The γ-process nucleosynthesis in core-collapse supernovae II. Effect of the explosive recipe
Astronomy & Astrophysics(2024)
摘要
The γ-process in core-collapse supernovae (CCSNe) can produce a number
of neutron-deficient stable isotopes heavier than iron (p-nuclei). However,
current model predictions do to not fully reproduce the solar abundances. We
investigate the impact of different explosion energies and parameters on the
nucleosynthesis of p-nuclei, by studying stellar models with different initial
masses and CCSN explosions. We find that the total p-nuclei yields are only
marginally affected by the CCSN explosion prescriptions if the γ-process
production is already efficient in the stellar progenitors due to a C-O shell
merger. In most of CCSN explosions from progenitors without C-O shell merger,
the γ-process yields increase with the explosion energy up to an order
of magnitude, depending on the progenitor structure and the CCSN prescriptions.
The trend of the p-nuclei production with the explosion energy is more
complicated if we look at the production of single p-nuclei. The light p-nuclei
tend to be the most enhanced with increasing the explosion energy. In
particular, for the CCSN models where the α-rich freeze-out component is
ejected, the yields of the lightest p-nuclei increase by up to three orders of
magnitude. We provide the first extensive study using different sets of massive
stars of the impact of varying CCSN explosion prescriptions on the production
of the p-nuclei. Unlike previous expectations and recent results in the
literature, we find that the average production of p-nuclei tends to increase
with the explosion energy. We also confirm that the pre-explosive production of
p-nuclei in C-O shell mergers is a robust result, independently from the
subsequent explosive nucleosynthesis. A realistic range of variations in the
evolution of stellar progenitors and in the CCSN explosions might boost the
CCSN contribution to the galactic chemical evolution of p-nuclei.
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