Vela Pulsar The fast rotating neutron star

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#Space #astronomy #darkvoid #pulsar • The Vela Pulsar (PSR B0833-45 / PSR J0835-4510 / 2U 0832-45) is a pulsar associated with the Vela Supernova Rest in the constellation of the same name. The relationship between both astronomical objects, carried out by astronomers from the University of Sydney in 1968, was direct proof that supernovae give rise to neutron stars. It is located about 936 light years from the solar system. • The Vela Pulsar emits at different wavelengths, from radio frequencies to gamma rays. It has a period of 89 ms, the shortest known at the time of its discovery. It is estimated that the remains of the supernova explosion, which occurred about 11,400 years ago, travel at a speed of 1200 km/s. • It has the third brightest optical component among all known pulsars, pulsating twice for each single radio pulse. Its apparent magnitude varies between +23.2 and +25.2, receiving the name of variable HU Velorum. The emission in visible light has its origin entirely in the magnetosphere. It is the brightest persistent object in the sky in rays high energy gamma. • Images of the compact nebula around the Vela Pulsar, obtained with the Chandra X-ray Observatory, show an arch-like structure in the forward part of the cloud; It is believed that this arc—and a smaller one within it—are edges of rings of X-ray emission from high-energy particles produced by the pulsar. Perpendicular to the arcs are jets emanating from the central pulsar, pointing in the same direction as the movement of the pulsar. It is thought that the origin of this activity is the enormous electric fields caused by the combination of the rapid rotation and the intense magnetic fields of the neutron star.

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