pulsar planet

The formation of planets requires the existence of a protoplanetary disk, most theories also require a "dead zone" within it where there is no turbulence. There, planetesimals can form and accumulate without falling into the star.{{sfn|Martin|Livio|Palaniswamy|2016|p=1}} Compared to young stars, pulsars have a much higher luminosity and thus the formation of a dead zone is hindered by the ionization of the disk by the pulsar's radiation,{{sfn|Martin|Livio|Palaniswamy|2016|p=8}} which allows the magnetorotational instability to trigger turbulence and thus destroy the dead zone.{{sfn|Martin|Livio|Palaniswamy|2016|p=4}} Thus, a disk needs to have a large mass if it is to give rise to planets.{{sfn|Wolszczan|2015}}

There are several processes{{efn|Pre-existent planets surviving the supernova are known as a "Salamander" scenario; in mythology salamanders are thought to survive fires. Planets formed from stellar debris are known as "Memnonides" scenarios; Memnonides, according to the Roman poet Ovid, were birds formed from the ashes of the warrior Memnon.{{sfn|Phinney|Hansen|1993|p=371}}}} that could give rise to planetary systems:

• "First-generation" planets are planets that orbited the star before it went supernova and became a pulsar:{{sfn|Patruno|Kama|2017|p=1}} Massive stars tend to lack planets, possibly due to the difficulty in detecting them around very bright stars but also because the radiation from such stars would destroy the protoplanetary disks. Planets orbiting within about four astronomical units of the star risk being engulfed and destroyed when it becomes a red giant or red supergiant. During the supernova, the system loses about half of its mass and unless the pulsar is ejected in the same direction as the planet was moving at the time of the supernova, the planets are likely to detach from the system. None of the known pulsar planet systems are likely to have formed in this process.{{sfn|Martin|Livio|Palaniswamy|2016|p=2}}
• "Second-generation" planets from material that falls back on the pulsar after a supernova:{{sfn|Patruno|Kama|2017|p=1}} The material could theoretically reach a mass comparable to that of a protoplanetary disk,{{sfn|Martin|Livio|Palaniswamy|2016|p=2}} but is likely to dissipate too fast to allow the formation of planets. There are no known examples of planets around young pulsars.{{sfn|Martin|Livio|Palaniswamy|2016|p=3}}{{sfn|Margalit|Metzger|2017|p=2798}}
• "Third-generation" planets:{{sfn|Patruno|Kama|2017|p=1}} A companion star is destroyed through the interaction with a pulsar, forming a low-mass disk. Pulsars can emit energetic radiation that heats the companion star, until it overflows its Roche lobe and is eventually destroyed. Another mechanism is the emission of gravitational waves, which shrink the orbit until the companion star (in these cases often a white dwarf) breaks up.{{sfn|Martin|Livio|Palaniswamy|2016|p=3}} In a third mechanism, the pulsar penetrates the envelope of a larger star, causing it to break up and form a disk{{sfn|Hirai|Podsiadlowski|2022|p=4545}} around the pulsar.{{sfn|Hirai|Podsiadlowski|2022|p=4553}} Disks formed in these processes are much more massive than these formed through fallback and thus persist for longer times, allowing the formation of planets.{{sfn|Martin|Livio|Palaniswamy|2016|p=3}} They also contain heavy elements that are essential building blocks for planets, and part of the disk will be accreted by the pulsar and spins it up in the process.{{sfn|Euvel|1992|p=668}} Alternatively, a light white dwarf is destroyed by the interaction with a more massive one; the light white dwarf gives rise to a debris disk that generates a planet while the larger white dwarf becomes a pulsar.{{sfn|Podsiadlowski|Pringle|Rees|1991|p=783}}
• A companion star may be destroyed during the interaction with a pulsar but leave a planet-sized remnant,{{sfn|Martin|Livio|Palaniswamy|2016|p=4}} such a system is known as a "black widow".{{sfn|Bailes|Bates|Bhalerao|Bhat|2011|p=1717}}
• Finally, it is possible that planets from companion stars or rogue planets are captured by a pulsar,{{sfn|Nekola Novakova|Petrasek|2017|p=1}} or that a pulsar merged with the original host star of the planets.{{sfn|Podsiadlowski|Pringle|Rees|1991|p=784}} The latter process would form a "common envelope" which eventually breaks down to form a disk from which planets can develop.{{sfn|MacRobert|2005|p=26}}

The formation scenarios have consequences for the planets' composition: A planet formed from supernova debris is likely rich in metals and radioactive isotopes{{sfn|Nekola Novakova|Petrasek|2017|p=1}} and may contain large quantities of water;{{sfn|Patruno|Kama|2017|p=10}} one formed through the break-up of a white dwarf would be carbon rich{{sfn|Nekola Novakova|Petrasek|2017|p=1}} and consist of large amounts of diamond;{{sfn|Margalit|Metzger|2017|p=2800}} an actual white dwarf fragment would be extremely dense.{{sfn|Nekola Novakova|Petrasek|2017|p=1}} {{As of|2022}}, the most common type of planet around a pulsar is a "diamond planet", a very low-mass white dwarf.{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2446}} Other objects around pulsars could include asteroids, comets and planetoids.{{sfn|Mottez|Heyvaerts|2011|p=1}} More speculative scenarios are planets consisting of strange matter, which could occur much more close to the pulsars than ordinary matter planets, potentially emitting gravitational waves.{{sfn|Kuerban|Geng|Huang|2019|p=1}}

Planets can interact with the magnetic field of a pulsar to produce so-called "Alfvén wings," these are wing-shaped electrical currents around the planet which inject energy into the planet{{sfn|Mottez|Heyvaerts|2011|p=8}} and could produce detectable radio emissions.{{sfn|Mottez|Heyvaerts|2011|p=9}}

Pulsars are extremely precise clocks{{sfn|Wolszczan|2015}} and pulsar timing is highly regular. It is thus possible to detect very small objects around pulsars, down to the size of large asteroids,{{sfn|Martin|Livio|Palaniswamy|2016|p=1}} from changes in the timing of the pulsar hosting them. The timing needs to be corrected for the effects of the motions of Earth and the Solar System, errors in the position estimates of the pulsar and of the travel times of the radiation across the interstellar medium. Pulsars spin and slow down over time in highly regular fashion;{{sfn|Wolszczan|2015}} planets alter this pattern through their gravitational attraction on the pulsar, causing a Doppler shift in the pulses.{{sfn|Flam|1992|p=290}} The technique could in theory be also used to detect exomoons around pulsar planets.{{sfn|Lewis|Sackett|Mardling|2008|p=156}} There are limitations to pulsar planet visibility, however; pulsar glitches and changes in the pulsation mode can mimick the existence of planets.{{sfn|Kerr|Johnston|Hobbs|Shannon|2015|p=1}}

The first{{efn|The earlier detection of the planets HD 114762 b and Gamma Cephei Ab was considered uncertain at the time and so they are not considered the first discovered exoplanets;{{sfn|Veras|2016|p=1}} additionally HD 114762 b was later discovered to be a star (red dwarf rather than a planet.{{sfn|Kiefer|2019|p=1}})}} extrasolar planets to be discovered (in 1992 by Dale Frail and Aleksander Wolszczan) were the pulsar planets around PSR B1257+12.{{sfn|Callegari|Ferraz-Mello|Michtchenko|2006|p=381}} The discovery demonstrated that exoplanets can be detected from Earth,{{sfn|Wolszczan|1994|p=542}} and led to the expectation that extrasolar planets might not be uncommon.{{sfn|Wolszczan|2015}} {{As of|2016}}{{sfn|Veras|2016|p=17}} the least massive known extrasolar planet (PSR B1257+12 A, only {{Earth mass|0.02}}) is a pulsar planet.{{sfn|Lewis|Sackett|Mardling|2008|p=153}}

