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 (Teff, 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 (Teff, 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

Cool star atmospheres present challenges to chemical abundance studies. To date, only a handful of elements have been quantified for a handful of M dwarfs. In high-resolution spectra from the CARMENES survey, we identify a series of dramatically hyperfine-split vanadium features between 800 and 910 nm, which have strong and clean profiles