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To investigate the physical nature of neutrino-heating on the result of a1-dimensional core-collapse supernova. Colgate were the first to suggest thatneutrinos may play a crucial role in core collapse supernova by taking upgravitational binding energy from the core and depositing it in the rest of thestar. The fluid is contained in a shock tube in a region extending from theneutrino-sphere of a star out 1000 km, and irradiated with a neutrino fluxemanating from the surface of the neutrino-sphere into the shock tube.Interaction due to electron-neutrino scattering off of fluid nucleons is usedto account for neutrino heating of the fluid. The numerical method used is theGodunov method implementing an exact Riemann solver Rezzolla when needed. Thesimulated core-collapse produces an energy output of up to $10^{36}$J on atimescale of 3.33 s. It was found that the Godunov method performs very wellusing Sod data, with standard deviations of between $0.22-0.04$%. Thus, thereis high confidence that the exact Riemann solver is working correctly and thatthe Godunov method is also reproducing the exact solutions to the Sod data withhigh confidence. A runtime of 3.33 s was used. The objective was to determinewhat would happen to the shock system over longer timescales, but thesimulations showed an explosion in a much shorter time frame. It was found thatthe shock not only continues to move outward, but is also driven by largeenergy and pressure behind the shock. The density profiles show that fluid massis pushed outward, but the fluid velocity actually reversed on timescales closeto 3.33 s. In this paper, net mass movement occurs at 500-600 km and on alonger timescale of 3.33 s mass has moved out to 700 km. This supports the\emph{delayed post bounce shock mechanism}.

A 1-D Special Relativistic Shock Tube where Stellar Fluid undergoes Neutrino Heating