Despite stellar magnetic activity being present in most cool stars, its effects on spectroscopic observations are still not well understood. Several activity indicators are routinely used to identify activity-related signals in radial velocity (RV) measurements, but not all indicators trace exactly the same effects, nor are any of them always

The first results of the application of the MANCHA code to the case of stars beyond the solar case are presented: hydrodynamical simulations of stars of spectral type K0V and M0V compared with the solar case.

Stars with initial masses above ~10 M ⊙ have an internal evolution completely different from those in the range between 4 and ~10 M ⊙. The former are able to ignite all the elements up to Fe in their cores without degeneration (becoming into red supergiants; RSGs). The latter are not, and they become into red giants first, and later into asymptotic

We aim to review the spectral synthesis technique to derive the stellar atmospheric parameters (T eff, log g, and [Fe/H]) of 348 M dwarfs in light of the optical and near-infrared spectra obtained with CARMENES, the high-resolution, double-channel spectrograph installed at the 3.5 m telescope at the Calar Alto observatory (Spain). The analysis

We aim to review the spectral synthesis technique to derive the stellar atmospheric parameters (T eff, log g, and [Fe/H]) of 348 M dwarfs in light of the optical and near-infrared spectra obtained with CARMENES, the high-resolution, double-channel spectrograph installed at the 3.5 m telescope at the Calar Alto observatory (Spain). The analysis

Dark magnetic spots co-rotating with the stellar surface lead to quasi-periodic brightness variations, which enclose relevant information on stellar rotation and magnetic activity properties. In this work, we analyzed the Kepler long-cadence data of 159,710 main-sequence and subgiant FGKM stars. Rotation-period candidates are obtained by combining