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 planets to be confirmed as discovered.
Pulsar planets are discovered through pulsar timing measurements, to detect anomalies in the pulsation period. Any bodies orbiting the pulsar will cause regular changes in its pulsation. Since pulsars normally rotate at near-constant speed, any changes can easily be detected with the help of precise timing measurements. The discovery of pulsar planets was unexpected; pulsars or neutron stars have previously gone supernova, and it was thought that any planets orbiting such stars would have been destroyed in the explosion.
In 1992, Aleksander Wolszczan and Dale Frail announced the discovery of a multi-planet planetary system around the millisecond pulsar PSR 1257+12. These were the first two extrasolar planets confirmed to be discovered, and thus the first multi-planet extrasolar planetary system discovered, and the first pulsar planets discovered. There was doubt concerning the discovery because of the retraction of the previous pulsar planet, and questions about how pulsars could have planets. However, the planets proved to be real. Two additional planets of lower mass were later discovered by the same technique, although one has since been retracted.
In 2000, the millisecond pulsar PSR B1620−26 was found to have a circumbinary planet (PSR B1620−26 b) that orbits both it and its companion white dwarf, WD B1620–26. This was announced as the oldest planet ever discovered, at 12.6 billion years old. It is currently believed to have originally been the planet of WD B1620–26 before becoming a circumbinary planet, and therefore, while discovered through the pulsar timing method, it did not form the way that PSR B1257+12's planets are thought to have.
In 2006, the magnetar 4U 0142+61, located 13,000 light-years (1.2×1017 km) from Earth, was found to have a circumstellar disk. The discovery was made by a team led by Deepto Chakrabarty of MIT using the Spitzer Space Telescope. The disk is thought to have formed from metal-rich debris left over from the supernova that formed the pulsar roughly 100,000 years ago and is similar to those seen around Sun-like stars, suggesting it may be capable of forming planets in a similar fashion. Pulsar planets would be unlikely to harbour life as we know it, because the high levels of ionizing radiation emitted by the pulsar and the corresponding paucity of visible light.
In 2011, a planet that is theorized to be the remaining core of a star that orbited a pulsar was announced. It orbits millisecond pulsar PSR J1719−1438, and represents a path to planetary status by evaporation of a star. The planet is estimated to have a density of at least 23 times that of water, a diameter of 55,000 km, a mass near that of Jupiter's, and a 2-hour, 10-minute orbital period at 600,000 km. It is thought to be the diamond crystal core remaining from the evaporated white dwarf, with an estimated weight of 2.0×1027 kg (1×1031 carats).
There are three types of pulsar planets known so far. The PSR B1257+12 planets were formed out of the debris of a merged companion star that used to orbit the pulsar when it was a white dwarf. In PSR J1719-1438, the planet most likely is the companion, or what's left of it after being almost entirely blasted away by the extreme irradiation from the nearby pulsar. PSR B1620–26 b is most likely a captured planet.
|Pulsar||Planetary object||Mass||Semimajor axis
|PSR B1957+20||PSR B1957+20 b||22 MJ||−||0.38 days||1988|
|PSR B1620-26||PSR B1620-26 b||2.5 MJ||23||100 years||2003|
|PSR B1257+12||PSR B1257+12 A||0.020 M⊕||0.19||25.262±0.003 days||1994|
|PSR B1257+12 B||4.3 M⊕||0.36||66.5419±0.0001 days||1992|
|PSR B1257+12 C||3.90 M⊕||0.46||98.2114±0.0002 days||1992|
|PSR B0943+10||PSR B0943+10 b||2.8 MJ||1.8||730 d||2014|
|PSR B0943+10 c||2.6 MJ||2.9||1460 d||2014|
|PSR B0329+54||PSR B0329+54 b||1.97 ± 0.19 M⊕||10.26 ± 0.07||27.76 ± 0.03 years||2017|
|PSR J2322-2650||PSR J2322-2650 b||0.7949 MJ||0.0102||0.322963997 d||2017|
|Pulsar||Planetary object||Mass||Semimajor axis
|PSR J1719-1438||PSR J1719-1438 b||~1 MJ||0.004||2.176951032 hours||2011 August 25|
|PSR J1544+4937||PSR J1544+4937 b||18 MJ||0.00537||0.1207729895±0.0000000001 d||2013|
|PSR B1937+21||PSR B1937+21 b||~0.0001 M🜨?||2.71||1999|
|4U 0142+61||debris disk||2006|
|1E 2259+586||candidate debris disk||2009|
|Geminga||Geminga b||1.7 M⊕|
|PSR B1829-10||PSR 1829-10 A||10 M⊕|
|PSR B1257+12||PSR B1257+12 D||0.0004 M⊕|
|PSR B1828-11||PSR B1828-11 A||3 M⊕|
|PSR B1828-11 B||12 M⊕|
|PSR B1828-11 C||8 M⊕|
|PSR B0329+54||PSR B0329+54A||0.3 M⊕|
|PSR B0329+54B||2.2±0.002 M⊕|