However, the size and particular spectroscopic traits makes actually visualizing such planets very difficult.{{sfn|Nekola Novakova|Petrasek|2017|p=1}} 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 magnetic field, the pulsar and the thermal emissions of planets are more likely avenues of getting information on the planets.{{sfn|Nekola Novakova|Petrasek|2017|p=2}}

Pulsar planets have been invoked to explain certain astronomical phenomena, such as X-ray bursts from soft gamma repeaters.{{sfn|Kurban|Zhou|Wang|Huang|2024|p=2}}

{{As of|2022}} only about half-dozen{{efn|The NASA Exoplanet Archive has seven planets listed for bodies with the name "PSR" {{As of|2023|3|25|lc=y}}{{sfn|NASAEp|2023}} while the Extrasolar Planets Encyclopedia has 24 planets listed for the same criteria.{{sfn|EPE|2023}}}} pulsar planets are known,{{sfn|Hirai|Podsiadlowski|2022|p=4553}} implying an occurrence rate of no more than one planetary system per 200 pulsars.{{efn|For comparison, it is believed that one fourth to one fifth of all known white dwarfs—the other kind of stellar corpse—bear planets.{{sfn|Veras|Vidotto|2021|p=1702}}}}{{sfn|Hirai|Podsiadlowski|2022|p=4554}} Most of the planet formation scenarios require that the precursor be a binary star with one star much more massive than the other, and that the system survives the supernova that generated the pulsar. Both these conditions are rarely met and thus the formation of pulsar planets is a rare process.{{sfn|Martin|Livio|Palaniswamy|2016|p=4}} Additionally, planets and their orbits would have to survive the energetic radiation emitted by pulsars, including X-rays, gamma rays and energetic particles ("pulsar wind").{{sfn|Patruno|Kama|2017|p=1}} This would be particularly important for millisecond pulsars that were spun up by accretion, while they formed X-ray binaries; the radiation emitted under these circumstances would evaporate any planet.{{sfn|Miller|Hamilton|2001|p=864}} Pulsars remain visible for only a few million years, less than the time it takes for a planet to form, thus limiting the chance of observing one.{{sfn|Miller|Hamilton|2001|p=869}}

Based on the known occurrence rate of pulsar planets, there might be as many as 10 million of them in the Milky Way.{{efn|By comparison, the Milky Way has about 100–400 billion stars,{{sfn|Stellato|2020|p=1}} most of which are thought to feature planets.{{sfn|Cassan|Kubas|Beaulieu|Dominik|2012|p=167}}}}{{sfn|Patruno|Kama|2017|p=2}} All known pulsar planets are found around millisecond pulsars,{{sfn|Martin|Livio|Palaniswamy|2016|p=1}} these are old pulsars that were spun up through the accretion of mass from a companion. {{as of|2015}} there are no known planets around young pulsars;{{sfn|Spiewak|Bailes|Barr|Bhat|2018|p=470}} they are less regular than millisecond pulsars, increasing the pulsar timing error and thus making planet detection more difficult.{{sfn|Nekola Novakova|Petrasek|2017|p=2}}

{{OrbitboxPlanet begin|name=parameters of known pulsar{{efn|Planets are named in order of discovery, beginning with a lowercase "b" which comes after the star's name. In multiple star systems, the stars are given an uppercase letter after the system's name, but beginning with "A" for the main star.{{sfn|IAU}}}}{{efn|Should be divided by ~318 to convert from Earth mass to Jupiter mass}}|table_ref={{sfn|NASAEp|2023}}}}{{efn|name=Radius1}}

|-

|M62H b

|{{Jupiter mass|>2.47}}

|

|{{val|0.132935}}

|~

|~

|{{Jupiter radius|<0.653}}

|-

|PSR B1257+12 b

|{{Earth mass|0.02}} ({{Jupiter mass|6.3 × 10⁻⁵}})

|0.19

|25.262

|0

|~

|~

|-

|PSR B1257+12 c

|{{Earth mass|4.3}} ({{Jupiter mass|0.0135}})

|0.36

|66.5419

|0.0186

|~

|

|-

|PSR B1257+12 d

|{{Earth mass|3.9}} ({{Jupiter mass|0.0123}})

