Miracle-dz/UniFAR-FTUs huggingface dataset:
Measurements of branching fraction ratios and CP asymmetries in B{sup {+-}{yields}D}{sub CP}K{sup {+-}}decays in hadron collisions

We reconstruct B{sup {+-}{yields}D}K{sup {+-}}decays in a data sample collected by the CDF II detector at the Tevatron collider corresponding to 1 fb{sup -1} of integrated luminosity. We select decay modes where the D meson decays to either K{sup -{pi}+} (flavor eigenstate) or K{sup -}K{sup +}, {pi}{sup -{pi}+} (CP-even eigenstates), and measure the direct CP asymmetry A{sub CP+}=0.39{+-}0.17(stat){+-}0.04(syst), and the double ratio of CP-even to flavor eigenstate branching fractions R{sub CP+}=1.30{+-}0.24(stat){+-}0.12(syst). These measurements will improve the determination of the Cabibbo-Kobayashi-Maskawa angle {gamma}. They are performed here for the first time using data from hadron collisions.
Solving One-Electron Systems in a Novel Gaussian-Sinc Mixed Basis Set

A novel Gaussian-Sinc mixed basis set for the calculation of the one-electron electronic structure within a uniform magnetic field in three dimensions is presented. The one-electron system is used to demonstrate the utility of this new methodology and is a first step in laying the foundation for further development of many-electron atomic and molecular methodology. It is shown in this manuscript how to effectively calculate all basis set integrals, which includes the mixed Gaussian-Sinc integrals, with a fast and accurate method. The Sinc basis is invariant to the choice of the position of the Coulomb potential, as opposed to traditional grid based methods. This invariance guarantees that the choice of the grids origin has no effect on the electronic structure calculation. This is because the Coulomb potential is treated properly in this methodology, as opposed to DVR methodologies. The off-diagonal terms are sparse but very important around the Coulomb singularity. In general, five to six significant digits of accuracy on all converged results without the linear dependency problems of the Gaussian methodologies are achievable. This methodology is applied to calculate the ground state energy of H atom, $H_2^{+}$ ion and $H_3^{2+}$ ion in magnetic fields up to a magnetic field strength of 2.35x$10^13$ G (10,000 au). From these calculations it is shown that $H_3^{2+}$ ion is unstable without relativistic considerations.
Galaxy Clusters in the Context of Superfluid Dark Matter

It has recently been proposed, by assuming that dark matter is a superfluid, that MOND-like effects can be achieved on small scales whilst preserving the success of $\Lambda$CDM on large scales. Here we aim to provide the first set of spherical models of galaxy clusters in the context of superfluid dark matter. We first outline the theoretical structure of the superfluid core and the surrounding "normal phase" dark halo of quasi-particles in thermal equlibrium. The latter should encompass the largest part of galaxy clusters. Here, we set the SfDM transition at the radius where the density and pressure of the superfluid and normal phase coincides, neglecting the effect of phonons in the suprefluid core. We then apply the theory to a sample of galaxy clusters, and directly compare the SfDM predicted mass profiles to data. We find that the superfluid formulation can reproduce the X-ray dynamical mass profile of clusters. The SfDM fits however display slight under-predictions of the gravity in the central regions which might be partly related to our neglecting of the effect of phonons in these regions. We conclude that this superfluid formulation is successful in describing galaxy clusters, but further work will be needed to determine whether the parameter choice is consistent with galaxies. Our model could be made more realistic by exploring non-sphericity and the SfDM transition condition we impose.
Gauge Invariant Extension of Linearized Horava Gravity

In the present paper we have constructed a gauge invariant extension of a generic Horava Gravity (HG) model (with quadratic curvature terms) in linearized version in a systematic procedure. No additional fields are introduced. The linearized HG model is explicitly shown to be a gauge fixed version of the Einstein Gravity (EG) thus proving the Bellorin-Restuccia conjecture in a robust way. In the process we have explicitly computed the correct Hamiltonian dynamics using Dirac Brackets appearing from the Second Class Constraints present in the HG model. We comment on applying this scheme to the full non-linear HG.
Formation of Supermassive Black Hole Seeds

