Speaker
Description
Understanding stellar nucleosynthesis requires expertise in stellar modelling and nuclear physics. Hints and constraints to the nucleosynthesis models come from atmospheric abundance analysis of different stars, as obtained by means of high resolution spectroscopy, and measurements of solar (and pre-solar) composition, as obtained by combining, beside solar spectroscopy, the abundance analyses of planets, minor bodies and, in particular, meteorites. Eventually, chemical evolution models coupled to abundance determinations of the interstellar gas may provide additional constraints. In this review I will introduce the methods currently adopted to calculate stellar chemical yields and I will discuss the present limits and future developments.
