Introduction. The NEO Rapid Observation, Characterization and Key Simulations (NEOROCKS) project is funded (2020-2023) through the H2020 European Commission programme to improve our knowledge on near-Earth objects by connecting expertise in performing small body astronomical observations and the related modelling needed to derive their dynamical

IntroductionAsteroid (594913) 'Aylo'chaxnim, formerly designated as 2020 AV2, is the only one known to orbit inside Venus orbit. It was first observed by the Zwicky Transient Facility on January 4, 2020 (Bolin et al. 2020) and it may represent the largest member of a new population of small bodies with the aphelion distance smaller than 0.718 a.u

Planets smaller than Neptune are ubiquitous in the Galaxy and those around M stars constitute the bulk of warm and temperate worlds amenable for detailed atmospheric characterization. In this talk, we present a re-analysis of all the available data on small transiting planets around M dwarfs, refining their masses and radii (Luque & Pallé 2022, in

The key role that hydrodynamic escape has on the mass loss of the planets and their evolution is well known. This is particularly important for close-in planets because the extreme stellar XUV irradiation they receive causes them to undergo hydrodynamic atmospheric escape. Although the mass loss caused by this mechanism may not be high enough to

We will present the opportunities of an ERASMUS+ strategic partnership KA2 funding schemes which we used to support (not only) early career researchers in astronomy. ERASMUS+ is a general funding scheme and we describe here one particular project funding education and international partnerhsip of institutions in astronomical research. Our first

IntroductionThe asteroid (4660) Nereus is considered one of the most accessible targets for a rendez-vous space mission. It was proposed as a possible target for the NASA Near-Earth Asteroid Rendezvous (NEAR) and for JAXA Hayabusa spacecraft. The lightcurve analysis and the radar shape modeling revealed a long rotational period of ≅ 15.16 ± 0.04 h