Chemical and Dynamical evolution of the Milky Way and galaxies of the Local Group

The chemical evolution of the Milky Way is a particularly interesting subject in view of the large present and future  spectroscopic surveys  that will produce the most extended map of our Galaxy ever made before. Our group has developed a very detailed model for the Milky Way galaxy which follows the evolution in time and space of 37 chemical abundances in the interstellar gas. In particular, we follow the  evolution of the bulge, the halo and the thin disk. The evolution of the thick disk is at the moment included in that of the halo. In this project we intend to model the thick-disk separately from the other components.

Concerning the bulge,  we are working at a new model which can explain the complex situation of its stellar populations recently revealed by accurate measures of chemical abundances.  For what concerns the thin-disk,  we intend to pursue the study of the effects of  radial flows on the formation of abundance gradients. Starting from the formation of gradients in the disk we also intend to run N-body simulations (in collaboration with researchers of OATO)  to see whether the stars of the thin-disk born in the innermost regions can have migrated at higher latitudes and given origin to the thick-disk . Finally, we intend to study the chemical evolution of dwarf spheroidals  and ultra-faint dwarf galaxies of the Local Group to understand whethet they could have been the building blocks of the Milky Way halo.

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