Understanding an origin of palladium in metal-poor stars based on the non-LTE analysis of Pd~I lines

Abstract

Palladium is one of poorly observed neutron-capture elements. Abundance determinations for stellar samples covering a broad metallicity range are needed for better understanding the mechanisms of Pd synthesis during the Galaxy evolution. We aim to obtain accurate abundances of Pd for the Sun and the sample of metal-poor stars based on the non-local thermodynamic equilibrium (non-LTE) line formation for Pd~I. We present a new, comprehensive model atom of Pd~I. Abundances of Pd, Sr, Ba, and Eu were derived for 48 stars from the non-LTE analyses of high resolution and high signal-to-noise ratio spectra provided by the ESO archives. Non-LTE leads to weakened Pd~I lines and positive non-LTE abundance corrections growing from 0.2~dex for the solar lines up to 0.8~dex for the lines in the most luminous star of the sample. Depending on a treatment of inelastic collisions with hydrogen atoms, the solar non-LTE abundance amounts to log eps = 1.61+-0.02 to 1.70+-0.02 and agrees within the error bars with the meteoritic abundance log eps_met = 1.65. Non-LTE largely removes the discrepancies in the LTE abundances between the giant and dwarf stars of similar metallicities. Palladium tightly correlates with Eu in the -1.71 < [Fe/H] < -0.56 range indicating the r- and s-process contributions to Pd synthesis of approximately 70% and 30%, respectively. Palladium is of pure r-process origin in our two r-II stars, and a dominant contribution of the r-process to the Pd abundances is found for another two very metal-poor (VMP, [Fe/H] < -2) stars. The two VMP stars, which are strongly enhanced with Sr relative to Ba and Eu, reveal also enhancements with Pd. We propose that the source of extra Sr and Pd in these stars are VMP, fast rotating massive stars. Non-LTE is essential for obtaining the observational constraints to future models of the Galactic Pd evolution.