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This interpretation suggests that the Quran referenced pulsars over 1,400 years ago, long before their discovery by modern science. [80] However, this interpretation is debated among scholars. Some argue that the term "Tariq" refers to a bright star visible at night, such as Venus, and does not specifically denote pulsars. They emphasize that ...
PSR B1919+21 is a pulsar with a period of 1.3373 seconds [4] and a pulse width of 0.04 seconds. Discovered by Jocelyn Bell Burnell on 28 November 1967, it is the first discovered radio pulsar. [5]
PSR B1937+21 is a pulsar located in the constellation Vulpecula a few degrees in the sky away from the first discovered pulsar, PSR B1919+21. [1] The name PSR B1937+21 is derived from the word "pulsar" and the declination and right ascension at which it is located, with the "B" indicating that the coordinates are for the 1950.0 epoch.
An intermediate-mass binary pulsar (IMBP) is a pulsar-white dwarf binary system with a relatively long spin period of around 10–200 ms consisting of a white dwarf with a relatively high mass of approximately . [7] The spin periods, magnetic field strengths, and orbital eccentricities of IMBPs are significantly larger than those of low mass binary pulsars (LMBPs). [7]
X-ray pulsars or "accretion-powered pulsars": a class of X-ray binaries. Low-mass X-ray binary pulsars: a class of low-mass X-ray binaries (LMXB), a pulsar with a main sequence star, white dwarf or red giant. Millisecond pulsar (MSP) ("recycled pulsar"). "Spider Pulsar", a pulsar where their companion is a semi-degenerate star. [116]
PSR J1719-1438 was discovered in 2011 by the High Time Resolution Survey, a radio astronomy search for astronomical objects that rapidly vary in radio brightness, such as pulsars. [1] Timing measurements using the Parkes Telescope and Lovell Telescope showed that it has a low-mass companion: PSR J1719-1438 b . [ 1 ]
The Crab Pulsar is one of very few pulsars to be identified optically. The optical pulsar is roughly 20 kilometres (12 mi) in diameter and has a rotational period of about 33 milliseconds , that is, the pulsar "beams" perform about 30 revolutions per second. [ 6 ]
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]