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Our study aims to elucidate both short-term and long-term variations in the light curve of the eclipsing system OGLE-LMC-ECL-14413, with a particular focus on the unusual reversals in eclipse depth. We aim to clarify the role of the accretion disk in these fluctuations, especially in long-cycle changes spanning hundreds of days. Additionally, we seek to determine the evolutionary stage of the system and gain insights into the internal structure of its stellar components. We analyzed photometric time series from the Optical Gravitational Lensing Experiment (OGLE) project in the I and V bands, and from the MAssive Compact Halo Objects project in the BM and RM bands, covering a period of 30.85 years. Using light curve data from 27 epochs, we constructed models of the accretion disk. An optimized simplex algorithm was employed to solve the inverse problem, deriving the best-fit parameters for the stars, orbit, and disk. We also utilized the Modules for Experiments in Stellar Astrophysics software to assess the evolutionary stage of the binary system, investigating the progenitors and potential future developments. We found an orbital period of 38.15917(54) d and a long-term cycle of approximately 780 d. Temperature, mass, radius, and surface gravity values were determined for both stars. The photometric orbital cycle and the long-term cycle are consistent with a disk containing variable physical properties, including two shock regions. The disk encircles the more massive star and the system brightness variations align with the long-term cycle at orbital phase 0.25. Our mass transfer rate calculations correspond to these brightness changes. \texttt{MESA} simulations indicate weak magnetic fields in the donor star's subsurface, which are insufficient to influence mass transfer rates significantly., Comment: 16 pages, 18 figures plus 3 figures in Zenodo. Accepted for publication in Astronomy and Astrophysics main journal

Context. The eclipsing close binary UU Cas is an interacting massive double-periodic system with a gainer star partly hidden in an accretion disk. Aims. In order to study the physics of the accretion process in greater detail, along with the structure and dynamics of the circumstellar matter in the system, we supplement our previous results obtained from photometry with an analysis of the spectra of UU Cas. Methods. We collected all available spectra used in previous publications on UU Cas and we acquired new ones. The method of disentangling was applied to this set of spectra spanning the years 2008-2021. The orbital parameters were disentangled and a fit of the separated component spectra by synthetic ones has been used to determine the physical parameters of the component stars. We compared the results to models of the evolution of interacting binaries. Results. We found that in addition to the dominant role of the donor star and a weak contribution of the gainer, the line profiles are strongly influenced by the circumstellar matter. The absorption lines reveal a presence of a disk wind emanating above the orbital plane. The variability of H{\alpha} emission yields evidence of changes in the structure of the circumstellar matter on a timescale of several orbital periods.

We present the results of the study of the close binary UU Cassiopeiae based on previously published multi wavelength photometric and spectroscopic data. Based on eclipse timings of the last 117 years, we find an improved orbital period of $\rm P_{o} = 8.519296(8)$ d. In addition, we find a long cycle of length $T$ $\sim$ 270 d in the $I_c$-band data. There is no evidence for orbital period change during the last century, suggesting that the rate of mass loss from the system or mass exchange between the stars should be small. Sporadic and rapid brightness drops of up to $\Delta$$V$ = 0.3 mag are detected during the whole orbital cycle and infrared photometry clearly suggests the presence of circumstellar matter. We model the orbital light curve of 11 published datasets fixing the mass ratio and cool star temperature from previous spectroscopic work; $q$= 0.52 and $T_c$= 22 700 K. We find a system seen at angle 74 degrees with a stellar separation of 52 ${\rm R_{\odot}}$, a temperature for the hotter star $T_h$= 30 200 $K$ and stellar masses 17.4 and 9 ${\rm M_{\odot}}$ , radii 7.0 and 16.9 ${\rm R_{\odot}}$ and surface gravities log g = 3.98 and 2.94, for the hotter and cooler star, respectively. We find an accretion disk surrounding the more massive star, with a radius of 21 ${\rm R_{\odot}}$ and vertical thickness in its outer edge of 6.5 ${\rm R_{\odot}}$, mostly occulting the hotter star. Two active regions hotter than the surrounding disk are found, one located roughly in the expected position where the stream impacts the disk and the other one in the opposite side of the disk. Changes are observed in parameters of the disk and spots in different datasets., Comment: Accepted for publication in Astronomy and Astrophysics, 10 pages, 11 figures

