on the large coupling of superradiant states to external fields and on the slow decay rate of subradiant states. We show that superradiant and subradiant ET mechanisms are efficient in different energy domains and therefore can be utilized independently. We present numerical results demonstrating the amplification effect for a layer of donors and an acceptor on a spherical plasmonic nanoparticle.
Genome Wide Association Study with Imputed Whole Genome Sequence Data Identifies a 431 kb Risk Haplotype on CFA18 for Congenital Laryngeal Paralysis in Alaskan Sled Dogs

Congenital laryngeal paralysis (CLP) is an inherited disorder that affects the ability of the dog to exercise and precludes it from functioning as a working sled dog. Though CLP is known to occur in Alaskan sled dogs (ASDs) since 1986, the genetic mutation underlying the disease has not been reported. Using a genome-wide association study (GWAS), we identified a 708 kb region on CFA 18 harboring 226 SNPs to be significantly associated with CLP. The significant SNPs explained 47.06% of the heritability of CLP. We narrowed the region to 431 kb through autozygosity mapping and found 18 of the 20 cases to be homozygous for the risk haplotype. Whole genome sequencing of two cases and a control ASD, and comparison with the genome of 657 dogs from various breeds, confirmed the homozygous status of the risk haplotype to be unique to the CLP cases. Most of the dogs that were homozygous for the risk allele had blue eyes. Gene annotation and a gene-based association study showed that the risk haplotype encompasses genes implicated in developmental and neurodegenerative disorders. Pathway analysis showed enrichment of glycoproteins and glycosaminoglycans biosynthesis, which play a key role in repairing damaged nerves. In conclusion, our results suggest an important role for the identified candidate region in CLP.
Ultraluminous X-ray sources: Three exciting years

The extreme extragalactic sources known as Ultraluminous X-ray Sources (ULX) represent a unique testing environment for compact objects population studies and the accretion process. Their nature has long been disputed. Their luminosity, well above the Eddington luminosity for a stellar-mass black hole, can imply the presence of an intermediate-mass black hole or a stellar black hole accreting above the Eddington limit. Both these interpretations are important to understand better the accretion process and the evolution of massive black holes. The last few years have seen a dramatic improvement of our knowledge of these sources. In particular, the super-Eddington interpretation for the bulk of the ULX population has gained a strong consensus. Nonetheless, exceptions to this general trend do exist, and in particular one ULX was shown to be a neutron star, and another was shown to be a very likely IMBH candidate. In this paper, I will review the most relevant results in this field of research in the last few years. (© 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
Type Ia Supernovae and Accretion Induced Collapse

Using the population synthesis binary evolution code StarTrack, we present theoretical rates and delay times of Type Ia supernovae arising from various formation channels. These channels include binaries in which the exploding white dwarf reaches the Chandrasekhar mass limit (DDS, SDS, and helium-rich donor scenario) as well as the sub-Chandrasekhar mass scenario, in which a white dwarf accretes from a helium-rich companion and explodes as a SN Ia before reaching the Chandrasekhar mass limit. We find that using a common envelope parameterization employing energy balance with alpha=1 and lambda=1, the supernova rates per unit mass (born in stars) of sub-Chandrasekhar mass SNe Ia exceed those of all other progenitor channels at epochs t=0.7 - 4 Gyr for a burst of star formation at t=0. Additionally, the delay time distribution of the sub-Chandrasekhar model can be divided in to two distinct evolutionary channels: the `prompt' helium-star channel with delay times 800 Myr spanning up to a Hubble time. These findings are in agreement with recent observationally-derived delay time distributions which predict that a large number of SNe Ia have delay times < 1 Gyr, with a significant fraction having delay times < 500 Myr. We find that the DDS channel is also able to account for the observed rates of SNe Ia. However, detailed simulations of white dwarf mergers have shown that most of these mergers will not lead to SNe Ia but rather to the formation of a neutron star via accretion-induced collapse. If this is true, our standard population synthesis model predicts that the only progenitor channel which can account for the rates of SNe Ia is the sub-Chandrasekhar mass scenario, and none of the other progenitors considered can fully account for the observed rates.
On supercycle lengths of active SU UMa stars

