The Sun is a magnetically active star with violent eruptions that can hit Earth´s magnetosphere and cause important perturbations in our technology-dependent society. The objective of the Whole Sun project is to tackle in a coherent way for the first time key questions in Solar Physics that involve as a whole the solar interior and atmosphere.

Galaxy discs are made of two components, the thin and the thick disc. Thick discs contain up to 50% of the baryonic mass of a galaxy. Because their stars are among the oldest in the Universe, thick discs are relics of the infancy of galaxies. Thus, understanding the origin of thick discs is key to unveil how galaxies themselves form, which in turn

Understanding the climate of our planet Earth is one of the greatest challenges in Science today. Much is still to be learned for example, on the variations of Earths albedo, or on external forcing factors, such as changes in the solar radiation. To truly go in depth into these open questions one may need to step out, view the Earth as a planet and

Most of the stars (M < 8 solar masses, Ms) end their lives with a phase of strong mass loss on the Asymptotic Giant Branch (AGB), just before they form planetary nebulae (PNe). The strong mass loss efficiently enriches the interstellar medium (ISM) with gas and dust; AGB stars are one of the main contributors to the enrichment of the ISM where new

Active galactic nuclei (AGN) feedback is the effect that nuclear activity produces in the interstellar and circumgalactic medium (ISM and CGM) of galaxies. Different modes of AGN feedback, which can be broadly divided into radiative/quasar and kinetic/radio, are now considered key processes in the evolution of massive galaxies by regulating black