Abstract The detection of quasars at z > 6 unveils the presence of supermassive black holes of a few billion solar masses. The rapid formation process of these extreme objects remains a fascinating and open issue. Such discovery implies that seed black holes must have formed early on, and grown via either rapid accretion or BH/galaxy mergers. In this theoretical review, we discuss in detail various BH seed formation mechanisms and the physical processes at play during their assembly. We discuss the three most popular BH formation scenarios, involving the (i) core-collapse of massive stars, (ii) dynamical evolution of dense nuclear star clusters, (iii) collapse of a protogalactic metal free gas cloud. This article aims at giving a broad introduction and an overview of the most advanced research in the field.
CONSTRAINTS ON THE MINIMUM ELECTRON LORENTZ FACTOR AND MATTER CONTENT OF JETS FOR A SAMPLE OF BRIGHT FERMI BLAZARS

We fit (quasi-)simultaneous multi-waveband spectral energy distributions for a sample of low-synchrotron-peaked (LSP) blazars with a one-zone leptonic model. The seed photons that predominantly come from the broad line region (BLR) and infrared (IR) molecular torus are considered in the context of an external Compton process. We find that modeling with IR seed photons is systematically better than that with BLR photons based on a χ2 test, which suggests that γ-ray-emitting regions are most likely found outside the BLR. The minimum electron Lorentz factor, γmin, is constrained from the modeling of these LSP blazars with good soft X-ray data (ranging from 5 to 160 with a median value of 55), which plays a key role in jet power estimation. Assuming a one-to-one ratio of protons to electrons, we find that the jet power for LSP blazars is systematically higher than that of FR II radio galaxies at a 151 MHz radio luminosity, L151 MHz even though FR IIs are regarded as the same as LSP blazars in a unification scheme except at the jet viewing angle. A possible reason for this is that there are some e± pairs in the jets of these blazars. If this is the case, we find that the number density of e± pairs should be several times higher than that of e−–p pairs by assuming the jet power is the same for LSP blazars and FR IIs at the given L151 MHz.
Normal state pair nematicity and hidden magnetic order and metal-insulator (fermion-boson)- crossover origin of pseudogap phase of cuprates II

In the present paper II, we will gain an understanding of the nematicity, insulating ground state (IGS), nematicity to stripe phase transition, Fermi pockets evolution, and resistivity temperature upturn, as to be metal - insulator (fermion-boson)- crossover (MIC) phenomena for the pseudogap (PG) region of cuprates. While in the paper I [1], we obtained an understanding of the observed heat conductivity downturn, anomalous Lorentz ratio, insulator resistivity boundary, nonlinear entropy as manifestations of the same MIC. The recently observed nematicity and hidden magnetic order are related to the PG pair intra charge and spin fluctuations. We will try to obtain an answer on the question: why ground state of YBCO is Fermi liquid oscillating and of Bi-2212 is insulating? We will also clarify the physics of the recently observed MIC results of Laliberte et al. [2] and explain the long-discussed transition of the electric charge density from doping to doping+1 dependence at the critical doping. We predict that at the upturns this density should have the temperature dependence $n\sim T^3n_2$ for $T\rightarrow 0$, where $n_2$ is density for dopings close to the critical value. We understood that the upturns before and after the first critical doping have the same nature. We will find understanding of all above mentioned phenomena within the PG pair physics.
Manufacturing offshoring and reshoring in Poland. Evidence from the fashion and electromechanical meta-sectors

After decades of offshoring, in recent years, companies have sometimes revised their location decisions implementing one of the three alternatives of the so-called ? relocations of the second degree? More specifically, they have relocated manufacturing activities either in their home country (back-shoring), in their home region (near-shoring), or in a further away location (further offshoring). While offshoring and relocations of the second degree have been heavily analysed in US and Western European countries, there is no evidence regarding companies in Central and Eastern Europe. This paper focuses on Polish companies belonging to the fashion and electromechanical meta-sectors. More specifically, it investigates the relocation of both manufacturing and supply activities. Based on 602 questionnaires collected during 2020-2021, it emerges that Polish companies rarely offshored their production activities in both the investigated industries. This is mainly explained by concerns in terms of reduced responsiveness, higher coordination and quality appraisal costs, and patriotism. Finally, some differences emerged in terms of geographical location between the two meta-sectors, inducing speculation that fashion companies were mainly boosted by efficiency-seeking aims, while electro-mechanical companies by market-seeking aims. Due to scant evidence of offshoring strategies, relocations of the second degree are very few. However, differences emerge between the two investigated meta-sectors. More specifically, when considering ? relocations of the second degree? , fashion companies preferred to back-shore, while electromechanical companies decided to relocate to a second host country.
Evaluation of mustard genotypes [Brassica juncea (L.) Czern and Coss] for quantitative traits and character association of seed yield and yield components at sub Himalayan region of West Bengal (India)

