Miracle-dz/UniFAR-FTUs huggingface dataset:
Structural and magnetic properties of lightly doped M-type hexaferrites

Vanadium substituted SrM hexaferrites (SrFe12-xVxO19 with x = 0.2, 0.4) and Eu-substituted BaM hexaferrite (Ba0.8Eu0.2Fe12O19) were prepared by high energy ball milling and sintering at 1200{\deg} C. X-ray diffraction measurements revealed that the V-substituted SrM samples exhibited phase separation resulting in the coexistence of the pure SrM magnetic phase with nonmagnetic Sr3(VO4)2 vanadate and {\alpha}-Fe2O3 iron oxide phase. Also, the Eu-substituted BaM hexaferrite revealed the formation of the pure BaM phase coexisting with {\alpha}-Fe2O3 secondary phase, and Eu-garnet minor phase. Although the magnetic properties of the samples deteriorated with respect to pure hexaferrite properties, the magnetic parameters of the substituted samples were found to be of potential importance for practical applications. Further, the results of the study suggest methods for the preparation of high quality SrM hexaferrites, and hexaferrite/garnet composites.
Fully renormalized stress tensor correlator in flat space

We present a general procedure to renormalize the stress tensor two-point correlation function on a Minkowski background in position space. The method is shown in detail for the case of a free massive scalar field in the standard Minkowski vacuum state, and explicit expressions are given for the counterterms and finite parts, which are in full accordance with earlier results for the massless case. For the general case in position space, only regularized — but not renormalized — results have been obtained previously. After a Fourier transformation to momentum space, we also check agreement with a previous calculation there. We generalize our results to general Hadamard states. Furthermore, the proposed procedure can presumably be generalized to the important case of an inflationary spacetime background, where the transition to momentum space is in general not possible.
Fitting the Density Substructure of the Stellar Halo with MilkyWay@home

We propose and test a method for applying statistical photometric parallax to main-sequence turnoff stars in the Sloan Digital Sky Survey (SDSS). Using simulated data, we show that if our density model is similar to the actual density distribution of our data, we can reliably determine the density model parameters of three major substructures in the Milky Way halo using the computational resources available on MilkyWay@home (a 20-parameter fit). We fit the stellar density in SDSS stripe 19 with a smooth stellar spheroid component and three major streams. One of these streams is consistent with the Sagittarius tidal stream at 21.1 kpc away, one is consistent with the trailing tail of the Sagittarius tidal stream in the north Galactic cap at 48 kpc away, and one is possibly part of the Virgo Overdensity at 6 kpc away. We find the 1σ widths of these three streams to be 1.0 kpc, 17.6 kpc, and 6.1 kpc, respectively. The width of the trailing tail is extremely wide (41 kpc full width at half maximum). This large width could have implications for the shape of the Milky Way dark matter halo. The width of the Virgo Overdensity-like structure is consistent with what we might expect for a “cloudlike” structure; analysis of additional stripes of data are needed to outline the full extent of this structure and confirm its association with the Virgo Overdensity.
Direct Constraints, Flavor Physics, and Flavor Anomalies in Composite Higgs Models

All main concepts of composite Higgs models (CHMs) are discussed at length. In the context of global numerical analyses of two explicit CHMs, direct collider constraints on vector, fermion, and scalar resonances are studied in detail. Two recent anomalies in rare B meson decays are analyzed model independently. A simple CHM is constructed that can explain both anomalies by partially composite left-handed muons. The flavor physics of the minimal fundamental partial compositeness model is studied in detail and its capability of explaining the anomalies is shown.
Cygnus X-3 transition from the ultrasoft to the hard state

