{ "id": "2110.06432", "version": "v1", "published": "2021-10-13T01:29:27.000Z", "updated": "2021-10-13T01:29:27.000Z", "title": "A Nuclear Equation of State Inferred from Stellar r-Process Abundances", "authors": [ "Erika M. Holmbeck", "Richard O'Shaughnessy", "Vera Delfavero", "Krzysztof Belczynski" ], "comment": "14 pages, 7 figures", "categories": [ "astro-ph.HE", "nucl-th" ], "abstract": "Binary neutron star mergers (NSMs) have been confirmed as one source of the heaviest observable elements made by the rapid neutron-capture (r-) process. However, modeling NSM outflows -- from the total ejecta masses to their elemental yields -- depends on the unknown nuclear equation of state (EOS) that governs neutron-star structure. In this work, we derive a phenomenological EOS by assuming that NSMs are the dominant sources of the heavy-element material in metal-poor stars with r-process abundance patterns. We start with a population synthesis model to obtain a population of merging neutron star binaries and calculate their EOS-dependent elemental yields. Under the assumption that these mergers were responsible for the majority of r-process elements in the metal-poor stars, we find parameters representing the EOS for which the theoretical NSM yields reproduce the derived abundances from observations of metal-poor stars. For our proof-of-concept assumptions, we find an EOS that is slightly softer than, but still in agreement with, current constraints, e.g., by the Neutron Star Interior Composition Explorer (NICER), with $R_{1.4}=12.25\\pm 0.03$~km and $M_{\\textrm TOV}$ of $2.17\\pm 0.03$~M$_\\odot$(statistical uncertainties, neglecting modeling systematics).", "revisions": [ { "version": "v1", "updated": "2021-10-13T01:29:27.000Z" } ], "analyses": { "keywords": [ "stellar r-process abundances", "nuclear equation", "metal-poor stars", "neutron star interior composition explorer", "elemental yields" ], "note": { "typesetting": "TeX", "pages": 14, "language": "en", "license": "arXiv", "status": "editable" } } }