|0.46

|98.2114

|0.03

|~

|

|-

|PSR B1620-26 b

|{{Jupiter mass|2.5}}

|23

|34,675

|~

|~

|{{Jupiter radius|1.18}}{{sfn|NASAcatalog|2024|loc=PSR B1620-26 b}}

|-

|PSR J1719-1438 b

|{{Jupiter mass|1.2}}

|0.0044

|0.090706293

|0.06

|~

|{{Jupiter radius|0.4}}{{sfn|NASAcatalog|2024|loc=PSR J1719-1438 b}}

|-

|PSR J2322-2650 b

|{{Jupiter mass|0.7949}}

|0.0102

|0.322963997

|0.0017

|~

|{{Jupiter radius|1.24}}{{sfn|NASAcatalog|2024|loc=PSR J2322-2650 b}}

|-

|PSR J1748-2021H b

|{{Jupiter mass|7.54}}

|0.0111

|0.360787526{{sfn|EPE|2024|loc=PSR J1748-2021H b}}

|~

|~

|~

|-

|PSR J0636+5129 b

|{{Jupiter mass|8.5}}

|0.0036

|0.0665513392

|~

|60

|{{Jupiter radius|0.74}}{{sfn|EPE|2024|loc=PSR J0636+5129 b}}

|-

|PSR J1807-2459 A b

|{{Jupiter mass|10.5}}

|~

|0.07{{sfn|EPE|2024|loc=PSR J1807-2459 A b}}

|~

|~

|~

|-

|PSR B1802-07 b

|{{Jupiter mass|10}}

|0.008098

|0.071092

|0.0000003{{sfn|EPE|2024|loc=PSR B1802-07 b}}

|~

|~

|-

|PSR J1211-0633 b

|{{Jupiter mass|10}}

|0.0116

|0.38634962{{sfn|EPE|2024|loc=PSR J1211-0633 b}}

|~

|~

|~

|-

|PSR J0312-0921 b

|{{Jupiter mass|10.47}}

|0.00465

|0.0975{{sfn|EPE|2024|loc=PSR J0312-0921 b}}

|~

|~

|~

|-

|PSR J1824-2452G b

|{{Jupiter mass|11}}

|0.004875

|0.1046

|0.0000003

|~

|~

|-

|PSR J1928+1245 b

|{{Jupiter mass|11}}

|0.005825

|0.1366347269{{sfn|EPE|2024|loc=PSR J1928+1245 b}}

|~

|~

|~

|-

|PSR J1824-2452M b

|{{Jupiter mass|11}}

|0.00854

|0.242519219 {{sfn|EPE|2024|loc=PSR J1824-2452M b}}

|~

|~

|~

|-

|PSR J1630+3550 b

|{{Jupiter mass|11.3}}

|~

|0.315863166

|0.00042

|~

|~

|-

|PSR J2241-5236 b

|{{Jupiter mass|12}}

|~

|0.1456722395{{sfn|EPE|2024|loc=PSR J2241-5236 b}}

|~

|~

|~

|-

|PSR J1311-3430 b

|{{Jupiter mass|12}}

|~

|0.065115{{sfn|EPE|2024|loc=PSR J1311-3430 b}}

|~

|~

|~

|-

{{Orbitbox end}}

M62H is a millisecond pulsar located in the constellation Ophiuchus. It is located in the globular cluster Messier 62,{{sfn|Vleeschower|Corongiu|Stappers|Freire|2024|p=1436}} at a distance of {{convert|5600|pc}} from Earth.{{sfn|Oliveira|Ortolani|Barbuy|Kerber|2022|p=1}} The pulsar was discovered in 2024 using the MeerKAT radio telescope.{{sfn|Vleeschower|Corongiu|Stappers|Freire|2024|p=1436}} M62H has a rotational period of 3.70 milliseconds, meaning it completes 270 rotations per second (270 Hz).{{sfn|Vleeschower|Corongiu|Stappers|Freire|2024|p=1440}} Its planetary companion has a minimum mass of {{Jupiter mass|2.5|link=y}} and a median mass of {{jupiter mass|2.83|link=y}}, assuming a mass of {{Solar mass|1.4|link=y}} for the pulsar. Its minimum density is of 11 g/cm{{sup|3}}. Assuming the median mass, it implies a maximum radius of {{convert|48850|km}}.{{sfn|Vleeschower|Corongiu|Stappers|Freire|2024|p=1454}} The planet takes just {{Convert|0.133|day|hour}} to complete an orbit, and is located at a distance equivalent to 0.49% of an astronomical unit from M62H.{{sfn|Vleeschower|Corongiu|Stappers|Freire|2024|p=1444}}

The pulsar PSR B1257+12, {{val|710|43|38}} parsecs away{{sfn|Yan|Shen|Yuan|Wang|2013|p=166}} in the constellation Virgo, was confirmed to have planets in 1992 based on observations made with the Arecibo Observatory.{{sfn|Cowen|1994|p=151}} The system consists of one tiny planet with a mass of {{val|0.02|0.002}} Earth masses and two Super-Earths with masses {{val|4.3|0.2}} and {{val|3.9|0.2}} times that of Earth, assuming that the pulsar has a mass of 1.4 solar masses.{{sfn|Wolszczan|2008|p=2}} They most likely formed from a protoplanetary disk,{{sfn|Martin|Livio|Palaniswamy|2016|p=1}} probably generated from the partial destruction of a companion star.{{sfn|Martin|Livio|Palaniswamy|2016|p=3}} Computer simulations have shown that the system should be stable for at least one billion years{{sfn|Wolszczan|2008|p=2}} and that exomoons could survive in the system.{{sfn|Donnison|2010|p=1919}} The system resembles the inner Solar System;{{sfn|Wolszczan|2015}} the planets orbit the pulsar at distances comparable to that of Mercury to the Sun and may have comparable surface temperatures.{{sfn|Wolszczan|Frail|1992|p=146}} Reports of additional bodies in this system might be due to solar disturbances.{{sfn|Hansen|Shih|Currie|2009|p=387}}

A cthonian planet{{sfn|Iorio|2021|p=1}} with a mass comparable to Jupiter but less than 40% of its radius orbits the pulsar PSR J1719-1438.{{efn|Sometimes also known as PSR J1719-14, per {{SIMBAD link|id=Psr+J1719-14|label=PSR J1719-14}}}}{{sfn|Martin|Livio|Palaniswamy|2016|p=1}} This planet is probably the carbon-rich remnant of a companion star that was evaporated by the pulsar's radiation{{sfn|Martin|Livio|Palaniswamy|2016|p=4}} and has been described as a "diamond planet".{{efn|Its density-mass-radius characteristics imply that it consists entirely of diamond.{{sfn|Smith|Eggert|Jeanloz|Duffy|2014|p=3}}}}{{sfn|Patruno|Kama|2017|p=1}}

A circumbinary planet with a mass of {{val|2.5|1}} Jupiter masses{{sfn|Wolszczan|2008|p=3}} orbits around PSR B1620-26, a binary star consisting of a pulsar and a white dwarf{{sfn|Martin|Livio|Palaniswamy|2016|p=1}} in the globular cluster M4.{{sfn|Wolszczan|2015}} This planet may have been captured into the pulsar's orbit, a process which is particularly likely within the packed environment of a globular cluster,{{sfn|Nekola Novakova|Petrasek|2017|p=1}} and may be about 12.6 billion years old, making it the oldest-known planet.{{efn|An alternative interpretation is that the planet formed through a common envelope, which could make it as young as 500 million years.{{sfn|MacRobert|2005|p=26}}}}{{sfn|Pasqua|Assaf|2014|p=1}} Its existence may demonstrate that planets can form in metal-poor medium including the globular clusters.{{sfn|Setiawan|Klement|Henning|Rix|2010|p=1642}}

PSR J2322-2650 seems to have a roughly Jupiter-mass companion. The radiation from the pulsar could be heating it to about {{val|2300|u=K}}; a light source observed close to the pulsar may be the planet.{{sfn|Spiewak|Bailes|Barr|Bhat|2018|p=474}} This pulsar is considerably less luminous than many, which may explain why the planet has survived to this day.{{sfn|Spiewak|Bailes|Barr|Bhat|2018|p=476}}

Timing variations of the pulsars PSR B1937+21 and PSR J0738-4042 may reflect the existence of an asteroid belt{{efn|In the case of PSR B1937+21, the most massive object is thought to have a mass of less than 1/10,000 of Earth's.{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2455}}}} around the pulsars, and collisions between asteroids or comets and pulsars have been proposed as an explanation for the phenomenon of fast radio bursts,{{efn|A fast radio burst is a burst of radio waves, lasting for milliseconds and originating outside of the Milky Way.{{sfn|Petroff|Johnston|Keane|van Straten|2015|p=457}} One theory about their cause is that planets orbiting within a pulsar's magnetic field create a disturbance that produces the bursts, but there are no known examples of this process.{{sfn|Petroff|Johnston|Keane|van Straten|2015|p=458}}}} the gamma ray burst GRB 101225A{{sfn|Patruno|Kama|2017|p=1}} and other types of pulsar variability.{{sfn|Shearer|Cunniffe|Voisin|Neustroev|2008|p=3}} There are no known debris disks around pulsars, although the magnetars 4U 0142+61 and 1E 2259+586{{efn|The source states that the name is 1E 2259+286{{sfn|Martin|Livio|Palaniswamy|2016|p=8}} but the correct name is 1E 2259+586.{{sfn|Kaplan|Chakrabarty|Wang|Wachter|2009}}}} have been suggested to harbour them.{{sfn|Martin|Livio|Palaniswamy|2016|p=8}}

The white dwarf–pulsar binary PSR J0348+0432 may be a system that could develop pulsar planets in the future.{{sfn|Antoniadis|Freire|Wex|Tauris|2013|p=448}} The existence of a dust cloud at the pulsar Geminga that may be a precursor to planets has been proposed.{{sfn|Greaves|Holland|2017|p=26}}

There were earlier reports of pulsar planets which were either retracted or considered unconvincing,{{sfn|Wolszczan|1994|p=538}} such as the 1991 "discovery" of a planet around PSR B1829-10 which turned out to be an artifact caused by the motion of the Earth.{{sfn|Wolszczan|2015}} The existence of planets around the pulsar PSR B0329+54 has been debated since 1979 and is still unresolved {{as of|2017|lc=y}}.{{sfn|Starovoit|Rodin|2017|p=948}} PSR B1828-11 has been conclusively established to display magnetospheric activity that mimicks planets, without having any,{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2447}} and a planet candidate around the pulsar Geminga was later attributed to timing noise.{{sfn|Greaves|Holland|2017|p=26}}

