Lecture on Neutron Stars

        Went on my evening walk re-listening to an astronomy lecture on Neutron Stars. Neutron stars are formed in type 2 supernovas. During the process of a star’s death where it’s burning through different elements it finally reaches iron 56 which cannot fuse. This iron core builds up pressure to the Chandrasekhar limit and electron degeneracy pressure takes over. Different outer layers keep burning lighter elements until they reach iron 56, which falls into this core (which is the size of the Earth) to exceed this limit. When the Chandrasekhar limit of 1.4 solar masses is exceeded and the pressure of the electron degeneracy pressure can no longer hold up against gravity the core implodes very fast at .01 the speed of light (I think that is the speed he said) and compresses around two solar masses into a sphere ten miles in diameter. As this takes place electrons and protons are squeezed together forming neutrons and it is the neutron degeneracy pressure that takes over the fight against gravity. Neutron stars spin very fast because of the angular momentum it got as it collapse into a smaller area- like a skater pulling in her arms to spin faster. Neutron stars emit high-energy radiation because of the spin and electrons flowing on its surface between its two magnetic poles- like a lighthouse. These are called Pulsars. This was how neutron stars were first found thirty years after Fritz Zwicky anticipated their structure. The next lecture will be on black holes.