Speaker
Elisabetta Caffau
(OBSPM)
Description
In order to derive the chemical composition of a star, observed spectra are compared to theoretical synthesis and to compute theoretical spectra the stellar atmosphere needs to be modelled. Several grids of stellar models are available as also several codes to compute them. The use of different models can imply differences in the abundances derived. We will discuss the limitations and differences in the stellar models and also the limitations due to observations.
Primary author
Elisabetta Caffau
(OBSPM)
