Sérgio F. A. Batista
CAUP

Abstract
Spectroscopy provides a powerful technique to derive stellar parameters for FGK-type stars. These derivations are done by measuring the equivalent widths of weak FeI and FeII absorption lines and then compute the measured abundances assuming LTE conditions. The solution found must satisfy the ionization and excitation equilibrium conditions as well as the independence between the metallicity and the measured equivalent widths. The standard method compares theoretical models with the observations. The latter is done through an iterative process until the best model, which fits the observations, is found.
In this talk, I will present some optimization methods that can be applied to the described problem and I will discuss their implementation. I will also stress out some of the obtained results.

27 November 2013, 13:30

Centro de Astrofísica
Rua das Estrelas
4150-762 Porto