Context. The physical conditions in stellar atmospheres, such as temperature, velocity, and magnetic fields, can be obtained by interpreting solar spectro-polarimetric observations. Traditional inversion codes, while successful, are computationally demanding, however, especially for lines whose formation is complex and dictated by nonlocal

The gas-phase metallicity distribution in galaxies offers significant information on their evolution. We report the discovery of negative radial gradients in the gas-phase metallicity of the narrow-line region (NLR) of the nine galaxies in the Measuring Active Galactic Nuclei Under MUSE Microscope (MAGNUM) galaxies: Centaurus A, Circinus, IC 5063

We report the discovery of a new black-widow millisecond pulsar, PSR J1544–2555, associated with the Fermi-Large Area Telescope (LAT) source 4FGL J1544.2–2554. Optical, radio, and gamma-ray observations confirmed its nature as a compact spider binary system. Optical photometry from ULTRACAM revealed a $\sim$2.7-h orbital period, guiding MeerKAT

Context. Modeling the solar atmosphere is challenging due to its layered structure and dynamic multi-scale processes. Aims. We aim to validate the new radiative magnetohydrodynamic (MHD) code MAGEC—built by integrating the MANCHA3D and MAGNUS codes into a finite-volume, shock-capturing framework—and to explore its capabilities through 2D

The Gaia BP/RP spectra provide an excellent opportunity to search for extremely metal-poor (EMP; [M/H] ≤ –3.0) stars. In this study, we assess the potential of our Gaia BP/RP-based candidate catalog, vetting newly identified EMP candidates with higher-resolution follow-up observations. The candidates are selected based on the metallicity derived

We present an independent spectroscopic and radial velocity analysis for nine stars from the Pennsylvania-Toruń Planet Search. For BD+24 4697, we present an updated true companion's mass (0.16±0.02 M☉) as well as evidence of stellar activity. For BD+54 1640 and BD+65 1241 we present true masses of companions, m=0.15±0.04 M☉ and m=0.091± 0.005 M☉