Brassica juncea is an important industrial and commercial oilseed crop grown primarily in India. This study aimed to assess 56 genotypes of Indian mustard to quantify genetic diversity, which aids the breeder in identifying genetically divergent parents to evaluate the proportional contributions of various components towards overall divergence. All the 56 Indian mustard genotypes were tested in RBD with three replications for 2 consecutive years i.e. 2016-17 and 2017-18 during the rabi season. Observations were recorded for 11 yield and its attributing traits. The findings revealed that height up to first branching, aphid count, penetration force and seed yield per plant had maximum PCV and GCV signifying that genetic factors have a greater impact on the inflow of these traits. Height up to first branching, secondary branches per plant, primary branches per plant, siliquae per plant, aphid count and 1000 seed weight had strong heritability combined with GA as % of mean. These indicate that the traits were controlled by additive gene action. Seed yield per plant was significantly correlated with penetration force and siliquae per plant. As a result, it's reasonable to predict that improving these traits by selection, could lead to significant yield gains. Four of the eleven PCs had eigen values greater than 1.0, accounting for 69.94% of the variance. PC I, which explained 30.31% of the overall variance. Mahalanobis D2 statistics revealed considerable genetic diversity among the genotypes. 56 genotypes were distributed into 7 clusters. This is anticipated that genotypes within a cluster are almost genetically related to one another. Cluster VII and II showed maximum inter-cluster divergence. From a breeding perspective, a divergence analysis revealed that genotypes like SKJM-05, RNWR-09-3, RW-351, B-85, DRMR-4001, RGN-386, TM52 276 and SKM-1313 can be selected as genetically divergent parents for hybridization to obtain desirable segregants.
SWIFT STUDY OF THE FIRST SOFT γ-RAY REPEATER LIKE BURST FROM AXP 1E 1841–045 IN SNR Kes 73

We report the study of the short (32 ms) and first soft γ-ray repeater like burst observed from the anomalous X-ray pulsar (AXP) 1E 1841–045 associated with the supernova remnant Kes 73, discovered on 2010 May 6 by the Burst Alert Telescope on board the Swift γ-ray observatory. The 15–100 keV time-averaged burst spectrum is modeled by a single power law (PL) with a photon index Γ = 3.2+1.8−1.0 and has a fluence of 1.1+0.4−0.6 × 10−8 erg cm−2, a luminosity of 2.9+1.1−1.6 × 1039 erg s−1, and an energy of 7.2+0.4−0.6 × 1036 erg. The prompt after-burst 0.5–10 keV quiescent spectrum obtained with the Swift X-ray Telescope (XRT) is best fit by an absorbed PL model with Γ = 2.6 ± 0.2 and an unabsorbed flux of 9.1+1.2−1.4 × 10−11 erg cm−2 s−1. To investigate the pre-burst 0.5–10 keV persistent emission, we analyzed the archival XMM-Newton observations, and the spectra are well fitted by a two-component blackbody plus PL model with a temperature kT = 0.45 ± 0.03 keV, Γ = 1.9 ± 0.2, and an unabsorbed flux of 4.3+0.9−1.2 × 10−11 erg cm−2 s−1. Comparing the Swift-XRT spectrum with the XMM-Newton spectrum, spectral softening post-burst is evident with a 2.1 times increase in the unabsorbed flux. We discuss the burst activity and the persistent emission properties of AXP 1E 1841–045 in comparison with other magnetars and in the context of the magnetar model.
The Hamburg/ESO R-process Enhanced Star survey (HERES) : VII. Thorium abundances in metal-poor stars