Aims:The nature of Cygnus X-3 is still not understood well. This binary system might host a black hole or a neutron star. Recent observations by INTEGRAL have shown that Cygnus X-3 was again in an extremely ultrasoft state. Here we present our analysis of the transition from the ultrasoft state, dominated by blackbody radiation at soft X-rays plus non-thermal emission in the hard X-rays, to the low hard state. Methods: INTEGRAL observed Cyg X-3 six times during three weeks in late May and early June 2007. Data from IBIS/ISGRI and JEM-X1 were analysed to show the spectral transition. Results: During the ultrasoft state, the soft X-ray spectrum is well-described by an absorbed (NH = 1.5 × 1022~cm-2) black body model, whereas the X-ray spectrum above 20 keV appears to be extremely low and hard (Γ ≃ 1.7). During the transition, the radio flux rises to a level of >1~Jy, and the soft X-ray emission drops by a factor of ~3, while the hard X-ray emission rises by a factor of ~14 and becomes steeper (up to Γ = 4). Conclusions: The ultrasoft state apparently precedes the emission of a jet, which is apparent in the radio and hard X-ray domain. Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic and Poland, and with the participation of Russia and the USA.
Education of the future: from post-war reconstruction to EU membership (Ukrainian case study)

The presented article reflects the results of the study of the prospects for the development of Ukrainian education in the postwar period. In particular, the trends due to the situation of full-scale war on the territory of the state and the results of research work on the plan for Ukrainian educational system innovation in accordance with European standards within the broader process of European integration are taken into account. The method of work with focus groups, formed of teachers of different levels of educational institutions on the territory of the country, was applied when conducting this research. In addition, in processing the results of published research, we used the axiomatic method and considered the existing obstacles (the reduction of the number of institutions, funding sources, incoming; the limitation of processes of innovation, digitalization, and development of methodological materials; the new context of professional training of teachers and academic mobility of education applicants) caused by the situation of full-scale war, as a starting point for the further deployment of perspective. The experience of Ukrainian educators in this case is a substrate for the research work, so the selected categories are designed to form a certain structure of the research process. In addition, a comparative approach was involved due to the need to provide predictions about educational trends of the future. In this paper, we present an attempt to reconcile the existing experience of the development of the institution of education in such a context. The result of the development of the presented topic is a model of educational development in Ukraine, which is based on the above-mentioned basis. The presented theoretical model is prognostic and corresponding recommendations require harmonization with the current norms of educational process management.
Isochronous mass measurements of 
Tz=−1fp
-shell nuclei from projectile fragmentation of 
Ni58

Atomic masses of seven $T_z=-1$, $fp$-shell nuclei from $^{44}$V to $^{56}$Cu and two low-lying isomers, $^{44m}$V ($J^\pi=6^+$) and $^{52m}$Co ($J^\pi=2^+$), have been measured with relative precisions of $1-4\times 10^{-7}$ with Isochronous Mass Spectrometry (IMS) at CSRe. The masses of $^{56}$Cu, $^{52g,52m}$Co, and $^{44m}$V were measured for the first time in this experiment. The Mass Excesses ($ME^{\prime}$s) of $^{44}$V, $^{48}$Mn, $^{50}$Fe, and $^{54}$Ni are determined with an order of magnitude improved precision compared to the literature values. $^{52g,52m}$Co and $^{56}$Cu are found to be $370$~keV and $400$~keV more bound, respectively, while $^{44g,44m}$V are $\sim 300$~keV less bound than the extrapolations in the Atomic-Mass Evaluation 2012 (AME$^{\prime}$12). The masses of the four $T_z=-1/2$ nuclei $^{45}$V, $^{47}$Cr, $^{49}$Mn, and $^{51}$Fe are re-determined to be in agreement, within the experimental errors, with the recent JYFLTRAP measurements or with the previous IMS measurements in CSRe. Details of the measurements and data analysis are described, and the impact of the new $ME$ values on different aspects in nuclear structure are investigated and discussed.
Timing Analysis of V404 Cyg during Its Brightest Outburst with INTEGRAL/SPI

