Vela Pulsar

The Vela Pulsar (PSR J0835-4510 or PSR B0833-45) is a radio, optical, X-ray, and gamma-emitting pulsar associated with the Vela Supernova Remnant in the constellation of Vela. Its parent Type II supernova exploded approximately 11,000–12,300 years ago, about 800 light-years away. It is the brightest pulsar at radio frequencies and spins 11 times per second, with a period of 89.33 milliseconds—the shortest known at its discovery. The remnant travels outward at 1,200 km/s. Its optical component pulses twice for every radio pulse and is the third-brightest among known pulsars (V = 23.6 mag). It is also the brightest persistent object in the high-energy gamma-ray sky, with pulsed emission detected up to 20 TeV, making it one of only two pulsars with such high-energy emissions. The Vela Pulsar is well-known for its glitches—sudden spin-ups in rotation—occurring on average every three years. In 2016, a glitch was observed live for the first time, revealing a brief nulling of pulses and changes in polarization. Another glitch in 2021 decreased its period by about one part in a million. These events reverse nearly 1% of the pulsar's long-term spin-down. The pulsar's association with the Vela Supernova Remnant was confirmed in 1968, providing direct evidence that supernovae form neutron stars. Studies using the Uhuru spacecraft in 1970–71 showed it is separate from but related to the pulsar wind nebula Vela X. The term Vela X initially referred to the entire remnant but was later identified as a distinct nebula driven by the pulsar's energy. The ...