Observational Studies of the Chemical Evolution in the Galactic Thin and Thick Disks

The origin and evolution of the thin and thick disks in the Galaxy have been studied by means of detailed stellar abundances. High-resolution spectra of 102 F and G dwarf stars have been obtained with the spectrographs on the ESO 3.6-m and ESO 1.5-m telescopes on La Silla (Chile), the Very Large Telescope (VLT) on Paranal (Chile), and the Nordic Optical Telescope (NOT) on La Palma (Canary Islands, Spain). Abundances for 14 elements (O, Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni, Zn, Y, Ba, and Eu) have been determined. The following results were found: 1) Both the thin and the thick disks show distinct and well-defined abundance trends at sub-solar metallicities; 2) The thick disk shows signatures of chemical enrichment from Type Ia Supernovae; 3) [O/Fe] in the thin disk continues to decrease linearly at super-solar metallicities; 4) The abundance trends we see in the thick disk are invariant with distance from the Galactic plane ($Z_{
m max}$) and galactocentric radius ($R_{
m m}$); 4) The thick disk sample is in the mean older than the thin disk sample.

The thesis also includes an investigation of ages and metallicities in the thick disk. The results from this study are; 5) There is a possible age-metallicity relation present in the thick disk, 6) Star formation has been ongoing for several billion years in the thick disk.

Based on these findings, together with other constraints from the literature, we discuss different formation scenarios for the thick disk. We suggest that the currently most likely formation scenario is a violent merger event or a close encounter between the Galaxy and a companion galaxy.