Modelado de atmosferas estelares para la obtención de sus parámetros físicos utilizando espectroscopia multi-banda

Abstract

The research aimed to analyse multiple wavelengths (X-ray to optical) of the supergiant star Dseta Ori by modelling stellar atmospheres. The analysis is based on X-ray data from Chandra and XMM-Newton, ultraviolet data from the International Explorer Ultraviolet and the COPERNICUS satellite, and optical data taken from the POLARBASE archive. For the research was carried out by checking the consistency of the physical parameters of the stellar atmospheres, such as the mass loss rate, assuming the abundance of Carbon, Nitrogen, Oxygen, derived from different spectral bands and providing more stringent constraints to reduce the systematic errors. In addition, two main stages were carried out. In the first stage, we detailed the photo spheric and wind parameters using the standard method for massive stars and the latest version of the radiative transfer code designed to solve the radiative transfer and statistical equilibrium equations in spherical geometry. In the second stage, the X-ray emission is modelled. In doing so, we check the consistency of the adopted parameters with the X-ray line profiles (mass-loss rates) and the line ratios (abundances). Finally, the synthetic spectrum for optical, UV and X-ray data was obtained and fitted correctly to the observed spectrum correctly matched the observed spectrum without the need to consider its magnetic field, however, it is recommended to quantify the effect of the companion star Ab on the H&I lines to estimate a better temperature.