The outburst of V404 Cyg during the summer of 2015 reached unparalleled intensities at X-ray and soft gamma-ray energies with fluxes Crab in the 20–50 keV energy band. To date, studies in the hard X-ray/soft gamma-ray energy domain have focused primarily on the energy spectra. In this work, a timing analysis has been performed with INTEGRAL/SPI data in the 20–300 keV energy range for INTEGRAL revolution 1557, which corresponds to the brightest flare of V404 Cyg (on 2015 June 26). The power spectra are fit with broken power-law and multi-Lorentzian models and compared with previously reported results of V404 Cyg flaring activity from 1989 and 2015. Also, we took advantage of the good signal-to-noise ratio obtained above 70 keV to quantify the timing/fast-variability properties of the source as a function of energy. We then point out similarities of V404 Cyg with the black hole transient V4641 Sgr. Like V4641 Sgr, we found that the power spectra of V404 Cyg during high flux periods did not possess the expected flat-top feature typically seen in a hard spectral state. Interpretations are proposed in the framework of the fluctuating-propagation model to explain the observed properties.
Atomic Structure of Domain and Interphase Boundaries in Ferroelectric HfO2

Though ferroelectric HfO2 thin films are now well characterized, little is currently known about their grain substructure. In particular, the formation of domain and phase boundaries requires investigation to better understand phase stabilization, switching, and phase interconversion. Here, scanning transmission electron microscopy is applied to investigate the atomic structure of boundaries in these materials. It is found that orthorhombic/orthorhombic domain walls and coherent orthorhombic/monoclinic interphase boundaries form throughout individual grains. The results inform how interphase boundaries can impose strain conditions that may be key to phase stabilization. Moreover, the atomic structure near interphase boundary walls suggests potential for their mobility under bias, which has been speculated to occur in perovskite morphotropic phase boundary systems by mechanisms similar to domain boundary motion.
Neutron Star Equation of State from the Quark Level in Light of GW170817

The matter state inside neutron stars (NSs) is an exciting problem in astrophysics, nuclear physics, and particle physics. The equation of state (EOS) of NSs plays a crucial role in the present multimessenger astronomy, especially after the event of GW170817. We propose a new NS EOS, “QMF18,” from the quark level, which describes robust observational constraints from a free-space nucleon, nuclear matter saturation, heavy pulsar measurements, and the tidal deformability of the very recent GW170817 observation. For this purpose, we employ the quark mean-field model, which allows us to tune the density dependence of the symmetry energy and effectively study its correlations with the Love number and the tidal deformability. We provide tabulated data for the new EOS and compare it with other recent EOSs from various many-body frameworks.
Site selection for the 3.4 m optical telescope of the Iranian National Observatory

The Results of the site selection campaign conducted for the proposed 3.4m optical telescope of the Iranian National Observatory are reported. During the first 3 years, among 33 nominated regions throughout the country, the potential regions were confined to four provinces, namely, Southern Khorasan located in the East, Kerman in the South East and Qom and Esfahan in the central part by examining the long-term meteorological and geographical parameters. Over the following 3 years, after astro-climate considerations and short-term atmospheric seeing measurements using differential image motion monitor (DIMM) technique were carried out, four candidate sites were selected among these regions. Simultaneous seeing measurements were carried out on the four candidate sites and finally, the Dinava located at the common border of the Esfahan and Qom provinces and Gargash in Kashan region were selected as the most promising sites. Continuous seeing measurements during 23 months yielded a median value of about 1.0" for both sites. The latitude and longitude of the Dinava are 50, 54 E and 34, 09 N, respectively and is situated at an altitude of about 3000 m and about 57 Km direct from Qom towards the south. The latitude and longitude of the Gargash are 51, 19 E and 33, 40 N, respectively and is situated at an altitude of about 3600 m and about 37km direct from Kashan towards the south. With two sites in hand, further comparative measurements of seeing and weather data continued at the two sites, which resulted in the selection of the Gargash site for the construction of the Iranian National Observatory.
Home-Based Exercise to Improve Motor Functions, Cognitive Functions, and Quality of Life in People with Huntington’s Disease: A Systematic Review and Meta-Analysis

