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 …

We extend the PARSEC library of stellar evolutionary tracks by computing new models of
massive stars, from 14 to 350 M⊙. The input physics is the same used in the PARSEC V1. 1 …

We present new theoretical stellar yields and surface abundances for three grids of metal-
rich asymptotic giant branch (AGB) models. Post-processing nucleosynthesis results are …

We present the colibri code for computing the evolution of stars along the thermally pulsing
asymptotic giant branch (TP-AGB) phase. Compared to purely synthetic TP-AGB codes …

We provide a set of stellar evolution and nucleosynthesis calculations that applies
established physics assumptions simultaneously to low-and intermediate-mass and massive …

We present stellar evolutionary tracks and nucleosynthetic predictions for a grid of stellar
models of low-and intermediate-mass asymptotic giant branch (AGB) stars at Z= 0.001 …

We present new theoretical stellar yields and surface abundances for asymptotic giant
branch (AGB) models with a metallicity appropriate for stars in the Small Magellanic Cloud …

The minimum initial mass required for a star to explode as an Fe core collapse supernova,
typically denoted M mas, is an important quantity in stellar evolution because it defines the …

We present new theoretical stellar evolutionary models of metal-rich asymptotic giant branch
(AGB) stars. Stellar models are evolved with initial masses between 1 and 7 M⊙ at Z …

Se presenta un resumen del estado actual de la investigación sobre las nebulosas
planetarias y sus estrellas centrales, y temas relacionados como los procesos atómicos en …