Neutron captures produce the vast majority of abundances of elements heavier than iron in
the Universe. Beyond the classical slow (s) and rapid (r) processes, there is observational …

The creation of carbon and oxygen in our Universe is one of the forefront questions in
nuclear astrophysics. The determination of the abundance of these elements is key to our …

To reach a deeper understanding of the origin of elements in the periodic table, we construct
Galactic chemical evolution (GCE) models for all stable elements from C (A= 12) to U (A …

We present a comprehensive study of the abundance evolution of the elements from H to U
in the Milky Way halo and local disc. We use a consistent chemical evolution model …

Probing the origin of r-process elements in the universe represents a multidisciplinary
challenge. We review the observational evidence that probes the properties of r-process …

We present a new set of models for intermediate-mass asymptotic giant branch (AGB) stars
(4.0, 5.0, and 6.0 M⊙) at different metallicities (− 2.15≤[Fe/H]≤+ 0.15). This set integrates …

The decomposition of the Solar system abundances of heavy isotopes into their s-and r-
components plays a key role in our understanding of the corresponding nuclear processes …

Rotation was shown to have a strong impact on the structure and light element
nucleosynthesis in massive stars. In particular, models including rotation can reproduce the …

Aims. To understand the formation and evolution of the different stellar populations within
our Galaxy it is essential to combine detailed kinematical and chemical information for large …

Context. We present a large homogeneous set of stellar parameters and abundances across
a broad range of metallicities, involving 13 classical dwarf spheroidal (dSph) and ultra-faint …