Neutron Stars are the remnants of massive stars at the end of their life cycles. They are formed when fusion fuel is depleted, resulting with the inward force of gravity having no resistence. During the collapse, even atoms are unable to maintain their structure, leaving the body of the star as a soup of neutrons. The free eletrons act as a degenerate fermi gas, making them extremely hard to compress, where the resulting outward pressure counters the force of gravity. Once the system is stable, the star contratcs down to a small fraction of its original size with extreme density. In our research, we are building a code to accurately simulate a neutron star and its resulting nuclear interactions at high temperature and high magnetic field. In doing so, we used comparative data to test the this simulation with a corresponding white dwarf code due to their similarities; The compared quantitative aspects were as follows: magnetic field, number density, energy density, pressure, perpendicular pressure, chemical potential, magnetization, and entropy. Overall, it was found that they behaved the same way, and the neutron star simulation is functional.