Estimating the Birthplaces and Metallicities of Samples of Nearby Main-Sequence Stars in the Milky Way

Abstract

     Knowing the birth environments with the signatures of the chemical compositions of main-sequence stars in our nearby galactic vicinity plays an important role in understanding the beginning evolution of the Milky Way.  We are carefully studying the selected objects of 67 (∼0.8 – 1.8 M☉) nearby main-sequence stars to know their ages, metallicities, and mostly the birth radii at the galactic disk. We analyze the stellar properties in comparison with the galactic chemical gradients with respect to cosmic time by integrating current isochrone models with the metallicity spectroscopic calculations and rotational data. Our findings confirm the existence of inverse correlation between stellar age and metallicity, as well as between mass and evolutionary phase, which suggests that the time resolution of the chemical enrichment structure in the interstellar medium. Considerably, the reassembled of birth radii shows that a significant number of stars, currently orbiting in the solar circle, were most likely born supplementary inward, thus correlations give important evidence of radial migration. The results support the argument of the dynamic activity of the Milky Way, in which the stellar kinematics and the chemical evolution are highly correlated.