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A neutron star is the collapsed core of a massive supergiant star, which had a total mass of between 10 and 25 solar masses, possibly more if the star was especially metal-rich. Except for black holes, and some hypothetical objects, neutron stars are the smallest and densest currently known class of stellar objects. Neutron stars have a radius on the order of 10 kilometres (6.2 mi) and a mass of about 1.4 solar masses. They result from the supernova explosion of a massive star, combined with gravitational collapse, that compresses the core past white dwarf star density to that of atomic nuclei.
PSR B1257+12, previously designated PSR 1257+12, alternatively designated PSR J1300+1240, is a millisecond pulsar located 2,300 light-years from the Sun in the constellation of Virgo, rotating at about 161 times per second. It is also named Lich, after a powerful, fictional undead creature of the same name.
Pulsar planets are planets that are found orbiting pulsars, or rapidly rotating neutron stars. The first such planets to be discovered were around a millisecond pulsar and were the first extrasolar planet to be confirmed as discovered.
A pulsar is a highly magnetized rotating compact star that emits beams of electromagnetic radiation out of its magnetic poles. This radiation can be observed only when a beam of emission is pointing toward Earth, and is responsible for the pulsed appearance of emission. Neutron stars are very dense and have short, regular rotational periods. This produces a very precise interval between pulses that ranges from milliseconds to seconds for an individual pulsar. Pulsars are one of the candidates for the source of ultra-high-energy cosmic rays.
Andrew Geoffrey Lyne FRS is a British physicist. Lyne is Langworthy Professor of Physics in the School of Physics and Astronomy, University of Manchester, as well as an ex-director of the Jodrell Bank Observatory. Despite retiring in 2007 he remains an active researcher within the Jodrell Bank Pulsar Group. Lyne was educated at The Portsmouth Grammar School, the Royal Naval School, Tal Handaq, Malta and at St. John's College at the University of Cambridge, continuing to the University of Manchester for a PhD in Radio Astronomy. Lyne writes that he is "mostly interested in finding and understanding radio pulsars in all their various forms and with their various companions. Presently, I am most occupied with the development of new multibeam search systems at Jodrell and Parkes, in order to probe deeper into the Galaxy, particularly for millisecond pulsars, young pulsars and any that might be in binary systems."
PSR J0737−3039 is the only known double pulsar. It consists of two neutron stars emitting electromagnetic waves in the radio wavelength in a relativistic binary system. The two pulsars are known as PSR J0737−3039A and PSR J0737−3039B. It was discovered in 2003 at Australia's Parkes Observatory by an international team led by the radio astronomer Marta Burgay during a high-latitude pulsar survey.
The Hulse–Taylor binary 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.
A binary pulsar is a pulsar with a binary companion, often a white dwarf or neutron star. Binary pulsars are one of the few objects which allow physicists to test general relativity because of the strong gravitational fields in their vicinities. Although the binary companion to the pulsar is usually difficult or impossible to observe directly, its presence can be deduced from the timing of the pulses from the pulsar itself, which can be measured with extraordinary accuracy by radio telescopes.
The Vela Pulsar is a radio, optical, X-ray- and gamma-emitting pulsar associated with the Vela Supernova Remnant in the constellation of Vela. Its parent Type II supernova exploded approximately 11,000–12,300 years ago.
The Tolman–Oppenheimer–Volkoff limit is an upper bound to the mass of cold, nonrotating neutron stars, analogous to the Chandrasekhar limit for white dwarf stars.
Tempo is a computer program to analyze radio observations of pulsars. Once enough observations are available, Tempo can deduce the pulsar rotation rate and phase, astrometric position and rates of change, and parameters of binary systems, by fitting models to pulse times of arrival measured at one or more terrestrial observatories. This is a non-trivial procedure because much larger effects must be removed before the detailed fit can be performed. These include:
PSR B0329+54 is a pulsar approximately 3,460 light-years away in the constellation of Camelopardalis. It completes one rotation every 0.71452 seconds and is approximately 5 million years old.
PSR B1259−63 is a pulsar and member of an eclipsing binary star system with the blue O9.5Ve-class star LS 2883. The pair has an eccentric orbit that is inclined to the line of sight from Earth by about 36°, leading to a 40-day-long eclipse each time the pulsar passes behind the star. The pulsar has a period of about 48 ms and a luminosity of 8.3 × 1035 erg/s. It emits very high energy gamma rays that vary on a time scale of several days.
