Pulsar planets are planets that are orbiting pulsars. The first such planets to be discovered were around a millisecond pulsar in 1992 and were the first extrasolar planets to be confirmed as discovered. Pulsars are extremely precise clocks, and even small planets can create detectable variations in pulsar traits. As of 2025, the least massive exoplanet observed by humans is a pulsar planet.
They are extremely rare, with only half a dozen listed by the NASA Exoplanet Archive. Only special processes can give rise to planet-sized companions around pulsars, and many are thought to be exotic bodies, such as planets made of diamond, that were formed through the partial destruction of a companion star. Pulsars' intense radiation and winds — consisting of electron-positron pairs — would tend to strip atmospheres away from such planets, exposing the surface to the stellar elements, and making them extraordinarily unlikely abodes for life.
Formation
The formation of planets requires the existence of a protoplanetary disk, and 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. 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, which allows the magnetorotational instability to trigger turbulence and thus destroy the dead zone. Thus, a disk needs to have a large mass if it is to give rise to planets.
There are several processes that could give rise to planetary systems: "First-generation" planets are planets that orbited the star before it went supernova and became a pulsar: Massive stars tend to lack planets, or at least appear to — 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. "Second-generation" planets from material that falls back on the pulsar after a supernova: The material could theoretically reach a mass comparable to that of a protoplanetary disk, but is likely to dissipate too fast to allow the formation of planets. There are no known examples of planets around young pulsars. "Third-generation" planets: 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. In a third mechanism, the pulsar penetrates the envelope of a larger star, causing it to break up and form a disk around the pulsar. 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. 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. 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. A companion star may be destroyed during the interaction with a pulsar but leave a planet-sized remnant, such a system is known as a "black widow" but is not always considered a form of pulsar planet. Finally, it is possible that planets from companion stars or rogue planets are captured by a pulsar, or that a pulsar merged with the original host star of the planets. The latter process would form a "common envelope" which eventually breaks down to form a disk from which planets can develop.
Implications
The formation scenarios have consequences for the planets' composition: A planet formed from supernova debris is likely rich in metals and radioactive isotopes and may contain large quantities of water; one formed through the break-up of a white dwarf would be carbon rich and consist of large amounts of diamond; an actual white dwarf fragment would be extremely dense. , the most common type of planet around a pulsar is a "diamond planet", a very low-mass white dwarf. Other objects around pulsars could include asteroids, comets and planetoids. 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.
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 and could produce detectable radio emissions.
Observability
Pulsars are extremely precise clocks and pulsar timing is highly regular. It is thus possible to detect very small objects around pulsars, down to the size of large asteroids, 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; planets alter this pattern through their gravitational attraction on the pulsar, causing a Doppler shift in the pulses. The technique could in theory be also used to detect exomoons around pulsar planets. There are limitations to pulsar planet visibility, however; pulsar glitches and changes in the pulsation mode can mimick the existence of planets.
The first extrasolar planets to be discovered (in 1992 by Dale Frail and Aleksander Wolszczan) were the pulsar planets around PSR B1257+12. The discovery demonstrated that exoplanets can be detected from Earth, and led to the expectation that extrasolar planets might not be uncommon. the least massive known extrasolar planet (PSR B1257+12 A, only ) is a pulsar planet.
However, the size and particular spectroscopic traits makes actually visualizing such planets very difficult. 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.
Pulsar planets have been invoked to explain certain astronomical phenomena, such as X-ray bursts from soft gamma repeaters.
Occurrence
only about half-dozen pulsar planets are known, implying an occurrence rate of no more than one planetary system per 200 pulsars although differences in the definition of "planet" mean that different surveys report different counts. This rarity is supported by the results of large-scale searches for pulsar planets. 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. 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"). 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. 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.
Based on the known occurrence rate of pulsar planets, there might be as many as 10 million of them in the Milky Way. All known pulsar planets are found around millisecond pulsars, these are old pulsars that were spun up through the accretion of mass from a companion. there are no known planets around young pulsars; they are less regular than millisecond pulsars, increasing the pulsar timing error and thus making planet detection more difficult.
Confirmed pulsar planets
|M62H b
|~ |~
|PSR B1257+12 b | () |0.19 |25.262 |0 |~ |~ |- |PSR B1257+12 c | () |0.36 |66.5419 |0.0186 |~
|PSR B1257+12 d | () |0.46 |98.2114 |0.03 |~
|PSR B1620−26 b | |23 |34,675 |~ |~
|PSR J1719−1438 b | |0.0044 |0.090706293 |0.06 |~
|PSR J2322−2650 b | |0.0102 |0.322963997 |0.0017 |~
|PSR J1748−2021H b | |0.0111 |0.360787526 |~ |~ |~ |- |PSR J0636+5129 b | |0.0036 |0.0665513392 |~ |60
|PSR J1807−2459 A b | |~ |0.07 |~ |~ |~ |- |PSR B1802−07 b | |0.008098 |0.071092 |0.0000003 |~ |~ |- |PSR J1211−0633 b | |0.0116 |0.38634962 |~ |~ |~ |- |PSR J0312−0921 b | |0.00465 |0.0975 |~ |~ |~ |- |PSR J1824−2452G b | |0.004875 |0.1046 |0.0000003 |~ |~ |- |PSR J1928+1245 b | |0.005825 |0.1366347269 |~ |~ |~ |- |PSR J1824−2452M b | |0.00854 |0.242519219 |~ |~ |~ |- |PSR J1630+3550 b | |~ |0.315863166 |0.00042 |~ |~ |- |PSR J2241−5236 b | |~ |0.1456722395 |~ |~ |~ |- |PSR J1311−3430 b | |~ |0.065115 |~ |~ |~
M62H is a millisecond pulsar located in the constellation Ophiuchus. It is located in the globular cluster Messier 62, at a distance of from Earth. The pulsar was discovered in 2024 using the MeerKAT radio telescope. M62H has a rotational period of 3.70 milliseconds, meaning it completes 270 rotations per second (270 Hz). Its planetary companion has a minimum mass of and a median mass of , assuming a mass of for the pulsar. Its minimum density is of 11 g/cm. Assuming the median mass, it implies a maximum radius of . The planet takes just to complete an orbit, and is located at a distance equivalent to 0.49% of an astronomical unit from M62H.
PSR B1257+12 The pulsar PSR B1257+12, parsecs away in the constellation Virgo, was confirmed to have planets in 1992 based on observations made with the Arecibo Observatory. The system consists of one tiny planet with a mass of Earth masses and two Super-Earths with masses and times that of Earth, assuming that the pulsar has a mass of 1.4 solar masses. They most likely formed from a protoplanetary disk, probably generated from the partial destruction of a companion star. Computer simulations have shown that the system should be stable for at least one billion years and that exomoons could survive in the system. The system resembles the inner Solar System; the planets orbit the pulsar at distances comparable to that of Mercury to the Sun and may have comparable surface temperatures. Reports of additional bodies in this system might be due to solar disturbances.
PSR J1719−1438 A cthonian planet with a mass comparable to Jupiter but less than 40% of its radius orbits the pulsar PSR J1719-1438. This planet is probably the carbon-rich remnant of a companion star that was evaporated by the pulsar's radiation and has been described as a "diamond planet".
PSR B1620−26