{{OrbitboxPlanet begin|name=parameters of candidate/suspect pulsar planets{{efn|Should be divided by ~318 to convert from Earth mass to Jupiter mass}}|table_ref={{sfn|NASAEp|2023}}{{sfn|Starovoit|Rodin|2017|p=948}}}}

|-

|PSR B0329+54 b

|{{Earth mass|1.97}} ({{Jupiter mass|0.0062}})

|10.26

|10,140

|0.236

|~

|{{Earth radius|1.22}}{{sfn|NASAcatalog|2024|loc=PSR B0329+54 b}}

|-

|PSR B1828-11 a

|{{Earth mass|1.3}} ({{Jupiter mass|0.0041}})

|~

|231

|0.14{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B1828-11 b

|{{Earth mass|6.0}} ({{Jupiter mass|0.0189}})

|~

|498

|0.23{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J1555-2908 c

|{{Earth mass|0.04132}} ({{Jupiter mass|1.3 × 10⁻⁴}})

|~

|4,500

|0.27{{sfn|EPE|2024|loc=PSR J1555-2908 c}}

|~

|~

|-

|PSR B0525+21 b

|{{Earth mass|0.2988}} ({{Jupiter mass|9.4 × 10⁻⁴}})

|10.35

|10,132

|0.96{{sfn|EPE|2024|loc=PSR B0525+21 b}}

|~

|~

|-

|PSR B1937+21 b

|{{Earth mass|0.3178}} ({{Jupiter mass|0.001}})

|11

|11,400

|0.2{{sfn|EPE|2024|loc=PSR B1937+21 b}}

|~

|~

|-

|PSR J2007+3120 b

|{{Earth mass|2.3}} ({{Jupiter mass|0.0072}})

|~

|723

|<0.38{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J0337+1715 (AB) b

|{{Earth mass|9.5348}} ({{Jupiter mass|0.030}})

|~

|3,000{{sfn|EPE|2024|loc=PSR J0337+1715 (AB) b}}

|~

|~

|~

|-

|SGR 1806-20 b

|{{Earth mass|18.0844}} ({{Jupiter mass|0.0569}})

|0.85

|238

|0.992{{sfn|EPE|2024|loc=SGR 1806-20 b}}

|~

|~

|-

|PSR B1540-06 b

|{{Earth mass|1.1}} ({{Jupiter mass|0.0034}})

|~

|1,473

|0.12{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B1714-34 b

|{{Earth mass|6.3}} ({{Jupiter mass|0.0198}})

|~

|1,417

|0.14{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B1826-17 b

|{{Earth mass|2.6}} ({{Jupiter mass|0.0082}})

|~

|1,102

|0.35{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B0144+59 b

|{{Earth mass|0.06}} ({{Jupiter mass|1.9 × 10⁻⁴}})

|~

|319

|0.45{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B1727-33 b

|{{Earth mass|3.5}} ({{Jupiter mass|0.0110}})

|~

|350

|0.26{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B2053+36 b

|{{Earth mass|0.09}} ({{Jupiter mass|2.8 × 10⁻⁴}})

|~

|1,013

|0.4{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J1758-1931 b

|{{Earth mass|6.1}} ({{Jupiter mass|0.0192}})

|~

|719

|0.43{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J1843-0744 b

|{{Earth mass|1}} ({{Jupiter mass|0.0031}})

|~

|650

|0.4{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J1904+0800 b

|{{Earth mass|1}} ({{Jupiter mass|0.0031}})

|~

|946

|0.18{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J2216+5759 b

|{{Earth mass|3.5}} ({{Jupiter mass|0.011}})

|~

|117

|0.41{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR J1947+1957 b

|{{Earth mass|3.7}} ({{Jupiter mass|0.0116}})

|~

|1,070

|0.56{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B1931+24 b

|{{Earth mass|56}} ({{Jupiter mass|0.176}})

|~

|5,180

|0.25{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|PSR B0823+26 b

|{{Earth mass|0.08}} ({{Jupiter mass|2.5 × 10⁻⁴}})

|~

|28

|0.37{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|-

|SWIFT J1756.9-2508 b

|{{Jupiter mass|7.8}}

|0.0012346

|0.0379907{{sfn|EPE|2024|loc=SWIFT J1756.9-2508 b}}

|~

|~

|~

|-

|PSR J2007+3120 b

|{{Earth mass|2.3}}{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|723{{sfn|Niţu|Keith|Stappers|Lyne|2022|p=2451}}

|~

|~

|~

|-

|PSR B0943+10 b

|{{Jupiter mass|2.8}}

|1.8

|730{{sfn|EPE|2024|loc=PSR B0943+10 b}}

|~

|~

|~

|-

|PSR B0943+10 c

|{{Jupiter mass|2.6}}

|2.9

|1,460{{sfn|EPE|2024|loc=PSR B0943+10 c}}

|~

|~

|~

|-

{{Orbitbox end}}

{{Main articles|Habitability of neutron star systems}}

Pulsars emit a very different radiation spectrum than regular stars, with very little optical or infrared radiation but large amounts of ionizing radiation{{sfn|Patruno|Kama|2017|p=2}} and electron-positron pairs, which are generated by the pulsar's magnetic field as it spins. Additionally, remnant heat from before the pulsar's birth, heating of the pulsar's poles from its own radiation and from mass accretion processes drives the emission of thermal radiation and neutrinos.{{sfn|Patruno|Kama|2017|pp=4-5}} The electron-positron pairs and X-rays are absorbed by planetary atmospheres and heat them, driving intense atmospheric escape that can strip them away.{{sfn|Patruno|Kama|2017|pp=5-6}} The presence of a planetary magnetic field could mitigate the impact of the electron-positron pairs.{{sfn|Patruno|Kama|2017|p=11}}

Habitability is conventionally defined by the equilibrium temperature of a planet, which is a function of the amount of incoming radiation; a planet is defined "habitable" if liquid water can exist on its surface{{sfn|Patruno|Kama|2017|p=6}} although even planets with little external energy can harbour underground life.{{sfn|Stamenkovic|Breuer|2009|p=58}} Pulsars do not emit large quantities of radiation given their small size; the habitable zone can easily end up lying so close to the star that tidal effects destroy the planets.{{sfn|Patruno|Kama|2017|p=4}} Additionally, it is often unclear how much radiation a given pulsar emits and how much of it can actually reach a hypothetical planet's surface; of the known pulsar planets, only these of PSR B1257+12 are close to the habitable zone{{sfn|Patruno|Kama|2017|p=7}} and {{As of|2015|lc=y}}, no known pulsar planet is likely to be habitable.{{sfn|Wolszczan|2015}}{{sfn|Veras|Vidotto|2021|p=1702}} Additional heat sources may be radioactive isotopes such as potassium-40 formed during the supernova that gave rise to the pulsar{{sfn|Patruno|Kama|2017|p=10}} and tidal heating for planets with close orbits.{{sfn|Iorio|2021|p=5}} Radiation from outside sources such as companion stars would also add to the energy budget.{{sfn|Iorio|2021|p=1}}

