Tracer Particles for Core-collapse Supernova Nucleosynthesis: The Advantages of Moving Backward

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Abstract
After decades, the theoretical study of core-collapse supernova explosions is moving from parameterized, spherically symmetric models to increasingly realistic multidimensional simulations. However, obtaining nucleosynthesis yields based on such multidimensional core-collapse supernova simulations is not straightforward. Frequently, tracer particles are employed. Tracer particles may be tracked in situ during the simulation, but often they are reconstructed in a post-processing step based on the information saved during the hydrodynamic simulation. Reconstruction can be done in a number of ways, and here we compare the approaches of backward and forward integration of the equations of motion to the results based on inline particle trajectories. We find that both methods agree reasonably well with the inline results for isotopes for which a large number of particles contribute. However, for rarer isotopes that are produced only by a small number of particle trajectories, deviations can be large. For our setup, we find that backward integration leads to better agreement with the inline particles by more accurately reproducing the conditions following freeze-out from nuclear statistical equilibrium, because the establishment of nuclear statistical equilibrium erases the need for detailed trajectories at earlier times. Based on our results, if inline tracers are unavailable, we recommend backward reconstruction to the point when nuclear statistical equilibrium was last applied, with an interval between simulation snapshots of at most 1 ms for nucleosynthesis post-processing.
Funding Information
  • DOE | Office of Science | Oak Ridge National Laboratory (DE-AC05-00OR22725)
  • NSF ∣ MPS ∣ Division of Physics (PHY-1913531)
  • NSF ∣ CISE ∣ Office of Advanced Cyberinfrastructure (OCI-0749242)
  • EC ∣ Horizon Europe ∣ Excellent Science ∣ HORIZON EUROPE Marie Sklodowska-Curie Actions (101065891)
  • NSF ∣ MPS ∣ Division of Astronomical Sciences (AST-0653376)
  • NASA ∣ SMD ∣ Astrophysics Division (NNH11AQ72I)
  • DOE ∣ NNSA ∣ LDRD ∣ Lawrence Berkeley National Laboratory (DE-AC02-05CH11231)

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