Emergent Nucleosynthesis from a 1.2 s Long Simulation of a Black Hole Accretion Disk

We simulate a black hole accretion disk system with full-transport general relativistic neutrino radiation magnetohydrodynamics for 1.2 s. This system is likely to form after the merger of two compact objects and is thought to be a robust site of r-process nucleosynthesis. We consider the case of a black hole accretion disk arising from the merger of two neutron stars. Our simulation time coincides with the nucleosynthesis timescale of the r-process (~1 s). Because these simulations are time-consuming, it is common practice to run for a "short" duration of approximately 0.1–0.3 s. We analyze the nucleosynthetic outflow from this system and compare the results of stopping at 0.12 and 1.2 s. We find that the addition of mass ejected in the longer simulation as well as more favorable thermodynamic conditions from emergent viscous ejecta greatly impacts the nucleosynthetic outcome. We quantify the error in nucleosynthetic outcomes between short and long cuts.. Authors: Sprouse, Trevor Michael [Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)] (ORCID:0000000243754369); Lund, Kelsey Alexandra [Los Alamos National Laboratory (LANL), Los Alamos, NM (United States); North Carolina State University, Raleigh, NC (United States)] (ORCID:0000000300311397); Miller, Jonah Maxwell [Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)] (ORCID:0000000164327860); McLaughlin, Gail C. [North Carolina State University, Raleigh, NC (United States)] (ORCID:0000000168116657); Mumpower, Matthew Ryan [Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)] (ORCID:0000000299509688). DOE Contract: 89233218CNA000001; AC52-07NA27344; FG02-00ER41132; FG02-02ER41216. Subjects: 79 ASTRONOMY AND ASTROPHYSICS; Magnetohydrodynamical simulations; Nuclear astrophysics; Nuclear physics; Nucleosynthesis; R-process; Stellar accretion discs