White dwarfs are remnants of stars with less than 3 solar masses, formed after a star sheds its outer layers, leaving a dense core. Black dwarfs are theoretical, representing white dwarfs that have cooled to the point of emitting negligible light, but none currently exist in the universe due to the long cooling process. Neutron stars occur when a massive star undergoes a supernova, compressing its core to the point where protons and electrons combine to form neutrons, creating a stable structure. The Chandrasekhar limit, set at 1.4 solar masses, defines the maximum mass for white dwarfs; exceeding this limit leads to the formation of neutron stars or black holes. Discussions also touched on the observation of supernovae and the challenges of witnessing such cosmic events with the naked eye.