Exercise in different settings has become a fundamental part of Huntington’s disease (HD) management. The aim of this systematic review and meta-analysis was to investigate the effectiveness of home-based exercises (HBE) in HD. Randomized controlled trials (RCTs) investigating the effect of HBE on motor, cognitive, or health-related quality of life (QoL) outcomes in HD were included. Standardized mean difference (SMD), the 95% confidence interval, and p-values were calculated by comparing the outcomes change between HBE and control groups. Seven RCTs met the inclusion criteria. The included RCTs prescribed different types of HBEs, i.e., aerobic strengthening, walking, balance, and fine motor exercises. The HBE protocol length was between 6 and 36 weeks. The meta-analyses showed a significant effect of HBE intervention on motor function measure by Unified Huntington Disease Rating and overall QoL measure by Short Form−36 post-treatment respectively, [SMD = 0.481, p = 0.048], [SMD = 0.378, p = 0.003]. The pooled analysis did not detect significant changes in cognition, gait characteristics, or functional balance scales. The current study shows the positive effect of HBE in HD, especially on motor function and QoL. No significant adverse events were reported. The current results support the clinical effect of HBE intervention on motor function and QoL in HD patients. However, these results should be taken with caution due to the limited available evidence. Well-designed clinical studies that consider the disease severity and stages are required in the future.
Boundedness of varieties of Fano type with alpha-invariants and volumes bounded below

We show that fixed dimensional klt weak Fano pairs with alpha-invariants and volumes bounded away from $0$ and the coefficients of the boundaries belong to the set of hyperstandard multiplicities $\Phi(\mathscr{R})$ associated to a fixed finite set $\mathscr{R}$ form a bounded family. We also show $\alpha(X,B)^{d-1}\mathrm{vol}(-(K_X+B))$ are bounded from above for all klt weak Fano pairs $(X,B)$ of a fixed dimension $d$.
X-shooter observations of low-mass stars in the η Chamaeleontis association

The nearby η Chamaeleontis association is a collection of 4–10 Myr old stars with a disk fraction of 35–45%. In this study, the broad wavelength coverage of VLT/X-shooter is used to measure the stellar and mass accretion properties of 15 low-mass stars in the η Chamaeleontis association. For each star, the observed spectrum is fitted with a non-accreting stellar template and an accretion spectrum obtained from assuming a plane-parallel hydrogen slab. Five of the eight stars with an IR disk excess show excess UV emission, indicating ongoing accretion. The accretion rates measured here are similar to those obtained from previous measurements of excess UV emission, but tend to be higher than past measurements from H α modeling. The mass accretion rates are consistent with those of other young star forming regions.
Nonlinearly charged black hole in the theory with nonminimal derivative coupling and its thermodynamics

We have obtained an exact solution for a static black hole in the theory with nonminimal derivative coupling of a scalar field and gravity with a power-law Maxwell field minimally coupled to gravity. Supposing that the black hole might be topological we examined the obtained solution. We also investigated black hole thermodynamics using Wald procedure for calculation of entropy of the black hole.
The Accretion Origin of the Milky Way’s Stellar Halo

We have used data from the Sloan Digital Sky Survey (SDSS) Data Release 5 to explore the overall structure and substructure of the stellar halo of the Milky Way using ~4 million color-selected main-sequence turnoff stars with 0.2 < g − r < 0.4 and 18.5 ⩽ r < 22.5. We fit oblate and triaxial broken power law models to the data, and found a “best-fit” oblateness of the stellar halo 0.5 < c/a < 0.8, and halo stellar masses between galactocentric radii of 1 and 40 kpc of 3.7 ± 1.2 × 108 M☉. The density profile of the stellar halo is approximately ρ ∝ r−α, where –2 > α > − 4. Yet, we found that all smooth and symmetric models were very poor fits to the distribution of stellar halo stars because the data exhibit a great deal of spatial substructure. We quantified deviations from a smooth oblate/triaxial model using the rms of the data around the model profile on scales ≳100 pc, after accounting for the (known) contribution of Poisson uncertainties. Within the DR5 area of the SDSS, the fractional rms deviation σ/total of the actual stellar distribution from any smooth, parameterized halo model is ≳40%: hence, the stellar halo is highly structured. We compared the observations with simulations of galactic stellar halos formed entirely from the accretion of satellites in a cosmological context by analyzing the simulations in the same way as the SDSS data. While the masses, overall profiles, and degree of substructure in the simulated stellar halos show considerable scatter, the properties and degree of substructure in the Milky Way’s halo match well the properties of a “typical” stellar halo built exclusively out of the debris from disrupted satellite galaxies. Our results therefore point toward a picture in which an important fraction of the stellar halo of the Milky Way has been accreted from satellite galaxies.
Almost sure convergence of random projected proximal and subgradient algorithms for distributed nonsmooth convex optimization

