During the early stages of planetary formation, planets undergo strong changes in their physical and orbital properties due to internal and external forces, which also affect their primordial atmospheres composed mainly of H and He. The study of planets in these early stages and their comparison with the more mature planet population is crucial for

Dwarf irregular galaxies, due to their lower masses, relative isolation, and high-quality data availability, are ideal laboratories to test various models of dark matter. In particular, the existence, morphology and formation of central cores in dwarf galaxies has been a contentious issue in the literature in light of apparent tensions with the

Asteroids (162173) Ryugu and (101955) Bennu observed by Hayabusa2 and Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) share many global properties, but high-spatial-resolution spectral observations by the telescopic Optical Navigation Camera (ONC-T) and MapCam detected subtle but significant

Context. Inferences of the magnetic field in the solar atmosphere by means of spectropolarimetric inversions (i.e., Stokes inversion codes) yield magnetic fields that are non-solenoidal (∇ ⋅ B ≠ 0). Because of this, results obtained by such methods are sometimes put into question. Aims: We aim to develop and implement a new technique that, in

Over the past decade, microlensing surveys in field stars and the Gaia-informed census of nearby star-forming regions have convincingly demonsrated the presence of a significant population of free-floating planetary-mass objects. The origin of these objects is still debated, with the main plausible scenarios being: the dynamical ejection from a

Context. The study of the Milky Way is living a golden era thanks to the enormous high-quality datasets delivered by Gaia, and space asteroseismic and ground-based spectroscopic surveys. However, the current major challenge to reconstructing the chronology of the Milky Way is the difficulty to derive precise stellar ages for large samples of stars