SUMMARY
A white dwarf star in a binary system cannot collapse directly into a neutron star without undergoing a supernova. When a white dwarf exceeds the Chandrasekhar limit of approximately 1.4 solar masses, it triggers a Type Ia supernova instead of collapsing. This occurs because white dwarfs, composed mainly of carbon and oxygen, still possess significant thermonuclear energy for fusion reactions. In contrast, neutron stars form from the collapse of more massive stars with iron cores, where no further fusion can occur, leading to a definitive collapse into a black hole if the Tolman-Oppenheimer-Volkoff limit is exceeded.
PREREQUISITES
- Understanding of white dwarf and neutron star formation
- Familiarity with the Chandrasekhar limit
- Knowledge of Type Ia supernova mechanisms
- Comprehension of the Tolman-Oppenheimer-Volkoff limit
NEXT STEPS
- Research the mechanisms of Type Ia supernovae
- Study the properties and formation processes of neutron stars
- Explore the implications of the Tolman-Oppenheimer-Volkoff limit on stellar evolution
- Investigate the nuclear binding energy curve and its significance in stellar collapse
USEFUL FOR
Astronomers, astrophysicists, and students studying stellar evolution and supernova phenomena will benefit from this discussion.