PSR B1257+12 b, alternatively designated PSR B1257+12 A, also named Draugr, is an extrasolar planet approximately 2,300 light-years away in the constellation of Virgo. The planet is the innermost object orbiting the pulsar PSR B1257+12, making it a pulsar planet in the dead stellar system. It is about twice as massive as the Moon, and is listed as the least massive planet known, including among the planets in the Solar System.
PSR B1257+12 c, alternatively designated PSR B1257+12 B, also named Poltergeist, is an extrasolar planet approximately 2,300 light-years away in the constellation of Virgo. It was one of the first planets ever discovered outside the Solar System, and is one of three pulsar planets known to be orbiting the pulsar PSR B1257+12.
PSR B1257+12 C, alternatively designated PSR B1257+12 d and also named Phobetor, is a super-Earth exoplanet orbiting the pulsar PSR B1257+12 approximately 2,315 light-years (710 parsecs, or nearly 2.1908×1016 km) away from Earth in the constellation of Virgo. It was one of the first planets ever discovered outside the Solar System. It was discovered using the pulsar timing method, where the regular pulses of a pulsar are measured to determine if there is a planet causing variations in the data.
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. 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. PSR B1937+21 was discovered in 1982 by Don Backer, Shri Kulkarni, Carl Heiles, Michael Davis, and Miller Goss.
PSR J0108−1431 is a solitary pulsar located at a distance of about 130 parsecs (424 light-years) in the constellation Cetus. This pulsar was discovered in 1994 during the Parkes Southern Pulsar Survey. It is considered a very old pulsar with an estimated age of 166 million years and a rotation period of 0.8 seconds. The rotational energy being generated by the spin-down of this pulsar is 5.8 × 1023 W and the surface magnetic field is 2.5 × 107 T. As of 2008, it is the second faintest known pulsar.
PSR B0943+10 is a pulsar 2,000 light years from Earth in the direction of the constellation of Leo. It was discovered at Pushchino in December 1968, original designation of this pulsar was PP 0943, it became the first pulsar, discovered by Soviet astronomers.
Ingrid Stairs is a Canadian astronomer currently based at the University of British Columbia. She studies pulsars and their companions as a way to study binary pulsar evolution, pulsar instrumentation and polarimetry, and Fast Radio Bursts (FRBs). She was awarded the 2017 Rutherford Memorial Medal for physics of the Royal Society of Canada, and was elected as a Fellow of the American Physical Society in 2018.
References
- ↑ Smith, D. A.; Guillemot, L.; Camilo, F.; Cognard, I.; et al. (2008). "Pulsar timing for the Fermi gamma-ray space telescope". Astronomy and Astrophysics. 492 (3): 923–931. arXiv: 0810.1637 . Bibcode:2008A&A...492..923S. doi:10.1051/0004-6361:200810285.
- 1 2 "PSR B1828-10 -- Pulsar". SIMBAD. Retrieved 2014-07-02.
- ↑ Bailes, M.; Lyne, A. G.; Shemar, S. L. (1993). "Limits on pulsar planetary systems from the Jodrell Bank timing database". Planets around pulsars; Proceedings of the Conference. California Inst. of Technology, Pasadena. pp. 19–30. Bibcode:1993ASPC...36...19B.
- ↑ Stairs, I. H.; Lyne, A. G.; Shemar, S. L. (2000). "Evidence for free precession in a pulsar". Nature. 406 (6795): 484–486. Bibcode:2000Natur.406..484S. doi:10.1038/35020010. PMID 10952302.
- ↑ Link, Bennett; Epstein, Richard I. "Precession Interpretation of the Isolated Pulsar PSR B1828-11". The Astrophysical Journal. 556 (1): 392–398. arXiv: astro-ph/0101434 . Bibcode:2001ApJ...556..392L. doi:10.1086/321581.
- ↑ Akgün, Taner; Link, Bennett; Wasserman, Ira (2006). "Precession of the isolated neutron star PSR B1828-11". Monthly Notices of the Royal Astronomical Society. 365 (2): 653–672. arXiv: astro-ph/0506606 . Bibcode:2006MNRAS.365..653A. doi:10.1111/j.1365-2966.2005.09745.x.
- ↑ Liu; et al. (2007). "PSR B1828-11: a precession pulsar torqued by a quark planet?". Monthly Notices of the Royal Astronomical Society: Letters . 381 (1): 1–5. arXiv: astro-ph/0411133 . Bibcode:2007MNRAS.381L...1L. doi:10.1111/j.1745-3933.2007.00337.x.
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