  To investigate the physical nature of neutrino-heating on the result of a
1-dimensional core-collapse supernova. Colgate were the first to suggest that
neutrinos may play a crucial role in core collapse supernova by taking up
gravitational binding energy from the core and depositing it in the rest of the
star. The fluid is contained in a shock tube in a region extending from the
neutrino-sphere of a star out 1000 km, and irradiated with a neutrino flux
emanating from the surface of the neutrino-sphere into the shock tube.
Interaction due to electron-neutrino scattering off of fluid nucleons is used
to account for neutrino heating of the fluid. The numerical method used is the
Godunov method implementing an exact Riemann solver Rezzolla when needed. The
simulated core-collapse produces an energy output of up to $10^{36}$J on a
timescale of 3.33 s. It was found that the Godunov method performs very well
using Sod data, with standard deviations of between $0.22-0.04$%. Thus, there
is high confidence that the exact Riemann solver is working correctly and that
the Godunov method is also reproducing the exact solutions to the Sod data with
high confidence. A runtime of 3.33 s was used. The objective was to determine
what would happen to the shock system over longer timescales, but the
simulations showed an explosion in a much shorter time frame. It was found that
the shock not only continues to move outward, but is also driven by large
energy and pressure behind the shock. The density profiles show that fluid mass
is pushed outward, but the fluid velocity actually reversed on timescales close
to 3.33 s. In this paper, net mass movement occurs at 500-600 km and on a
longer timescale of 3.33 s mass has moved out to 700 km. This supports the
\emph{delayed post bounce shock mechanism}.
