SUMMARY
The formation of a neutron star or a pulsar is determined by the conditions of the core remnant after a supernova explosion. A neutron star becomes a pulsar if it possesses sufficient rotational speed and a strong magnetic field. The process involves the neutron star radiating electromagnetic energy, which gradually slows its rotation. If the core remnant does not exceed the Tolman-Oppenheimer-Volkoff (TOV) limit, a neutron star is formed, while pulsars are characterized by their energetic emissions and magnetic fields that create observable pulses.
PREREQUISITES
- Understanding of supernova mechanisms and remnants
- Knowledge of neutron star and pulsar characteristics
- Familiarity with the Tolman-Oppenheimer-Volkoff (TOV) limit
- Basic concepts of electromagnetic radiation and its effects on stellar bodies
NEXT STEPS
- Research the Tolman-Oppenheimer-Volkoff (TOV) limit and its implications for neutron star formation
- Explore the mechanisms of pulsar emissions and the role of magnetic fields
- Investigate the lifecycle of neutron stars and their transition to pulsars
- Study the accretion processes of matter onto neutron stars and their effects on pulsar characteristics
USEFUL FOR
Astronomers, astrophysicists, and students interested in stellar evolution, particularly those focusing on neutron stars and pulsars.