Spectroscopy of dwarf stars

Spectroscopic information is of paramount importance in characterising the stars and analysing planets possibly orbiting them, and in studying the Galactic disc evolution. The aim of this work was to analyse all bright (V<8mag) F, G, and K dwarf stars using high-resolution spectra in the selected sky fields near the northern celestial pole.

The observations were carried out with the 1.65m diameter telescope at the Molttai Astronomical Observatory and a fibre-fed high-resolution spectrograph covering a full visible wavelength range (4000-8500{AA}). The atmospheric parameters were derived using the classical equivalent width approach while the individual chemical element abundances were determined from spectral synthesis. For both tasks the one-dimensional plane-parallel LTE MARCS stellar model atmospheres were applied.