We explore the interplay between Jeans analyses of velocity dispersions and millisecond-pulsar (MSP) timing measurements that trace line-of-sight accelerations to analyze the kinematics of Omega Centauri, performing the first combined analysis of its kind. By using HST proper motion data and recent MSP kinematic measurements, we are able to tightly

Current theories of planetary evolution predict that infant giant planets have large radii and very low densities before they slowly contract to reach their final size after about several hundred million years. These theoretical expectations have remained untested for a long time, as the detection and characterization of very young planets is

The completeness of stellar spectral libraries in all stellar evolutionary phases, parameter space (effective temperature, surface gravity, global metallicity) and chemical abundances, is required to build more sophisticated stellar population synthesis models to decode the enclosed information of galaxies of varying types. On the hand, due to

Context. In our previous work, we derived the CR-IGIMF, which is a new scenario for a variable stellar initial mass function (IMF) that combines numerical results on the role played by cosmic rays (CR) in setting the thermal state of star-forming gas with the analytical approach of the integrated galaxy-wide IMF (IGIMF). Aims: In this work, we

The nearby LHS 1678 (TOI-696) system contains two confirmed planets and a wide-orbit, likely brown-dwarf companion, which orbit an M2 dwarf with a unique evolutionary history. The host star occupies a narrow "gap" in the Hertzsprung–Russell diagram lower main sequence, associated with the M dwarf fully convective boundary and long-term luminosity

We analyse the spatial distribution and vertical stratification of the physical parameters of the solar atmosphere when an X-class flare occurs. We made use of observations acquired by the Interferometric Bidimensional Spectropolarimeter instrument when observing the full Stokes parameters for the Fe I 6173 Å and Ca II 8542 Å transitions. We