The Origin of Elements from Carbon to Uranium
  To reach a deeper understanding of the origin of elements in the periodic
table, we construct Galactic chemical evolution (GCE) models for all stable
elements from C (A=12) to U (A=238) from first principles, i.e., using
theoretical nucleosynthesis yields and event rates of all chemical enrichment
sources. This enables us to predict the origin of elements as a function of
time and environment. In the solar neighborhood, we find that stars with
initial masses of M>30M_\odot can become failed supernovae if there is a
significant contribution from hypernovae (HNe) at M~20-50M_\odot. The
contribution to GCE from super asymptotic giant branch (AGB) stars (with
M~8-10M_\odot at solar metallicity) is negligible, unless hybrid white dwarfs
from low-mass super-AGB stars explode as so-called Type Iax supernovae, or
high-mass super-AGB stars explode as electron-capture supernovae (ECSNe). Among
neutron-capture elements, the observed abundances of the second (Ba) and third
(Pb) peak elements are well reproduced with our updated yields of the slow
neutron-capture process (s-process) from AGB stars. The first peak elements,
Sr, Y, and Zr, are sufficiently produced by ECSNe together with AGB stars.
Neutron star mergers can produce rapid neutron-capture process (r-process)
elements up to Th and U, but the timescales are too long to explain
observations at low metallicities. The observed evolutionary trends, such as
for Eu, can well be explained if ~3% of 25-50 M_\odot hypernovae are
magneto-rotational supernovae producing r-process elements. Along with the
solar neighborhood, we also predict the evolutionary trends in the halo, bulge,
and thick disk for future comparison with galactic archaeology surveys.
