Ekaterina Magg
Max-Planck Institute for Astronomy, Heidelberg, Germany

Abstract
Solar chemical composition is the first step in understanding stellar populations, both from theoretical and observational perspectives. It is also a crucial ingredient in stellar evolutionary models which describe stars’ life cycles. Despite significant advances in our understanding of the Sun — our closest and most studied star — its chemical makeup is still affected by the modelling assumptions and uncertainties of experimental data. I will talk about state-of-the-art Non-LTE and 3D modelling of stellar atmospheres, its cost, importance, and applications. I will then focus on our recent study of the solar abundances and the influence of derived abundances on the Standard Solar Model, a step-stone of the decade-long ’solar abundances crisis’, where spectroscopic and helioseismic observation could not be reconciled.

2022 May 04, 13:30

IA
Online broadcast (Zoom)