We report thorium abundances for 77 metal-poor stars in the metallicity range of -3.5 < [Fe/H] < -1.0, based on "snapshot" spectra obtained with VLT-UT2/UVES during the HERES Survey. We were able to determine the thorium abundances with better than 1 sigma confidence for 17 stars, while for 60 stars we derived upper limits. For five stars common with previous studies, our results were in good agreement with the literature results. The thorium abundances span a wide range of about 4.0 dex, and scatter exists in the distribution of log (Th/Eu) ratios for lower metallicity stars, supporting previous studies suggesting the r-process is not universal. We derived ages from the log (Th/Eu) ratios for 12 stars, resulting in large scattered ages, and two stars with significant enhancement of Th relative to Eu are found, indicating the "actinide boost" does not seem to be a rare phenomenon and thus highlighting the risk in using log (Th/Eu) to derive stellar ages.
The intergalactic medium over the last 10 billion years - II. Metal-line absorption and physical conditions: Metal-line absorption and physical conditions

We investigate the metallicity evolution and content of the intergalactic medium (IGM) and galactic halo gas from z=2->0 using 110-million particle cosmological hydrodynamic simulations. We focus on the detectability and physical properties of UV resonance metal-line absorbers observable with Hubble's Cosmic Origins Spectrograph (COS). We confirm that galactic superwind outflows are required to enrich the IGM to observed levels down to z=0 using three wind prescriptions contrasted to a no-wind simulation. Our favoured momentum-conserved wind prescription deposits metals closer to galaxies owing to its moderate energy input, while the more energetic constant wind model enriches the warm-hot IGM 6.4x more. Despite these significant differences, all wind models produce metal-line statistics within a factor of two of existing observations. This is because OVI, CIV, SiIV, and NeVIII absorbers primarily arise from T<10^5 K, photo-ionised gas that is enriched to similar levels in the three feedback schemes. OVI absorbers trace the diffuse phase with delta<100, which is enriched to ~1/50 Zsol at z=0, although the absorbers themselves usually exceed 0.3 Zsol and arise from inhomogeneously distributed, un-mixed winds. CIV and SiIV absorbers trace primarily T~10^4 K gas inside haloes. We predict COS will observe a population of NeVIII photo-ionised absorbers tracing T<10^5 K, delta~10 gas. MgX and SiXII are rarely detected in COS S/N=30 simulated sight lines although detections trace T=10^(6-7) K halo gas. In general, the IGM is enriched in an outside-in manner, where wind-blown metals released at higher redshift reach lower overdensities, resulting in higher ionisation species tracing lower-density, older metals. At z=0, the 90% of baryons outside of galaxies are enriched to 0.096 Zsol, but the 65% of unbound baryons in the IGM have 0.018 Zsol and contain only 4% of all metals.
Holographic Superconducting Quantum Interference Device

We present a holographic model of the SQUID (Superconducting QUantum Interference Device) in the external magnetic field. The model of the gravitational theory considered in this paper is the Einstein-Maxwell-complex scalar model on the four-dimensional Anti-de Sitter Schwarzschild black brane geometry, where one space direction is compacted into a circle and we arrange the coefficient of the time components profile so that we can model the SQUID, where the profile plays the role of the chemical potential for the cooper pair.
Consistent metallicity scale for cool dwarfs and giants. A benchmark test using the Hyades