• Lists of planets
• List of stars with proplyds
• Andrew Lyne

{{notelist|notes=

{{efn|1=Radius calculated with median mass and minimum density in the equation d=(1.89813*10^(30)*m)/((4/3)*{{pi}}*r{{sup|3}}), where d is density (in g/cm{{sup|3}}), m is the mass (in {{jupiter mass}}) and r is the radius (in centimeters). Should be divided by {{val|7.1492|e=9}} to convert from centimeters to {{jupiter radius}}|name=Radius1}}

}}

{{Reflist}}

{{refbegin}}

• {{cite journal |last1=Antoniadis |first1=John |last2=Freire |first2=Paulo C. C. |last3=Wex |first3=Norbert |last4=Tauris |first4=Thomas M. |last5=Lynch |first5=Ryan S. |last6=van Kerkwijk |first6=Marten H. |last7=Kramer |first7=Michael |last8=Bassa |first8=Cees |last9=Dhillon |first9=Vik S. |last10=Driebe |first10=Thomas |last11=Hessels |first11=Jason W. T. |last12=Kaspi |first12=Victoria M. |last13=Kondratiev |first13=Vladislav I. |last14=Langer |first14=Norbert |last15=Marsh |first15=Thomas R. |last16=McLaughlin |first16=Maura A. |last17=Pennucci |first17=Timothy T. |last18=Ransom |first18=Scott M. |last19=Stairs |first19=Ingrid H. |last20=van Leeuwen |first20=Joeri |last21=Verbiest |first21=Joris P. W. |last22=Whelan |first22=David G. |title=A Massive Pulsar in a Compact Relativistic Binary |journal=Science |date=26 April 2013 |volume=340 |issue=6131 |pages=1233232 |doi=10.1126/science.1233232 |pmid=23620056 |arxiv=1304.6875 |bibcode=2013Sci...340..448A |s2cid=15221098 |url=https://www.science.org/doi/epdf/10.1126/science.1233232 |language=en |issn=0036-8075}}
• {{cite journal |last1=Bailes |first1=M. |last2=Bates |first2=S. D. |last3=Bhalerao |first3=V. |last4=Bhat |first4=N. D. R. |last5=Burgay |first5=M. |last6=Burke-Spolaor |first6=S. |last7=D’Amico |first7=N. |last8=Johnston |first8=S. |last9=Keith |first9=M. J. |last10=Kramer |first10=M. |last11=Kulkarni |first11=S. R. |last12=Levin |first12=L. |last13=Lyne |first13=A. G. |last14=Milia |first14=S. |last15=Possenti |first15=A. |last16=Spitler |first16=L. |last17=Stappers |first17=B. |last18=van Straten |first18=W. |title=Transformation of a Star into a Planet in a Millisecond Pulsar Binary |journal=Science |date=23 September 2011 |volume=333 |issue=6050 |pages=1717–1720 |doi=10.1126/science.1208890 |pmid=21868629 |arxiv=1108.5201 |bibcode=2011Sci...333.1717B |s2cid=206535504 |url=https://www.science.org/doi/full/10.1126/science.1208890 |language=en |issn=0036-8075}}
• {{cite journal |last1=Callegari |first1=N. |last2=Ferraz-Mello |first2=S. |last3=Michtchenko |first3=T. A. |title=Dynamics of Two Planets in the 3/2 Mean-motion Resonance: Application to the Planetary System of the Pulsar PSR B1257+12 |journal=Celestial Mechanics and Dynamical Astronomy |date=1 April 2006 |volume=94 |issue=4 |pages=381–397 |doi=10.1007/s10569-006-9002-4 |bibcode=2006CeMDA..94..381C |s2cid=123024733 |url=https://link.springer.com/article/10.1007/s10569-006-9002-4 |language=en |issn=1572-9478}}
• {{cite journal |last1=Cassan |first1=A. |last2=Kubas |first2=D. |last3=Beaulieu |first3=J.-P. |last4=Dominik |first4=M. |last5=Horne |first5=K. |last6=Greenhill |first6=J. |last7=Wambsganss |first7=J. |last8=Menzies |first8=J. |last9=Williams |first9=A. |last10=Jørgensen |first10=U. G. |last11=Udalski |first11=A. |last12=Bennett |first12=D. P. |last13=Albrow |first13=M. D. |last14=Batista |first14=V. |last15=Brillant |first15=S. |last16=Caldwell |first16=J. a. R. |last17=Cole |first17=A. |last18=Coutures |first18=Ch |last19=Cook |first19=K. H. |last20=Dieters |first20=S. |last21=Prester |first21=D. Dominis |last22=Donatowicz |first22=J. |last23=Fouqué |first23=P. |last24=Hill |first24=K. |last25=Kains |first25=N. |last26=Kane |first26=S. |last27=Marquette |first27=J.-B. |last28=Martin |first28=R. |last29=Pollard |first29=K. R. |last30=Sahu |first30=K. C. |last31=Vinter |first31=C. |last32=Warren |first32=D. |last33=Watson |first33=B. |last34=Zub |first34=M. |last35=Sumi |first35=T. |last36=Szymański |first36=M. K. |last37=Kubiak |first37=M. |last38=Poleski |first38=R. |last39=Soszynski |first39=I. |last40=Ulaczyk |first40=K. |last41=Pietrzyński |first41=G. |last42=Wyrzykowski |first42=Ł |title=One or more bound planets per Milky Way star from microlensing observations |journal=Nature |date=January 2012 |volume=481 |issue=7380 |pages=167–169 |doi=10.1038/nature10684 |pmid=22237108 |arxiv=1202.0903 |bibcode=2012Natur.481..167C |s2cid=2614136 |url=https://www.nature.com/articles/nature10684 |language=en |issn=1476-4687}}
• {{cite journal |last1=Miller |first1=M. Coleman |last2=Hamilton |first2=Douglas P. |title=Implications of the PSR 1257+12 Planetary System for Isolated Millisecond Pulsars |journal=The Astrophysical Journal |date=April 2001 |volume=550 |issue=2 |pages=863 |doi=10.1086/319813 |arxiv=astro-ph/0012042 |bibcode=2001ApJ...550..863M |s2cid=10770838 |url=https://iopscience.iop.org/article/10.1086/319813/meta |language=en |issn=0004-637X}}
• {{cite news|last=Cowen|first=Ron|title=New evidence for planets orbiting a pulsar|journal=Science News |agency=Science News|volume=145|issue=10|date=5 March 1994|pages=151–152 |via=Gale Academic OneFile|url=https://link.gale.com/apps/doc/A14908916/AONE?u=wikipedia&sid=bookmark-AONE&xid=4140c2b9|access-date=23 March 2023}}
• {{cite journal |last1=Donnison |first1=J. R. |title=The Hill stability of the possible moons of extrasolar planets: Stability of extrasolar moons |journal=Monthly Notices of the Royal Astronomical Society |date=May 2010 |volume=406 |issue=3 |pages=1918–1934 |doi=10.1111/j.1365-2966.2010.16796.x |doi-access=free |s2cid=117784599 }}
• {{cite encyclopedia|url=https://exoplanet.eu/catalog/|title=Catalog|access-date=25 March 2023|encyclopedia=Extrasolar Planets Encyclopaedia|date=1995 |ref={{harvid|EPE|2023}}}}
• {{cite encyclopedia|url=https://exoplanet.eu/catalog/|title=Catalog|access-date=9 October 2024|encyclopedia=Extrasolar Planets Encyclopaedia|date=1995 |ref={{harvid|EPE|2024}}}}
