CONICET | Buscador de Institutos y Recursos Humanos

In this work I present the current progress on the study of the 285.2 nm spectral line.Atomic models are essential to compute the populations in full NLTE. In this case, we test how changes in the atomic model of neutral magnesium influence in the formation of the line mentioned in the Sun and in the GJ832 star.Given the relevance of the spectral features formed by Mg I in the stellar spectrum of late type stars, and because there is a need to improve the Mg I atomic model mainly in the NUV range (eg. 285.2 nm inverted line), the populations and the spectra of 52 species were recalculated using the Solar-Stellar Radiation Physical Modeling (SSRPM) code using different atomic models for Mg I. Then we compared the numerical results in the populations and the effects in the synthetic spectra.Our main goal is to understand the physical processes that rule the formation of our line of interest. We started doing this by changing the next parameters:?Excitation Collision with electrons?Ionizing Collision with electrons?Recombination Coefficients?Radiative parametersFor the first case we used different methods to calculate de Effective Collision Strengths. The original parameters were calculated using the Seaton?s formula for allowed transitions, and the Van Regemorter formula to forbidden transitions. Our new calculations were made using the Distorted-Wave method. We compared the data provided for this two methods with the data provided for the R-matrix calculation (Barklem et al. (2017, A&A 606, A11)).For the next atomic parameters we made arbitrary changes in order to see if those processes play an important role at the height of the line formation.This work in progress will be extended to different stars of different spectral type to finally understand the information that the line 285.2 nm can provide in the observed spectra.