Determination of atomic abundances of solar-type stars

We discuss the results of abundance determinations of the solar- type stars HD1835 and HD10700 using our new procedure. This procedure has the advantage of automated pipeline usage for large amounts of spectroscopic data, with minimal user input. It is based on the spectral synthesis method, where the best values are found with our own developed minimization technique. We reduce the number of free parameters in minimization space using thefit to the observed atomic iron lines. We calibrated our procedure usingfits to the observed solar spectrum. Then we determined abundances in two solar- type stars, namely the metal- deficient star HD10700 and the metal- rich star HD1835. We found good agreement with previously published results. Thus, we aim to use this procedure for the abundance determination of solar- type stars, particularly planet hosting stars, where the knowledge of abundances is crucial for our understanding of their evolution and formation processes.