In several instances chemical abundances of dwarf and giant stars are used simultaneously under the assumption that they share the same abundance scale. This assumption might have implications in different astrophysical contexts. We aim to ascertain a methodology capable of producing a consistent metallicity scale for giants and dwarfs. To achieve that, we analyzed giants and dwarfs in the Hyades open cluster. All these stars have archival high-resolution spectroscopic data obtained with HARPS and UVES. In addition, the giants have interferometric measurements of the angular diameters. We analyzed the sample with two methods. The first method constrains the atmospheric parameters independently from spectroscopy. For that we present a novel calibration of microturbulence based on 3D model atmospheres. The second method is the classical spectroscopic based on Fe lines. We also tested two line lists in an attempt to minimize possible non-LTE effects and to optimize the treatment of the giants. We show that it is possible to obtain a consistent metallicity scale between dwarfs and giants. The preferred method should constrain the three parameters $T_{\rm eff}$, $\log~g$, and $\xi$ independent of spectroscopy. In particular, the lines should be chosen to be free of blends in the spectra of giants. When attention is paid to the line list, the classical spectroscopic method can also produce consistent results. The metallicities derived with the well-constrained set of stellar parameters are consistent independent of the line list used. Therefore, for this cluster we favor the metallicity of +0.18$\pm$0.03 dex obtained with this method. The classical spectroscopic analysis, using the line list optimized for the giants, provides a metallicity of +0.14$\pm$0.03 dex, in agreement with previous works.
Strange quark matter in strong magnetic fields within a confining model

model. The confinement is modeled by means of the Richardson potential for quark-quark interaction modified suitably to account for a strong magnetic field. We compare our results for the equation of state and magnetization of matter to those derived within the MIT bag model. The differences between these models arise mainly due to the momentum dependence of the strong interaction between quarks in the Richardson model. Specifically, we find that the magnetization of strange quark matter in this model �
Non-Hermitian interferometer: Unidirectional amplification without distortion

A non-Hermitian interferometer can realize asymmetric transmission in the presence of imaginary potential and magnetic flux. Here, we propose a non-Hermitian dimer with an unequal hopping rate by an interferometer-like cluster in the framework of tight-binding model. The intriguing features of this design are the wave-vector independence and unidirectionality of scattering, which amplifies wavepacket without distortion and absorbs incoherent wave without reflection. The absorption relates to the system spectral singularities, the dynamical behaviors of the spectral singularities are also investigated analytically and numerically.
Calibrating the α parameter of convective efficiency using observed stellar properties

Context. Synthetic model atmosphere calculations are still the most commonly used tool when determining precise stellar parameters and stellar chemical compositions. Besides three-dimensional models that consistently solve for hydrodynamic processes, onedimensional models that use an approximation for convective energy transport play the major role. Aims. We use modern Balmer-line formation theory as well as spectral energy distribution (SED) measurements for the Sun and Procyon to calibrate the model parameter that describes the e ciency of convection in our 1D models. Convection was calibrated over a significant range in parameter space, reaching from F-K along the main sequence and sampling the turno and giant branch over a wide range of metallicities. This calibration was compared to theoretical evaluations and allowed an accurate modeling of stellar atmospheres. Methods. We used Balmer-line fitting and SED fits to determine the convective e ciency parameter . Both methods are sensitive to the structure and temperature stratification of the deeper photosphere. Results. While SED fits do not allow a precise determination of the convective parameter for the Sun and Procyon, they both favor values significantly higher than 1.0. Balmer-line fitting, which we find to be more sensitive, suggests that the convective e ciency parameter is 2.0 for the main sequence and quickly decreases to 1.0 for evolved stars. These results are highly consistent with predictions from 3D models. While the values on the main sequence fit predictions very well, measurements suggest that the decrease of convective e ciency as stars evolve to the giant branch is more dramatic than predicted by models.
Effects of radiative transfer on the structure of self-gravitating discs, their fragmentation and the evolution of the fragments

We investigate structure of self-gravitating disks, their fragmentation and evolution of the fragments (the clumps) using both analytic approach and three-dimensional radiation hydrodynamics simulations starting from molecular cores. The simulations show that non-local radiative transfer determines disk temperature. We find the disk structure is well described by an analytical model of quasi-steady self-gravitating disk with radial radiative transfer. Because the radiative process is not local and radiation from the interstellar medium cannot be ignored, the local radiative cooling would not be balanced with the viscous heating in a massive disk around a low mass star. In our simulations, there are cases in which the disk does not fragment even though it satisfies the fragmentation criterion based on disk cooling time (Q � 1 and tcool � 1). This indicates that at least the criterion is not sufficient condition for fragmentation. We determine the parameter range for the host cloud core in which disk fragmentation occurs. In addition, we show that the temperature evolution of the center of the clump is close to that of typical first cores and the minimum initial mass of clumps to be about a few Jupiter mass.