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Area of Science:

  • Astrophysics
  • Nuclear Physics
  • Computational Science

Background:

  • Black-hole-neutron-star mergers are key astrophysical events.
  • Understanding nucleosynthesis in their ejecta is crucial for astrophysics and nuclear physics.
  • Previous studies lacked long-term simulations of merger ejecta.

Purpose of the Study:

  • To investigate nucleosynthesis in black-hole-neutron-star merger ejecta.
  • To analyze the contribution of dynamical and postmerger ejecta to element formation.
  • To constrain nuclear equations of state using nucleosynthetic signatures.

Main Methods:

  • Performed long-term neutrino-radiation-magnetohydrodynamics simulations.
  • Analyzed the composition of merger ejecta, focusing on electron fraction and velocity.
  • Compared simulated nucleosynthetic abundances with observations of r-process-enhanced stars.

Main Results:

  • The combined ejecta reproduce a solar-like r-process abundance pattern.
  • Actinide enhancement is sensitive to the electron fraction and velocity of dynamical ejecta.
  • A mean electron fraction of ≳0.05 in dynamical ejecta is required to match observed abundances.

Conclusions:

  • Black-hole-neutron-star mergers are potential sources for r-process elements, including actinides.
  • The neutron richness of tidal ejecta provides constraints on nuclear equations of state.
  • These findings link merger simulations to observational constraints from actinide-boost stars.