• {{cite journal |last=Euvel |first=E. P. J. Van Den H. |title=Pulsar planets |journal=Nature |date=April 1992 |volume=356 |issue=6371 |pages=668 |doi=10.1038/356668b0 |bibcode=1992Natur.356..668V |s2cid=186241974 |language=en |issn=1476-4687|doi-access=free }}
• {{cite journal |last1=Flam |first1=Faye |title=Have Astronomers Bagged A Pair of Pulsar Planets?: New observations strengthen the case for planets circling burned-out stars—and spur the search for an explanation |journal=Science |date=17 January 1992 |volume=255 |issue=5042 |pages=290 |doi=10.1126/science.255.5042.290|pmid=17779576 }}
• {{cite journal |last1=Greaves |first1=J. S. |last2=Holland |first2=W. S. |title=The Geminga pulsar wind nebula in the mid-infrared and submillimetre |journal=Monthly Notices of the Royal Astronomical Society: Letters |date=October 2017 |volume=471 |issue=1 |pages=L26–L30 |doi=10.1093/mnrasl/slx098 |doi-access=free |url=https://academic.oup.com/mnrasl/article/471/1/L26/3868795}}
• {{cite journal |last1=Hansen |first1=Brad M. S. |last2=Shih |first2=Hsin-Yi |last3=Currie |first3=Thayne |title=The Pulsar Planets: A Test Case of Terrestrial Planet Assembly |journal=The Astrophysical Journal |date=January 2009 |volume=691 |issue=1 |pages=382–393 |doi=10.1088/0004-637X/691/1/382 |arxiv=0908.0736 |bibcode=2009ApJ...691..382H |s2cid=18322234 |url=https://iopscience.iop.org/article/10.1088/0004-637X/691/1/382/meta |language=en |issn=0004-637X}}
• {{cite journal |last1=Hirai |first1=Ryosuke |last2=Podsiadlowski |first2=Philipp |title=neutron stars colliding with binary companions: formation of hypervelocity stars, pulsar planets, bumpy superluminous supernovae and Thorne–Żytkow objects |journal=Monthly Notices of the Royal Astronomical Society |date=2 November 2022 |volume=517 |issue=3 |pages=4544–4556 |doi=10.1093/mnras/stac3007 |doi-access=free |url=https://academic.oup.com/mnras/article/517/3/4544/6764732|arxiv=2208.00915 }}
• {{cite web |title=Naming Exoplanets |url=https://www.iau.org/public/themes/naming_exoplanets/ |publisher=International Astronomical Union |access-date=12 September 2023|ref={{harvid|IAU}}}}
• {{cite journal |last1=Iorio |first1=Lorenzo |title=The Impact of Classical and General Relativistic Obliquity Precessions on the Habitability of Circumstellar neutron stars' Planets |journal=The Astronomical Journal |date=July 2021 |volume=162 |issue=2 |pages=51 |doi=10.3847/1538-3881/ac09f8 |arxiv=2106.06024 |bibcode=2021AJ....162...51I |s2cid=235417162 |language=en |issn=1538-3881 |doi-access=free }}
• {{cite journal |last1=Kaplan |first1=David L. |last2=Chakrabarty |first2=Deepto |last3=Wang |first3=Zhongxiang |last4=Wachter |first4=Stefanie |title=A Mid-Infrared Counterpart to the Magnetar 1E 2259+586 |journal=The Astrophysical Journal |date=June 2009 |volume=700 |issue=1 |pages=149–154 |doi=10.1088/0004-637X/700/1/149 |arxiv=0906.1604 |bibcode=2009ApJ...700..149K |s2cid=9937378 |url=https://iopscience.iop.org/article/10.1088/0004-637X/700/1/149 |language=en |issn=0004-637X}}
• {{cite journal |last1=Kerr |first1=M. |last2=Johnston |first2=S. |last3=Hobbs |first3=G. |last4=Shannon |first4=R. M. |title=Limits on Planet Formation Around Young Pulsars and Implications for Supernova Fallback Disks |journal=The Astrophysical Journal Letters |date=August 2015 |volume=809 |issue=1 |pages=L11 |doi=10.1088/2041-8205/809/1/L11 |arxiv=1507.06982 |bibcode=2015ApJ...809L..11K |s2cid=118144284 |url=https://iopscience.iop.org/article/10.1088/2041-8205/809/1/L11/meta |language=en |issn=2041-8205}}
• {{cite journal |last1=Kiefer |first1=Flavien |title=Determining the mass of the planetary candidate HD 114762 b using Gaia |journal=Astronomy & Astrophysics |date=1 December 2019 |volume=632 |pages=L9 |doi=10.1051/0004-6361/201936942 |arxiv=1910.07835 |bibcode=2019A&A...632L...9K |s2cid=204743831 |url=https://www.aanda.org/articles/aa/full_html/2019/12/aa36942-19/aa36942-19.html |language=en |issn=0004-6361}}
• {{cite journal |last1=Kuerban |first1=Abudushataer |last2=Geng |first2=Jin-Jun |last3=Huang |first3=Yong-Feng |title=GW emission from merging strange quark star-strange quark planet systems |journal=AIP Conference Proceedings |date=17 July 2019 |volume=2127 |issue=1 |pages=020027 |doi=10.1063/1.5117817 |bibcode=2019AIPC.2127b0027K |s2cid=199118120 |issn=0094-243X|doi-access=free }}
• {{cite journal |last1=Kurban |first1=Abdusattar |last2=Zhou |first2=Xia |last3=Wang |first3=Na |last4=Huang |first4=Yong-Feng |last5=Wang |first5=Yu-Bin |last6=Nurmamat |first6=Nurimangul |title=Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet |journal=Astronomy & Astrophysics |date=1 June 2024 |volume=686 |pages=A87 |doi=10.1051/0004-6361/202347828 |arxiv=2403.13333 |bibcode=2024A&A...686A..87K }}
• {{cite journal |last1=Lewis |first1=Karen M. |last2=Sackett |first2=Penny D. |last3=Mardling |first3=Rosemary A. |title=Possibility of Detecting Moons of Pulsar Planets through Time-of-Arrival Analysis |journal=The Astrophysical Journal |date=September 2008 |volume=685 |issue=2 |pages=L153 |doi=10.1086/592743 |arxiv=0805.4263 |bibcode=2008ApJ...685L.153L |s2cid=17818202 |url=https://iopscience.iop.org/article/10.1086/592743/meta |language=en |issn=0004-637X}}
• {{cite journal|url=https://ui.adsabs.harvard.edu/abs/2005S%26T...109Q..26M/abstract|last=MacRobert|first=A. M.|year=2005|title=Follow That Story: The Pulsar Planet in M4|journal=Sky and Telescope|volume=109|issue=1|page=26|bibcode=2005S&T...109Q..26M }}
• {{cite journal |last1=Margalit |first1=Ben |last2=Metzger |first2=Brian D. |title=Merger of a white dwarf–neutron star binary to 10 29 carat diamonds: origin of the pulsar planets |journal=Monthly Notices of the Royal Astronomical Society |date=1 March 2017 |volume=465 |issue=3 |pages=2790–2803 |doi=10.1093/mnras/stw2640 |doi-access=free |url=https://academic.oup.com/mnras/article/465/3/2790/2417383|arxiv=1608.08636 }}
• {{cite journal |last1=Martin |first1=Rebecca G. |last2=Livio |first2=Mario |last3=Palaniswamy |first3=Divya |title=Why Are Pulsar Planets Rare? |journal=The Astrophysical Journal |date=November 2016 |volume=832 |issue=2 |pages=122 |doi=10.3847/0004-637X/832/2/122 |arxiv=1609.06409 |bibcode=2016ApJ...832..122M |s2cid=118490527 |language=en |issn=0004-637X |doi-access=free }}
