The chemical evolution of the Universe is governed by the chemical yields from stars, which
in turn are determined primarily by the initial stellar mass. Even stars as low as 0.9 M⊙ can …

The study of stellar oscillations allows us to infer the properties of stellar interiors.
Meanwhile, fundamental parameters such as mass and radius can be obtained by studying …

An updated grid of stellar yields for low-to intermediate-mass thermally pulsing asymptotic
giant branch (AGB) stars is presented. The models cover a range in metallicity Z= 0.02 …

Astrophysicists are increasingly taking into account the effects of orbiting companions on
stellar evolution. New discoveries have underlined the role of binary star interactions in a …

We investigate anew the distribution of absolute carbon abundance, A (C)= log epsilon (C),
for carbon-enhanced metal-poor (CEMP) stars in the halo of the Milky Way, based on high …

We present models for the slow neutron-capture process (s-process) in asymptotic giant
branch stars of metallicity [Fe/H]=− 2.3 and masses 0.9–6 M☉. We encountered different …

Context. Results from observations report a growing number of metal-poor stars showing an
abundance pattern midway between the s-and r-processes. These so-called r/s-stars raise …

High-resolution spectroscopic observations of 100 metal-poor carbon and s-rich stars
(CEMP-s) collected from the literature are compared with the theoretical nucleosynthesis …

Context. Masses are one of the most difficult stellar properties to measure. In the case of the
white-dwarf (WD) companions of Barium (Ba) stars, the situation is worse. These stars are …

We present a high-resolution elemental-abundance analysis for a sample of 23 very metal-
poor ([Fe/H]<− 2.0) stars, 12 of which are extremely metal-poor ([Fe/H]<− 3.0), and 4 of which …