The solar chromosphere is the region between the relatively thin and cold photosphere (temperature of a few thousand degrees) and the hot and extended corona...

The Sun is the only star where we can resolve the intricate magnetism that all convective stars harbor. Yet, more than 99% of its visible surface along the...

The magnetic field in the solar chromosphere plays a key role in the heating of the outer solar atmosphere and in the build-up and sudden release of energy in...

We present a detailed study of the gas chemical abundances in planetary nebulae (PNe), the final fate of solar-like stars, through high spatial resolution...

Can neural networks distinguish computer simulated galaxy images from observed galaxies? This is the question that has been addressed in this work. For years...

Puzzling properties of massive early-type galaxies (ETGs) emerge when studying their spectra at near-infrared (NIR) wavelengths. Massive ETGs show strong CO...

Ultrahot giant exoplanets receive thousands of times Earth’s insolation. Their high-temperature atmospheres (greater than 2,000 kelvin) are ideal laboratories...

CaII Kgrains, i.e., intermittent, short-lived (about 1 minute), periodic (2-4 minutes), pointlike chromospheric brightenings, are considered to be the...

In the current cosmological model, galaxies are formed in a hierarchical way, by merging with each other. These mergers can lead to kinematic anomalies that can...