A Computational Study of Nucleo-Synthesis Inside Stars

We continue our interest in Astrophysical objects in this computational study of nucleosynthesis inside stars. in the past, research showed that a combination of the shock-wave nucleosynthesis and of hydrostatic-burning processes create most isotopes of the elements carbon (Z = 6), oxygen (Z = 8), and elements with Z = 10–28 (from Ne to Ni). It is now generally accepted that the rapid neutron-capture process (r-process) is fundamentally important for explaining the origin of approximately half of the stable nuclei with A > 60. The models that used to obtain our results are based on the theoretical methods used in the work of S. Goriely, A. Bauswein and H. Janka. The work of these researchers revealed that the merger of binary Neutron Stars (NSs) are a credible primary source for the heavy (A >~ 140) galactic r-nuclei for rates of 10^-5 yr^-1. We utilized C and C++ languages to implement the theoretical models. Novel data about the r-process was discovered in 2017,by the LIGO and Virgo observatories from a merger of two neutron stars. With more data from the gravitational wave detectors, we will test our theoretical models, and our theoretical predictions on nucleosynthesis. We will also simulate the formation of some quarks composites in supernovae.