2022ApJ...926..196H -
Astrophys. J., 926, 196-196 (2022/February-3)
A Nuclear Equation of State Inferred from Stellar r-process Abundances.
HOLMBECK E.M., O'SHAUGHNESSY R., DELFAVERO V. and BELCZYNSKI K.
Abstract (from CDS):
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, with R 1.4 = 12.25 ± 0.03 km and M TOV = 2.17 ± 0.03 M ☉ (statistical uncertainties, neglecting modeling systematics).
Abstract Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
Journal keyword(s):
Nucleosynthesis - R-process - Population II stars - Neutron stars
Simbad objects:
6
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