The relationships between atmosphere parameters and chemical abundances of post ZAMS stars of intermediate mass

In this study we performed chemical abundance analysis of 17 intermediate-mass, slow-rotating post zero age main sequence stars covering the late B to early F spectral type range using their high-resolution spectra obtained with the RTT150 telescope at TÜBİTAK National Observatory. The atmosphere parameters, radial velocities and projected rotational velocities were determined spectroscopically. Model atmospheres were computed for each star with the ATLAS9 code, which is based on local thermodynamic equilibrium and plane parallel assumptions. The abundances of C, N, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, Eu, Gd, and Hg were measured from the spectra of the stars. Accordingly, HD 4321, HD 125658, HD 137928, HD 154713, and HD 159834 could be metallic-line stars, HD 2924 and HD 26553 could be of normal A-type. The positions of the stars on the Hertzsprung Russel diagram were determined. The masses and ages were predicted using theoretical evolution tracks and isochrones. Their radii were calculated using the obtained luminosity and effective temperatures. Pearson, Spearman, and Kendall correlation analyses were conducted to investigate the possible relationships between the parameters and chemical abundances. As the effective temperature and surface gravity acceleration increased, a significant decrease in Sc abundance and a tendency to increase in Ti, V, Cr, Mn, Fe, Ni, Zn, Y, Zr, and Ba abundances were observed. While Sc abundance decreased, Ti, V, Cr, Mn, Fe, Ni, Zn, Sr, Zr, and Ba abundances increased.