S22A0128

The astrophysical production sites of the heaviest elements in the universe remain a mystery. Incorporating the heavy-element signatures of metal-poor, r-process-enhanced stars into theoretical studies of r-process production can provide crucial constraints on the origin of heavy elements. A well-established method for obtaining empirical evidence on r-process sites is through observations of stars that are strongly enhanced of r-process elements in the Milky Way. The LAMOST medium-resolution spectroscopic survey has measured the Eu and Ba abundances of more than 10,000 stars, and has discovered 12 new r-process enhanced stars. Importantly, these stars are more metal-rich than most of the r-process enhanced stars found in the Galactic halo or dwarf galaxies. Follow-up observation of these stars allow us to 1) confirm the Eu abundance derived from LAMOST R ∼ 7,500 spectra, 2) analyze the abundance patterns, and to 3) complete the vacancy of the metal-rich end of r-process enhanced stars. Here, we propose to observe these 12 r-process enhanced stars using Subaru/HDS, aiming to derive their detailed abundance patterns for constraints on the conditions of the r-process in the stellar production sites.

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