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A pulsar is a highly magnetized, rotating neutron star that emits beams of electromagnetic radiation, observed as pulses as the star rotates. Pulsars were first discovered in 1967 by Jocelyn Bell Burnell and Antony Hewish while analyzing radio signals from a celestial source. Initially, their periodic nature led to speculation about artificial origins, but they were later identified as natural phenomena.

Pulsars are formed during the supernova collapse of massive stars, leaving behind a dense core composed primarily of neutrons. Their extreme density—often comparable to that of an atomic nucleus—results in intense gravitational and magnetic fields. The rotation of these stars, combined with their magnetic fields, accelerates charged particles along magnetic field lines, producing beams of radiation that sweep across space like a lighthouse beam.

The most common type of pulsar emits radio waves, but some also emit visible light, X-rays, or gamma rays. Their rotational periods range from milliseconds to several seconds, with some pulsars slowing down over time due to energy loss via electromagnetic radiation. Millisecond pulsars, which rotate extremely rapidly (hundreds of times per second), are thought to have been spun up by accreting matter from a companion star in a binary system.

Pulsars are valuable astronomical tools for studying general relativity, gravitational waves, and the interstellar medium. Their precise timing makes them useful for testing Einstein’s theory of relativity, while their distribution can help map the structure of the Milky Way. Some pulsars are also considered candidates for detecting gravitational waves through pulsar timing arrays.

Notable examples include the Crab Pulsar, associated with the Crab Nebula and known for its rapid rotation and strong emissions, and PSR B1937+21, one of the fastest-spinning millisecond pulsars discovered. Ongoing research continues to expand our understanding of these enigmatic objects and their role in astrophysics.