Chemodynamical Evolution of Dwarf Galaxies

Abstract

Abundances of elements in metal-poor stars reflect the evolutionary histories of galaxies. Chemical evolution of galaxies is highly related to dynamical evolution with them. It is necessary to conduct chemodynamical studies to fully understand the evolutionary histories of galaxies. This chapter aims to show that the isolated dwarf galaxy models used in this work can reproduce basic observed properties of dwarf galaxies in the Local Group. In this chapter, we compare computed radial profiles, star formation histories, metallicity distribution functions, mass-metallicity relations, and \\(\\alpha \\)-element abundances with observed ones. We also discuss the parameter dependence on these quantities (Contents in this chapter have been in part published in [15, 16, 17] reproduced by permission of the AAS and Oxford University Press).