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In rotation-powered pulsars, the beam is the result of the rotational energy of the neutron star, which generates an electrical field and very strong magnetic field, resulting in the acceleration of protons and electrons on the star surface and the creation of an electromagnetic beam emanating from the poles of the magnetic field.
Neutron stars, including pulsars, can be as small as about 12 miles across—if Earth rotated at the same speed as one of these stars, an Earth day would be nearly 4,300 hours long.
Stellar rotation is the angular motion of a star about its axis. The rate of rotation can be measured from the spectrum of the star, or by timing the movements of active features on the surface. The rotation of a star produces an equatorial bulge due to centrifugal force. As stars are not solid bodies, they can also undergo differential rotation.
PSR J0952–0607 is a massive millisecond pulsar in a binary system, located between 3,200–5,700 light-years (970–1,740 pc) from Earth in the constellation Sextans. [6] It holds the record for being the most massive neutron star known as of 2022, with a mass 2.35 ± 0.17 times that of the Sun—potentially close to the Tolman–Oppenheimer–Volkoff mass upper limit for neutron stars.
Millisecond pulsars have been detected in radio, X-ray, and gamma ray portions of the electromagnetic spectrum. The leading hypothesis for the origin of millisecond pulsars is that they are old, rapidly rotating neutron stars that have been spun up or "recycled" through accretion of matter from a companion star in a close binary system.
In 2004, Taylor and Joel M. Weisberg published a new analysis of the experimental data to date, concluding that the 0.2% disparity between the data and the predicted results is due to poorly known galactic constants, including the Sun's distance from the Galactic Center, the pulsar's proper motion and its distance from Earth. While there are ...
PSR J1748−2446ad is the fastest-spinning pulsar known, at 716 Hz (times per second), [2] or 42,960 revolutions per minute.This pulsar was discovered by Jason W. T. Hessels of McGill University on November 10, 2004, and confirmed on January 8, 2005.
The formation scenarios have consequences for the planets' composition: A planet formed from supernova debris is likely rich in metals and radioactive isotopes [15] and may contain large quantities of water; [18] one formed through the break-up of a white dwarf would be carbon rich [15] and consist of large amounts of diamond; [19] an actual white dwarf fragment would be extremely dense. [15]