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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]
The Hulse–Taylor pulsar (known as PSR B1913+16, PSR J1915+1606 or PSR 1913+16) is a binary star system composed of a neutron star and a pulsar which orbit around their common center of mass. It is the first binary pulsar ever discovered.
In addition to a double pulsar system, a whole range of differing two-body systems are known where only one member of the system is a pulsar. Known examples are variations on a binary star : A pulsar–white dwarf system; e.g, PSR B1620−26. A pulsar–neutron star system, e.g, PSR B1913+16.
PSR J0348+0432 is a pulsar–white dwarf binary system in the constellation Taurus. It was discovered in 2007 with the National Radio Astronomy Observatory's Robert C. Byrd Green Bank Telescope in a drift-scan survey. [2] In 2013, a mass measurement for this neutron star was announced: slightly over two times the mass of the Sun (2.01 ± 0.04 M ...
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.
Typical pulsar periods for young pulsars are of the order of one second, and they increase with time; the very short periods exhibited by so-called millisecond pulsars are due to the transfer of material from a binary companion. The pulse period of PSR B1620-26 is a few milliseconds, providing strong evidence for matter transfer.
PSR J1946+2052 is a short-period binary pulsar system located 11,000–14,000 light-years (3,500–4,200 pc) away from Earth in the constellation Vulpecula.The system consists of a pulsar and a neutron star orbiting around their common center of mass every 1.88 hours, which is the shortest orbital period among all known double neutron star systems as of 2022.
AR Scorpii (AR Sco) is a binary pulsar that consists of a white dwarf and a red dwarf. [3] It is located close to the ecliptic plane in the constellation Scorpius. Parallax measurements made by Gaia put the system at a distance of about 380 light-years (120 parsecs). [4] A broadband optical light curve for AR Scorpii, plotted from Kepler data [6]