Sensitivity of p-Process Nucleosynthesis to Nuclear Reaction Rates in a 25 Solar Mass Supernova Model

TL;DR

This study examines how variations in nuclear reaction rates affect the synthesis of proton-rich nuclei in a 25 solar mass supernova, highlighting key reaction pathways and uncertainties in p-process nucleosynthesis.

Contribution

It provides a comprehensive analysis of the sensitivity of p-process yields to nuclear reaction rate uncertainties in a supernova model.

Findings

Reaction flux identifies main synthesis pathways.

Reaction rate variations significantly alter p-nuclei abundances.

Results inform future experimental strategies.

Abstract

The astrophysical p process, which is responsible for the origin of the proton rich stable nuclei heavier than iron, was investigated using a full nuclear reaction network for a type II supernova explosion when the shock front passes through the O/Ne layer. Calculations were performed with a multi-layer model adopting the seed of a pre-explosion evolution of a 25 solar mass star. The reaction flux was calculated to determine the main reaction path and branching points responsible for synthesizing the proton rich nuclei. In order to investigate the impact of nuclear reaction rates on the predicted p-process abundances, extensive simulations with different sets of collectively and individually modified neutron-, proton-, alpha-capture and photodisintegration rates have been performed. These results are not only relevant to explore the nuclear physics related uncertainties in p-process calculations but are also important for identifying the strategy and planning of future experiments.