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  2. Pulsar - Wikipedia

    en.wikipedia.org/wiki/Pulsar

    Pulsars that were discovered before 1993 tend to retain their B names rather than use their J names (e.g. PSR J1921+2153 is more commonly known as PSR B1919+21). Recently discovered pulsars only have a J name (e.g. PSR J0437−4715). All pulsars have a J name that provides more precise coordinates of its location in the sky. [38]

  3. Rotating radio transient - Wikipedia

    en.wikipedia.org/wiki/Rotating_radio_transient

    After the discovery of pulsars in 1967, searches for more pulsars relied on two key characteristics of pulsar pulses in order to distinguish pulsars from noise caused by terrestrial radio signals. The first is the periodic nature of pulsars.

  4. Hulse–Taylor pulsar - Wikipedia

    en.wikipedia.org/wiki/Hulse–Taylor_pulsar

    The pulsar and its neutron star companion both follow elliptical orbits around their common center of mass. The period of the orbital motion is 7.75 hours, and the two neutron stars are believed to be nearly equal in mass, about 1.4 solar masses.

  5. Pulsar planet - Wikipedia

    en.wikipedia.org/wiki/Pulsar_planet

    One potential way to image a planet is to detect its transit in front of the star: in case of pulsar planets, the probability of a planet transiting in front of pulsar is very low because of the small size of pulsars. Spectroscopic analyses of planets are rendered difficult by the complicated spectra of pulsars. Interactions between a planetary ...

  6. PSR J0737−3039 - Wikipedia

    en.wikipedia.org/wiki/PSR_J0737%E2%88%923039

    The orbital decay and the speedup of the orbital period was tested to follow the quadrupole formula with a great precision of 0.013% mainly because of the unique characteristics of the system which has two pulsars, is nearby and possesses an inclination close to 90°. [7] [8] [9]

  7. PSR J0437−4715 - Wikipedia

    en.wikipedia.org/wiki/PSR_J0437%E2%88%924715

    Two other pulsars, PSR B1855+09 and PSR B1937+21 are known to be comparable in stability to atomic clocks, or about 3 parts in 10 14. PSR J0437−4715 is the first MSP to have its X-ray emission detected and studied in detail. [8] It is also the first of only two pulsars to have the full three-dimensional orientation of its orbit determined. [9]

  8. X-ray pulsar - Wikipedia

    en.wikipedia.org/wiki/X-ray_pulsar

    An X-ray pulsar is a type of binary star system consisting of a typical star (stellar companion) in orbit around a magnetized neutron star.The magnetic field strength at the surface of the neutron star is typically about 10 8 Tesla, over a trillion times stronger than the strength of the magnetic field measured at the surface of the Earth (60 μT).

  9. PSR J0952–0607 - Wikipedia

    en.wikipedia.org/wiki/PSR_J0952–0607

    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. [5] 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.