📝 SummarXiv

Abstract

The dominant site(s) of the $r$-process are a subject of current debate. Ejecta from $r$-process enrichment events like kilonovae are difficult to directly measure, so we must instead probe abundances in metal-poor stars to constrain $r$-process models. This requires state-of-the-art Non-Local Thermodynamic Equilibrium (NLTE) modeling, as LTE is a poor approximation for the low-opacity atmospheres of metal-poor giants. Neodymium (Nd) is a prominent $r$-process element detected in both near-infrared kilonovae spectra and spectra of metal-poor stars, so precise Nd stellar abundances are particularly needed to model kilonovae and constrain $r$-process sites. We thus constructed a Nd I / Nd II model atom to compute NLTE abundances in FGK metal-poor stars. We obtain $\mathrm{A(Nd)}_\odot = 1.44\pm0.05$, in agreement with the meteoritic value, when calibrating the model atom with a Drawin hydrogen collision factor of $S_H=0.1$. For a sample of metal-poor $r$-process enhanced stars with observed optical and near-infrared Nd II lines, we find NLTE Nd corrections in the range $-0.3$ to $0.3$ dex. Optical and UV lines have positive NLTE corrections, whereas H band lines have negative corrections. Additionally, we compute a large grid of NLTE corrections for 122 Nd II spectral lines ranging from the UV to the H band, for stellar parameters of typical metal-poor FGK dwarfs and giants with $-3.00\le\mbox{[Fe/H]}\le-1.00$ and $-2.0\le\mathrm{A(Nd)}\le2.0$. Within this grid, we find NLTE corrections ranging from $-0.3$ to $+0.5$ dex. Deviations from LTE are found to be strongest for blue lines with low excitation potentials in the most metal-poor giants.