• {{cite journal |last1=Mottez |first1=F. |last2=Heyvaerts |first2=J. |title=Magnetic coupling of planets and small bodies with a pulsar wind |journal=Astronomy & Astrophysics |date=1 August 2011 |volume=532 |pages=A21 |doi=10.1051/0004-6361/201116530 |arxiv=1106.0657 |bibcode=2011A&A...532A..21M |s2cid=26955561 |url=https://www.aanda.org/articles/aa/abs/2011/08/aa16530-11/aa16530-11.html |language=en |issn=0004-6361}}
• {{cite web|access-date=9 October 2024|url=https://science.nasa.gov/exoplanets/|title=Exoplanets - NASA Science|date=7 June 2023 |ref={{harvid|NASAcatalog|2024}}}}
• {{cite journal |last1=Niţu |first1=Iuliana C |last2=Keith |first2=Michael J |last3=Stappers |first3=Ben W |last4=Lyne |first4=Andrew G |last5=Mickaliger |first5=Mitchell B |title=A search for planetary companions around 800 pulsars from the Jodrell Bank pulsar timing programme |journal=Monthly Notices of the Royal Astronomical Society |date=29 March 2022 |volume=512 |issue=2 |pages=2446–2459 |doi=10.1093/mnras/stac593 |doi-access=free |url=https://academic.oup.com/mnras/article/512/2/2446/6542453|arxiv=2203.01136 }}
• {{cite journal |last1=Pasqua |first1=Antonio |last2=Assaf |first2=Khudhair A. |title=Possibility of Detection of Exomoons with Inclined Orbits Orbiting Pulsar Planets Using the Time-of-Arrival Analysis |journal=Advances in Astronomy |date=25 February 2014 |volume=2014 |pages=e450864 |doi=10.1155/2014/450864 |bibcode=2014AdAst2014E...6P |language=en |issn=1687-7969|doi-access=free }}
• {{cite journal |last1=Petroff |first1=E. |last2=Johnston |first2=S. |last3=Keane |first3=E. F. |last4=van Straten |first4=W. |last5=Bailes |first5=M. |last6=Barr |first6=E. D. |last7=Barsdell |first7=B. R. |last8=Burke-Spolaor |first8=S. |last9=Caleb |first9=M.|author9-link=Manisha Caleb |last10=Champion |first10=D. J. |last11=Flynn |first11=C. |last12=Jameson |first12=A. |last13=Kramer |first13=M. |last14=Ng |first14=C. |last15=Possenti |first15=A. |last16=Stappers |first16=B. W. |title=A survey of FRB fields: limits on repeatability |journal=Monthly Notices of the Royal Astronomical Society |date=21 November 2015 |volume=454 |issue=1 |pages=457–462 |doi=10.1093/mnras/stv1953 |doi-access=free |url=https://academic.oup.com/mnras/article/454/1/457/1130397|arxiv=1508.04884 }}
• {{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PS|title=Table|website=NASA Exoplanet Archive|access-date=25 March 2023|ref={{harvid|NASAEp|2023}}}}
• {{cite conference |last1=Nekola Novakova |first1=J. |last2=Petrasek |first2=T. |title=Feasibility and benefits of pulsar planet characterization |date=1 September 2017 |pages=EPSC2017–623 |bibcode=2017EPSC...11..623N |url=https://ui.adsabs.harvard.edu/abs/2017EPSC...11..623N/abstract|conference=European Planetary Science Congress 2017}}
• {{cite journal |last1=Oliveira |first1=R. A. P. |last2=Ortolani |first2=S. |last3=Barbuy |first3=B. |last4=Kerber |first4=L. O. |last5=Maia |first5=F. F. S. |last6=Bica |first6=E. |last7=Cassisi |first7=S. |last8=Souza |first8=S. O. |last9=Pérez-Villegas |first9=A. |title=Precise distances from OGLE-IV member RR Lyrae stars in six bulge globular clusters |journal=Astronomy & Astrophysics |date=January 2022 |volume=657 |pages=A123 |doi=10.1051/0004-6361/202141596|arxiv=2110.13943 |bibcode=2022A&A...657A.123O }}
• {{cite journal |last1=Patruno |first1=A. |last2=Kama |first2=M. |title=neutron star planets: Atmospheric processes and irradiation |journal=Astronomy & Astrophysics |date=1 December 2017 |volume=608 |pages=A147 |doi=10.1051/0004-6361/201731102 |arxiv=1705.07688 |bibcode=2017A&A...608A.147P |s2cid=119191976 |url=https://www.aanda.org/articles/aa/full_html/2017/12/aa31102-17/aa31102-17.html |language=en |issn=0004-6361}}
• {{cite conference|conference=ASP Conference Series|last1=Phinney|first1=E. S.|last2=Hansen|first2=B. M. S.|date=January 1993|title=The pulsar planet production process|series=Planets around pulsars|volume=36|pages=371–390|url=https://adsabs.harvard.edu/full/record/seri/ASPC./0036/1993ASPC...36..371P.html}}
• {{cite journal |last1=Podsiadlowski |first1=Ph |last2=Pringle |first2=J. E. |last3=Rees |first3=M. J. |title=The origin of the planet orbiting PSR1829 – 10 |journal=Nature |date=August 1991 |volume=352 |issue=6338 |pages=783–784 |doi=10.1038/352783a0 |bibcode=1991Natur.352..783P |s2cid=4235775 |url=https://www.nature.com/articles/352783a0 |language=en |issn=1476-4687}}
• {{cite journal |last1=Setiawan |first1=Johny |last2=Klement |first2=Rainer J. |last3=Henning |first3=Thomas |last4=Rix |first4=Hans-Walter |last5=Rochau |first5=Boyke |last6=Rodmann |first6=Jens |last7=Schulze-Hartung |first7=Tim |title=A Giant Planet Around a Metal-Poor Star of Extragalactic Origin |journal=Science |date=17 December 2010 |volume=330 |issue=6011 |pages=1642–1644 |doi=10.1126/science.1193342 |pmid=21097905 |arxiv=1011.6376 |bibcode=2010Sci...330.1642S |s2cid=657925 |url=https://www.science.org/doi/pdf/10.1126/science.1193342 |language=en |issn=0036-8075}}
• {{cite journal |last1=Shearer |first1=Andy |last2=Cunniffe |first2=John |last3=Voisin |first3=Bruno |last4=Neustroev |first4=Vitaly |last5=Browne |first5=Michael |last6=Andersen |first6=Torben |last7=Enmark |first7=Anita |last8=Linde |first8=Peter |editor-first1=Torben E. |editor-last1=Andersen |title=High time resolution astrophysics and ELTs: Which wavelength? |journal=Extremely Large Telescopes: Which Wavelengths? Retirement Symposium for Arne Ardeberg |date=22 April 2008 |volume=6986 |pages=94–102 |doi=10.1117/12.801261 |url=https://www.spiedigitallibrary.org/conference-proceedings-of-spie/6986/69860A/High-time-resolution-astrophysics-and-ELTs-Which-wavelength/10.1117/12.801261.short |publisher=SPIE|bibcode=2008SPIE.6986E..0AS |s2cid=120761231 }}