We performed a detailed analysis of extensive photometric observations of a sample of most active dwarf novae, that is SU UMa stars which are characterised by supercycle lengths shorter than 120 days. We found the observational evidence that supercycle lengths for these objects have been constantly increasing over the past decades, which indicates that their mean mass transfer rates have been decreasing during that time. This seems to be a common feature for this type of stars. We present numerical results in each case and estimate time scales of future development of these systems. This study is important in the context of evolution of dwarf novae stars and perhaps other cataclysmic variables.
Dynamo action and magnetic buoyancy in convection simulations with vertical shear

A hypothesis for sunspot formation is the buoyant emergence of magnetic flux tubes created by the strong radial shear at the tachocline. In this scenario, the magnetic field has to exceed a threshold value before it becomes buoyant and emerges through the whole convection zone. We follow the evolution of a random seed magnetic field with the aim of study under what conditions it is possible to excite the dynamo instability and whether the dynamo generated magnetic field becomes buoyantly unstable and emerges to the surface as expected in the flux-tube context. We perform numerical simulations of compressible turbulent convection that include a vertical shear layer. Like the solar tachocline, the shear is located at the interface between convective and stable layers. We find that shear and convection are able to amplify the initial magnetic field and form large-scale elongated magnetic structures. The magnetic field strength depends on several parameters such as the shear amplitude, the thickness and location of the shear layer, and the magnetic Reynolds number ($\Rm$). Whenever the toroidal magnetic field reaches amplitudes greater a threshold value which is close to the equipartition value, it becomes buoyant and rises into the convection zone where it expands and forms mushroom shape structures. Some events of emergence, i.e. those with the largest amplitudes of the initial field, are able to reach the very uppermost layers of the domain. These episodes are able to modify the convective pattern forming either broader convection cells or convective eddies elongated in the direction of the field. However, in none of these events the field preserves its initial structure.
Thermodynamics of the Quark‐Gluon Plasma at Finite Chemical Potential: Color Path Integral Monte Carlo Results

Based on the constituent quasiparticle model of the quark‐gluon plasma (QGP), color quantum path‐integral Monte‐Carlo (PIMC) calculations of the thermodynamic properties of the QGP are performed. We extend our previous zero chemical potential simulations to the QGP at finite baryon chemical potential. The results indicate that color PIMC can be applied not only above the QCD critical temperature Tc but also below Tc. Besides reproducing the lattice equation of state our approach yields also valuable additional insight into the internal structure of the QGP, via the pair distribution functions of the various quasiparticles. In particular, the pair distribution function of gluons reflects the existence of gluon‐gluon bound states at low temperatures and μ = 175 MeV, i.e. glueballs, while meson‐like bound states are not found. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Renormalized entropy solutions of scalar conservation laws.

A scalar conservation law ut +div (u) = f is considered with the initial datum u|t=0 = u0 2 L1 loc(RN) and f 2 L1 loc(RN ×(0, T)) only. In this case the classical Krushkov condition can make no sense because of unboundedness of u, if no growth condition on is assumed. This obstacle is overcome by introducing the so-called renormalized entropy solution generalizing the classical one. Existence and uniqueness of such a solution is established.
On the number-phase problem

The known approaches of number-phase problem (for a quantum oscillator) are mutually contradictory. All of them are subsequent in respect with the Robertson-Schr\"{o}dinger uncertainty relation (RSUR). In oposition here it is proposed a new approacch aimed to be aboriginal as regard RSRUR. From the new perspective the Dirac's operators for vibrational number and phase appear as correct mathematical tools while the alluded problem receives a natural solution. PACS codes: 03.65. -w, 03.65. Ca, 03.65. Fd, 03.65. Ta Keywords: quantum oscillator, number and phase, uncertainty relations.
Implications of Radial Migration for Stellar Population Studies

