Chemical abundance analysis of the a-type star HD 58552

In this thesis study, chemical abundance analysis was performed to the high resolution spectra of the A-type star HD 58552. Detailed abundance analysis of this star is not available in the litrature. The abundance values of the observed elements in the spectrum of HD 58552 were calculated and compared to the solar abundances. The spectrum of the star was obtained using the Coude spectrograph attached to the 1.5 m diameter telescope at the TÜBİTAK National Observatory. The observational spectrum, covering a wavelength range of 3900-8000 Å was reduced using the IRAF program. Model atmopheres were generated using the ATLAS9 code. The atomic line list was compiled from the Vienna Atomic Line Database. The synthetic spectra generated using the line list were adapted to the BINMAG program to determine the central wavelengths and measure the equivalent width of all absorption lines. Synthetically produced hydrogen Balmer line profiles were compared with the observational data of the star to verify the atmosphere parameters obtained by using photometric calibrations. The atmosphere parameters of HD 58552 were determined as Teff = 9000±150 K, log g =4.4±0.1 dex and ξ=3.2±0.5 kms-1 by performing analyses to the spectra of the star. The rotational velocity of the star was measured as 16±2 kms-1 . The abundances of C, O, Na, Mg, Si, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Ni, Sr, Y and Ba were calculated by adapting the measured equivalent widths to the WIDTH9 program. The abundance distribution of HD 58552 was found to be consistent with the chemical peculiar A-type stars of the metallic-line class. The star was positioned on the H-R diagram using the derived Teff from the spectrum of HD 58552. Evolutionary tracks and isochrones were overlaid on the H-R diagram to estimate the mass of this main sequence star as 2.06±0.09 Mʘ and age as 400±80 million years. The mass calculated using the MTGR was found to be consistent with the result obtained above.