• {{cite journal |last1=Smith |first1=R. F. |last2=Eggert |first2=J. H. |last3=Jeanloz |first3=R. |last4=Duffy |first4=T. S. |last5=Braun |first5=D. G. |last6=Patterson |first6=J. R. |last7=Rudd |first7=R. E. |last8=Biener |first8=J. |last9=Lazicki |first9=A. E. |last10=Hamza |first10=A. V. |last11=Wang |first11=J. |last12=Braun |first12=T. |last13=Benedict |first13=L. X. |last14=Celliers |first14=P. M. |last15=Collins |first15=G. W. |title=Ramp compression of diamond to five terapascals |journal=Nature |date=July 2014 |volume=511 |issue=7509 |pages=330–333 |doi=10.1038/nature13526 |pmid=25030170 |bibcode=2014Natur.511..330S |s2cid=4389771 |url=https://www.nature.com/articles/nature13526 |language=en |issn=1476-4687}}
• {{cite journal |last1=Spiewak |first1=R |last2=Bailes |first2=M |last3=Barr |first3=E D |last4=Bhat |first4=N D R |last5=Burgay |first5=M |last6=Cameron |first6=A D |last7=Champion |first7=D J |last8=Flynn |first8=C M L |last9=Jameson |first9=A |last10=Johnston |first10=S |last11=Keith |first11=M J |last12=Kramer |first12=M |last13=Kulkarni |first13=S R |last14=Levin |first14=L |last15=Lyne |first15=A G |last16=Morello |first16=V |last17=Ng |first17=C |last18=Possenti |first18=A |last19=Ravi |first19=V |last20=Stappers |first20=B W |last21=van Straten |first21=W |last22=Tiburzi |first22=C |title=PSR J2322−2650 – a low-luminosity millisecond pulsar with a planetary-mass companion |journal=Monthly Notices of the Royal Astronomical Society |date=21 March 2018 |volume=475 |issue=1 |pages=469–477 |doi=10.1093/mnras/stx3157 |doi-access=free |url=https://academic.oup.com/mnras/article/475/1/469/4710309|arxiv=1712.04445 }}
• {{cite journal |last1=Starovoit |first1=E. D. |last2=Rodin |first2=A. E. |title=On the existence of planets around the pulsar PSR B0329+54 |journal=Astronomy Reports |date=1 November 2017 |volume=61 |issue=11 |pages=948–953 |doi=10.1134/S1063772917110063 |arxiv=1710.01153 |bibcode=2017ARep...61..948S |s2cid=255206063 |url=https://link.springer.com/article/10.1134/S1063772917110063 |language=en |issn=1562-6881}}
• {{cite journal |last1=Stellato |first1=Judy |title=The Milky Way and Lentil Beans |journal=Science Scope |date=2020 |volume=43 |issue=6 |pages=44–49 |doi=10.1080/08872376.2020.12291320 |jstor=27048035 |url=https://www.jstor.org/stable/27048035 |issn=0887-2376}}
• {{cite journal |last1=Veras |first1=Dimitri |last2=Vidotto |first2=Aline A |title=Planetary magnetosphere evolution around post-main-sequence stars |journal=Monthly Notices of the Royal Astronomical Society |date=15 July 2021 |volume=506 |issue=2 |pages=1697–1703 |doi=10.1093/mnras/stab1772 |url=https://academic.oup.com/mnras/article/506/2/1697/6308830|doi-access=free |arxiv=2106.10293 }}
• {{cite journal |last1=Veras |first1=Dimitri |title=Post-main-sequence planetary system evolution |journal=Royal Society Open Science |date=February 2016 |volume=3 |issue=2 |pages=150571 |doi=10.1098/rsos.150571 |pmid=26998326 |pmc=4785977 |arxiv=1601.05419 |bibcode=2016RSOS....350571V |language=en |issn=2054-5703}}
• {{cite journal |first1=Vlada|last1=Stamenkovic|first2=Doris|last2=Breuer|title=Special Issue: Abstracts from the Eighth European Workshop on Astrobiology, Neuchâtel, Switzerland, 1-3 September, 2008 |journal=Origins of Life and Evolution of Biospheres |date=1 February 2009 |volume=39 |issue=1 |pages=1–89 |doi=10.1007/s11084-008-9155-0 |pmid=19184520 |s2cid=37433981 |url=https://link.springer.com/article/10.1007/s11084-008-9155-0 |language=en |issn=1573-0875}}
• {{cite journal |last1=Vleeschower |first1=L |last2=Corongiu |first2=A |last3=Stappers |first3=B W |last4=Freire |first4=P C C |last5=Ridolfi |first5=A |last6=Abbate |first6=F |last7=Ransom |first7=S M |last8=Possenti |first8=A |last9=Padmanabh |first9=P V |last10=Balakrishnan |first10=V |last11=Kramer |first11=M |last12=Venkatraman Krishnan |first12=V |last13=Zhang |first13=L |last14=Bailes |first14=M |last15=Barr |first15=E D |last16=Buchner |first16=S |last17=Chen |first17=W |title=Discoveries and timing of pulsars in M62 |journal=Monthly Notices of the Royal Astronomical Society |date=13 April 2024 |volume=530 |issue=2 |pages=1436–1456 |doi=10.1093/mnras/stae816|doi-access=free |arxiv=2403.12137 |bibcode=2024MNRAS.530.1436V }}
• {{cite journal |last1=Wolszczan |first1=Alexander |title=Confirmation of Earth-Mass Planets Orbiting the Millisecond Pulsar PSR B1257 + 12 |journal=Science |date=22 April 1994 |volume=264 |issue=5158 |pages=538–542 |doi=10.1126/science.264.5158.538|pmid=17732735 |bibcode=1994Sci...264..538W |s2cid=19621191 }}
• {{cite journal |last1=Wolszczan |first1=A |title=Fifteen years of the neutron star planet research |journal=Physica Scripta |date=August 2008 |volume=T130 |pages=014005 |doi=10.1088/0031-8949/2008/T130/014005 |bibcode=2008PhST..130a4005W |s2cid=122989232 |url=https://iopscience.iop.org/article/10.1088/0031-8949/2008/T130/014005/meta}}
• {{cite journal |last1=Wolszczan |first1=A. |last2=Frail |first2=D. A. |title=A planetary system around the millisecond pulsar PSR1257 + 12 |journal=Nature |date=January 1992 |volume=355 |issue=6356 |pages=145–147 |doi=10.1038/355145a0 |bibcode=1992Natur.355..145W |s2cid=4260368 |url=https://www.nature.com/articles/355145a0 |language=en |issn=1476-4687}}
• {{cite book |last1=Wolszczan |first1=Alexander |chapter=Pulsar Planets |title=Encyclopedia of Astrobiology |date=2015 |pages=2089–2092 |doi=10.1007/978-3-662-44185-5_1309 |chapter-url=https://link.springer.com/referenceworkentry/10.1007/978-3-662-44185-5_1309 |publisher=Springer |bibcode=2015enas.book.2089W |isbn=978-3-662-44184-8 |language=en}}
• {{cite journal |last1=Yan |first1=Zhen |last2=Shen |first2=Zhi-Qiang |last3=Yuan |first3=Jian-Ping |last4=Wang |first4=Na |last5=Rottmann |first5=Helge |last6=Alef |first6=Walter |title=Very long baseline interferometry astrometry of PSR B1257+12, a pulsar with a planetary system |journal=Monthly Notices of the Royal Astronomical Society |date=21 July 2013 |volume=433 |issue=1 |pages=162–169 |doi=10.1093/mnras/stt712|doi-access=free }}

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