Abstract Two distributed algorithms are described that enable all users connected over a network to cooperatively solve the problem of minimizing the sum of all users’ objective functions over the intersection of all users’ constraint sets, where each user has its own private nonsmooth convex objective function and closed convex constraint set, which is the intersection of a number of simple, closed convex sets. One algorithm enables each user to adjust its estimate using the proximity operator of its objective function and the metric projection onto one constraint set randomly selected from a number of simple, closed convex sets. The other determines each user’s estimate using the subdifferential of its objective function instead of the proximity operator. Investigation of the two algorithms’ convergence properties for a diminishing step-size rule revealed that, under certain assumptions, the sequences of all users generated by each of the two algorithms converge almost surely to the same solution. It also showed that the rate of convergence depends on the step size and that a smaller step size results in quicker convergence. The results of numerical evaluation using a nonsmooth convex optimization problem support the convergence analysis and demonstrate the effectiveness of the two algorithms.
New semi-Hamiltonian hierarchy related to integrable magnetic flows on surfaces

We consider magnetic geodesic flows on the two-torus. We prove that the question of existence of polynomial in momenta first integrals on one energy level leads to a semi-Hamiltonian system of quasi-linear equations, i.e. in the hyperbolic regions the system has Riemann invariants and can be written in conservation laws form.
Numerical 3+1 General Relativistic Magnetohydrodynamics: A Local Characteristic Approach

We present a general procedure to solve numerically the general relativistic magnetohydrodynamics (GRMHD) equations within the framework of the 3+1 formalism. The work reported here extends our previous investigation in general relativistic hydrodynamics (Banyuls et al. 1997) where magnetic fields were not considered. The GRMHD equations are written in conservative form to exploit their hyperbolic character in the solution procedure. All theoretical ingredients necessary to build up high-resolution shock-capturing schemes based on the solution of local Riemann problems (i.e., Godunov-type schemes) are described. In particular, we use a renormalized set of regular eigenvectors of the flux Jacobians of the relativistic MHD equations. In addition, the paper describes a procedure based on the equivalence principle of general relativity that allows the use of Riemann solvers designed for special relativistic MHD in GRMHD. Our formulation and numerical methodology are assessed by performing various test simulations recently considered by different authors. These include magnetized shock tubes, spherical accretion onto a Schwarzschild black hole, equatorial accretion onto a Kerr black hole, and magnetized thick disks accreting onto a black hole and subject to the magnetorotational instability.
The Bimodal Galaxy Color Distribution: Dependence on Luminosity and Environment

We analyze the u - r color distribution of 24,346 galaxies with Mr ≤ -18 and z < 0.08, drawn from the Sloan Digital Sky Survey first data release, as a function of luminosity and environment. The color distribution is well fitted with two Gaussian distributions, which we use to divide the sample into a blue and red population. At fixed luminosity, the mean color of the blue (red) distribution is nearly independent of environment, with a weakly significant (~3 σ) detection of a trend for colors to become redder by 0.1-0.14 (0.03-0.06) mag with a factor of ~100 increase in local density, as characterized by the surface density of galaxies within a ±1000 km s-1 redshift slice. In contrast, at fixed luminosity the fraction of galaxies in the red distribution is a strong function of local density, increasing from ~10%-30% of the population in the lowest density environments to ~70% at the highest densities. The strength of this trend is similar for both the brightest (-23 < Mr < -22) and faintest (-19 < Mr < -18) galaxies in our sample. The fraction of red galaxies within the virialized regions of clusters shows no significant dependence on velocity dispersion. Even at the lowest densities explored, a substantial population of red galaxies exists, which might be fossil groups. We propose that most star-forming galaxies today evolve at a rate that is determined primarily by their intrinsic properties and independent of their environment. Any environmentally triggered transformations from blue to red colors must occur either on a short timescale or preferentially at high redshift to preserve the simple Gaussian nature of the color distribution. The mechanism must be effective for both bright and faint galaxies.