Coloquio SO: Spectroscopy's Role in Stellar Astrophysics

To characterize a star, the stellar fundamental parameters such as mass, radius, metal abundance, and effective temperature should be known. Direct measurements of these parameters, especially for single stars, are quite challenging, and indirect methods are often employed to obtain these characteristics. The most effective method for determining these parameters is spectroscopy, which is an analysis technique of spectra. It allows us to determine the stellar atmospheric parameters such as effective temperature, surface gravity, metallicity, micro turbulence, and rotational velocity values. These parameters play a crucial role in comprehending not only the structure and evolution of stars but also in understanding the evolution of the Milky Way and the chemical evolution of the Universe. Therefore, spectroscopy is a unique tool for a deep understanding of the Universe and its fundamental blocks: stars. To estimate the fundamental atmospheric parameters from spectroscopy there are different methods and this talk will focus on the most prevalent methods used for single and binary B, A, and F-type stars. The presentation will introduce the techniques employed for spectral classification, the determination of atmospheric parameters, the estimation of chemical abundances, the calculation of radial velocity variations in binary systems, and the application of spectral disentangling in binary systems. Furthermore, the impact of spectroscopy on the seismic analysis of pulsating stars will be discussed.