Recent theoretical work suggests that it may be common for stars in the disks of spiral galaxies to migrate radially across significant distances in the disk. Such migrations are a result of resonant scattering with spiral arms and move the guiding centers of the stars while preserving the circularities of their orbits. Migration can therefore efficiently mix stars in all parts of the Galactic disk. We are rapidly approaching an important confluence of theory and observation, where we may soon be able to uncover signatures of such processes in our own Milky Way. The resolution and robustness of the physical modeling in simulations has improved drastically, while observational datasets are increasing in depth and astrometric accuracy. Here, we discuss the results from our idealized N-body/SPH simulations of disk formation and evolution, emphasizing specifically the observational consequences of stellar migration on the solar neighborhood and the vertical structure of the disk. We demonstrate that radial mixing of stars is a crucial dynamical process that we must try to understand if we are to draw significant conclusions about our Galactic history from the properties of stars in our vicinity.
A novel double-shielding technique for ac quantum Hall measurement

We describe a novel double-shield configuration applied to ac quantum Hall devices which is a very significant advance in that it eliminates the effect of all presently known ac losses. The ac quantum Hall resistance measured in this way is therefore an excellent quantum standard of impedance having a relative uncertainty well below 1 × 10−8.
AN H i SURVEY OF SIX LOCAL GROUP ANALOGS. II. H i PROPERTIES OF GROUP GALAXIES

We have conducted an H i 21 cm emission-line survey of six loose groups of galaxies chosen to be analogs to the Local Group. The survey was conducted using the Parkes multibeam instrument and the Australia Telescope Compact Array (ATCA) over a ∼1 Mpc2 area and covering the full depth of each group, with an MH i sensitivity of ∼7 × 105 M☉. Our survey detected 110 sources, 61 of which are associated with the six groups. All of these sources were confirmed with ATCA observations or were previously cataloged by HIPASS. The sources all have optical counterparts and properties consistent with dwarf irregular or late-type spiral galaxies. We present here the H i properties of the groups and their galaxies. We derive an H i mass function (HIMF) for the groups that is consistent with being flatter than the equivalent field HIMF. We also derive a circular velocity distribution function, tracing the luminous dark matter halos in the groups, that is consistent with those of the Local Group and HIPASS galaxies, both of which are shallower than that of clusters or predictions from cold dark matter models of galaxy formation.
In Vivo Antimalarial Activity of the Leaf Extract of Osyris quadripartita Salzm. ex Decne and Its Major Compound (–) Catechin

Background The leaves of Osyris quadripartita Salzm. ex Decne, endemic to Ethiopia, are traditionally used for the treatment of malaria. Previous phytochemical investigations of Osyris species showed the presence of flavonoids, anthracene derivatives, and sesquiterpene lactones as the main constituents. The aim of the present study was to investigate the antimalarial activity of the leaf extract of O. quadripartita and its isolated constituent against mice infected with Plasmodium berghei. Methods Isolation of a compound was carried out on silica gel column chromatography of the extract eluting with gradient mixtures of CHCl3/MeOH. Structural elucidation of the isolated compound was achieved by ESI-MS and 1D-and 2D-NMR spectral data. Peter's 4-day suppressive test method was used to determine the antimalarial activity of the test substances. Level of parasitemia, survival time, and body weight change were used to determine the antimalarial activity of the test substances. Results (–) Catechin was isolated and characterized from the hydroalcoholic extract of O. quadripartita. At a concentration of 400 mg/kg, both the extract and (–) catechin exhibited antimalarial activity with the highest chemosuppression values of 70.61% and 64.26%, respectively. Conclusion These findings indicate that O. quadripartita is endowed with genuine antimalarial activity attributed in part, to its (–) catechin content. Hence, the present study may validate the traditional use of the plant for the treatment of malaria.
A possible common nature of equatorial half-gyrofrequency VLF emissions and discrete plasmaspheric emissions

Une tentative est realisee de connecter les emissions TBF dans une bande de frequence juste au-dessus de la moitie de la gyrofrequence electronique observees dans la region equatoriale magnetospherique au-dela de la plasmapause et les emissions plasmaspheriques discretes avec une frequence de coupure inferieure proche d'un quart de la gyrofrequence electronique equatoriale, observees sur des satellites a basse altitude dans la plasmasphere
Weighted Adversarial Domain Adaptation for Machine Remaining Useful Life Prediction

