Date of Award
Doctor of Philosophy (PhD)
Physics & Astrophysics
Population III stars are the first stars formed after the Big Bang, comprised of primarily
hydrogen and helium and lack heavy elements from previous generations. Using the
one-dimensional radiation-hydrodynamics code BOOM, a grid of eighteen stellar models
with masses of 15-80 solar masses , are exploded under a low and high explosion energy criteria.
Three types of central compact remnants are considered. The 3208 isotope TORCH nuclear
reaction network is used to calculate the nucleosynthesis that occurs during the
supernovae. The two convection criteria, Ledoux and Scharzschild, produce vastly
different stellar structures and thus produce different nucleosynthetic trends. When
comparing the numerically calculated abundances to observed extremely metal poor stars
([Fe/H] < â3), it is found that even using abundances from both the Schwarzschild and
Ledoux convection model a fit was not possible. The overall Ni-56 production claculated
for a given distribution and the peak production of Ni-56 is compared to observationally
calculated values from Population II supernovae. We show that for high energy
Schwarzschild models, integrated over a Salpeter initial mass function, the yields
approach that of the more compact lower energy Ledoux series, but heavier elemental
abundances of these metal poor stars need to be observed and determined to better fit the
data. The produced nickel for both series is high compared to observational work and is
likely to be lessened for larger central remnants.
Teffs, Jacob, "The Impact Of Stellar Convection Criteria On Population Iii Supernovae Nucleosynthesis" (2018). Theses and Dissertations. 2362.