Bulletin of the American Physical Society
APS April Meeting 2019
Volume 64, Number 3
Saturday–Tuesday, April 13–16, 2019; Denver, Colorado
Session D12: Undergraduate Research III
3:30 PM–5:18 PM,
Saturday, April 13, 2019
Sheraton
Room: Plaza Court 1
Chair: Brad Conrad, Society of Physics Students/Sigma Pi Sigma
Abstract: D12.00007 : A Computational Study of Nucleo-Synthesis Inside Stars*
4:42 PM–4:54 PM
Presenter:
Jose pacheco
(Northern New Mexico College)
Authors:
Jose pacheco
(Northern New Mexico College)
Ajit S Hira
(Northern New Mexico College)
Alicia Sandoval
(Northern New Mexico College)
Edwardine Fernandez
(Santa Fe Community College)
Arrick Gonzales
(Northern New Mexico College)
Tommy Cathey
(Lockheed Information Systems)
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.
*Funding from the NSF.
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