The subtype of hot algol semidetached binaries dubbed Double Periodic Variables (DPVs) are characterized by a photometric cycle longer than the orbital one, whose nature has been related to a magnetic dynamo in the donor component controlling the mass transfer rate. We aim to understand the morphologic changes observed in the light curve of OGLE-BLG-ECL-157529 that are linked to the long cycle. In particular, we want to explain the changes in relative depth of primary and secondary eclipses. We analyze $I$ and $V$-band OGLE photometric times series spanning 18.5 years and model the orbital light curve. We find that OGLE-BLG-ECL-157529 is a new eclipsing Galactic DPV of orbital period 24\fd8, and that its long cycle length decreases in amplitude and length during the time baseline. We show that the changes of the orbital light curve can be reproduced considering an accretion disk of variable thickness and radius, surrounding the hottest stellar component. Our models indicate changes in the temperatures of hot spot and bright spot during the long cycle, and also in the position of the bright spot. This, along with the changes in disk radius might indicate a variable mass transfer in this system., Comment: 8 pages, 14 figures, 2 tables, accepted for publication in Astronomy and Astrophysics

The ground state of the U-Mo system is studied in this work using an evolutionary algorithm coupled with \textit{ab initio} calculations. This methodology is applied to several compositions, with a more detailed examination at the U-rich side. A new ground state is identified within an approach that considers structures for up to 3 formula units per cell. A supercell scheme based on the pure phase structure of each element is used for dilute compositions. The ground state at a pressure of 1 atm. is characterized by only two stable compounds: $\Omega$-phase and a new phase, named $\alpha$-U$_{15}$Mo in this work, with a structure determined by adding a substitutional Mo impurity to a $1\times 2\times 2$ supercell of $\alpha$-U. A range of immiscibility of U in bcc-Mo based structures is extended from 0 to nearby 50 at. \% of U. The new $\alpha$-U$_{15}$Mo phase comprising the ground state has similar features to those of the $\alpha'$-phase formed in quenched samples at room temperature. The internal relaxation of U atoms in this phase resembles the movements due to charge density waves observed in orthorhombic $\alpha_1$-U. The ground state of the U$_{15}$Mo compound at T=0 K can not be fully identified due to the charge density wave associated with $\alpha$-U. That structure could be a supercell based on the structurally undefined $\alpha_3$-U phase., Comment: 8 pages, 6 figures (15 individual figures)

Antiferromagnets (AFs) are remarkable magnetically ordered materials that due to the absence of a net magnetic moment do not generate dipolar fields and are insensitive to external magnetic field perturbations. However, it has been notoriously difficult to control antiferromagnetic moments by any practical means suitable for device applications. This has left AFs over their hundred years history virtually unexploited and only poorly explored, in striking contrast to the thousands of years of fascination and utility of ferromagnetism. Very recently it has been predicted and experimentally confirmed that relativistic spin-orbit torques can provide the means for efficient electrical control of an AF. Here we place the emerging field of antiferromagnetic spintronics on the map of non-volatile solid state memory technologies. We demonstrate the complete write/store/read functionality in an antiferromagnetic CuMnAs bit cell embedded in a standard printed circuit board communicating with a computer via a USB interface. We show that the elementary-shape bit cells fabricated from a single-layer AF are electrically written on timescales ranging from milliseconds to nanoseconds and we demonstrate their deterministic multi-level switching. The multi-level cell characteristics, reflecting series of reproducible, electrically controlled domain reconfigurations, allow us to integrate memory and signal counter functionalities within the bit cell., Comment: 13 pages, 3 figures

Using ab initio calculations, unexpected structural instability was recently found in the ground state of the U$_2$Mo compound. Instead of the unstable $I4/mmm$ structure, in this work the $P6/mmm$ ($\# 191$) space group, usually called $\Omega$-phase, is proposed as the fundamental state. Electronic and elastic properties are studied in this work in order to characterize the physical properties of the new ground state. The stability of the $\Omega$-phase is studied by means of its elastic constants calculation and phonon dispersion spectrum. Analysis of isotropic indices shows that the new phase is a ductile material with a minimal degree of anisotropy, suggesting that U$_2$Mo in the $P6/mmm$ structure is an elastic isotropic material. Analysis of charge density, density of electronic states (DOS) and the character of the bands revealed a high level of hybridization between $d$-molybdenum electronic states and $d$- and $f$-uranium ones., Comment: 10 pages, 19 figures