Project Details
Projekt Print View

Nuclear physics for stellar explosions

Subject Area Nuclear and Elementary Particle Physics, Quantum Mechanics, Relativity, Fields
Term from 2016 to 2023
Project identifier Deutsche Forschungsgemeinschaft (DFG) - Project number 286691198
 
Final Report Year 2024

Final Report Abstract

The synthesis of the elements in our universe takes place in all stages of stellar evolution, from hydrogen burning in main sequence stars over subsequent burning phases to their eventual death, and even beyond, when stellar remnants collide or accrete mass from companion stars. The interplay between the astrophysical environments necessary to allow for nucleosynthesis and the nuclear reactions that facilitate the transmutation of one element into another gives rise to an abundance of nucleosynthesis processes the modelling of which requires information on a highly varied set of nuclear properties. With a focus on the production of the proton rich p-nuclei, thought to be produced mainly in stellar explosions classified as type II supernovae, this work program aimed at reducing uncertainties associated with the nucleus+α optical model potential (α-OMP), nuclear level densities (NLD) at high excitation energies, and the γ-strength function (γ-SF). These properties are used to calculate cross sections in the framework of Hauser-Feshbach statistical model calculations in order to model the vast reaction networks involved in the production of p-nuclei, particularly via the γ process. To study these properties, experimentally determined cross sections are compared to theoretical calculations.

Publications

 
 

Additional Information

Textvergrößerung und Kontrastanpassung