Speaker
Description
The metallicity of Proxima Centauri is a quantity of this red dwarf star that is particularly unknown due to heavy molecules that grow on the stellar atmosphere and photosphere for stellar temperatures below 5000 K. The stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA) and the Vienna Atomic Line Database (VALD) are used to investigate observational and spectral data from Proxima Centauri. Metallicity of 0.004 < Z < 0.01 creates minute differences in their respective models’ results. The model with the greatest luminosity value, Proxima Centauri at Z=0.004, has 6.1329x10$^{8}$ years left in its simulated existence. Reduced metallicity resulted in greater brightness, according to the Proxima Centauri simulation. As a result, stellar life expectancy is shortened. The link between log L–log R and log Teff–log g is directly proportional, according to the linear regression performed on the data of model Z=0.004. On the other hand, log L–log g, log R–log g, and log Teff–log R are inversely proportional. In this study, a preliminary metallicity analysis of Proxima Centauri is presented. The spectral lines of Proxima Centauri’s atmosphere were calculated using the VALD database and the MESA simulation model’s parameters.