In industry, accurate remaining useful life (RUL) prediction is critical in improving system reliability and reducing downtime and accident risk. Numerous deep-learning approaches have been proposed and achieved impressive performance in RUL prediction. Nevertheless, most of them are based on an unrealistic assumption, that is, the training (source) and testing (target) data follow similar distributions. In real-world applications, the source and target domains usually have different data distributions, which degrades the model performance on the unlabeled target domain. Existing adversarial domain adaptive RUL prediction methods fail to consider the label information, which potentially aligns samples with very different semantic information and ultimately leads to negative transfer. To address the above issue, this article proposes a weighted adversarial loss (WAL) for cross-domain RUL prediction. To be specific, WAL utilizes the ground-truth labels of the source domain and the pseudo-labels of the target domain to calculate weight and then obtain the WAL. This proposed loss forces the adversarial model to align samples with similar RULs from the source and target domains. Therefore, WAL can enhance positive transfer while alleviating negative transfer. Extensive experiments demonstrate that the proposed loss can be effectively plugged into existing adversarial domain adaptation methods and yield state-of-the-art results.
Nidificação de Parachartergus pseudapicalis Willink em substrato vegetal (Hymenoptera, Polistinae)

Vespas sociais utilizam diferentes substratos para nidificação, incluindo construções humanas e numerosas espécies vegetais. Trabalhos já foram publicados a respeito da seleção de substratos para nidificação por vespas neotropicais, todavia há poucas informações para a espécie Parachartergus pseudapicalis Willink. No presente trabalho, reportam-se quatro registros de nidificação desta espécie, no domínio de Mata Atlântica, em 2013, 2014 e 2022, no município de Inconfidentes, Minas Gerais. Levou-se em consideração seleção de substrato e coletando-se os indivíduos para identificação das espécies. Não se encontraram padrões de similaridade morfológica entre as espécies vegetais que pudessem evidenciar preferência das vespas, mas sim quando consideradas as ocorrências no contexto da paisagem, de modo que os ninhos se encontravam em áreas de topografia relativamente deprimida e nas proximidades de corpos de água. Portanto, considera-se que a presença de recursos hídricos possa ser a variável de importância para a seleção de substratos para nidificação por P. pseudapicalis.
Food effect risk assessment in preformulation stage using material sparing μFLUX methodology

The intake of food and meal type can strongly impact the bioavailability of orally administered drugs and can consequently impact drug efficacy and safety. During the early stages of drug development, only a small amount of drug substance is available, and the solubility difference between fasted state simulated intestinal fluid and fed state simulated intestinal fluid may provide an early indication about the probable food effect. But higher drug solubility in fed state simulated intestinal fluid may not always results in an increased oral absorption. In the present research, we demonstrated using 11 model compounds that in addition to the drug dissolution in biorelevant media, the evaluation of the diffusion flux of a drug in solution, across artificial lipid coated membrane, where only the unbound drug crosses the membrane, is a reliable way to predict the food effect. Although, the combination of dissolution and diffusion flux may not reliably predict the food effect in case of drugs undergoing intestinal metabolism or when transporters are involved in the drug absorption, the technique generally provides good information about the food effect at very early stages of drug development that may help in designing a clinical plan by adjusting the drug dose in the fed state.
Statistical physics of fracture, friction, and earthquakes

The present status of research and understanding regarding the dynamics and the statistical properties of earthquakes is reviewed, mainly from a statistical physical view point. Emphasis is put both on the physics of friction and fracture, which provides a microscopic basis for our understanding of an earthquake instability, and on the statistical physical modelling of earthquakes, which provides macroscopic aspects of such phenomena. Recent numerical results from several representative models are reviewed, with attention to both their critical and their characteristic properties. Some of the relevant notions and related issues are highlighted, including the origin of power laws often observed in statistical properties of earthquakes, apparently contrasting features of characteristic earthquakes or asperities, the nature of precursory phenomena and nucleation processes, and the origin of slow earthquakes, etc.