Pulsar

This article is about a type of neutron star. For other uses, see Pulsar (disambiguation).

PSR B1509−58 – X-rays from Chandra are gold; Infrared from WISE in red, green and blue/max.

Animation of a rotating pulsar. The sphere in the middle represents the neutron star, the curves indicate the magnetic field lines and the protruding cones represent the emission zones.

Illustration of the "lighthouse" effect produced by a pulsar.

A pulsar (from puls(ating st)ar, on the model of quasar) ^[1] is a highly magnetized rotating neutron star that emits beams of electromagnetic radiation out of its magnetic poles. ^[2] This radiation can be observed only when a beam of emission is pointing toward Earth (similar to the way a lighthouse can be seen only when the light is pointed in the direction of an observer), 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. (See also centrifugal mechanism of acceleration.)

Pulsars’ highly regular pulses make them very useful tools for astronomers. For example, observations of a pulsar in a binary neutron star system were used to indirectly confirm the existence of gravitational radiation. The first extrasolar planets were discovered in 1992 around a pulsar, specifically PSR B1257+12. In 1983, certain types of pulsars were detected that, at that time, exceeded the accuracy of atomic clocks in keeping time. ^[3]

History of observation

Discovery

Signals from the first discovered pulsar were initially observed by Jocelyn Bell while analyzing data recorded on August 6, 1967, from a newly commissioned radio telescope that she helped build. Initially dismissed as radio interference by her supervisor and developer of the telescope, Antony Hewish, ^{[4] [5]} the fact that the signals always appeared at the same declination and right ascension soon ruled out a terrestrial source. ^[6] On November 28, 1967, Bell and Hewish using a fast strip chart recorder resolved the signals as a series of pulses, evenly spaced every 1.337 seconds. ^[7] No astronomical object of this nature had ever been observed before. On December 21, Bell discovered a second pulsar, quashing speculation that these might be signals beamed at earth from an extraterrestrial intelligence. ^{[8] [9] [10] [11]}

When observations with another telescope confirmed the emission, it eliminated any sort of instrumental effects. At this point, Bell said of herself and Hewish that "we did not really believe that we had picked up signals from another civilization, but obviously the idea had crossed our minds and we had no proof that it was an entirely natural radio emission. It is an interesting problem—if one thinks one may have detected life elsewhere in the universe, how does one announce the results responsibly?" ^[12] Even so, they nicknamed the signal LGM-1, for "little green men" (a playful name for intelligent beings of extraterrestrial origin).

Chart on which Jocelyn Bell first recognised evidence of a pulsar, exhibited at Cambridge University Library

It was not until a second pulsating source was discovered in a different part of the sky that the "LGM hypothesis" was entirely abandoned. ^[13] Their pulsar was later dubbed CP 1919, and is now known by a number of designators including PSR B1919+21 and PSR J1921+2153. Although CP 1919 emits in radio wavelengths, pulsars have subsequently been found to emit in visible light, X-ray, and gamma ray wavelengths. ^[14]

The word "pulsar" first appeared in print in 1968:

An entirely novel kind of star came to light on Aug. 6 last year and was referred to, by astronomers, as LGM (Little Green Men). Now it is thought to be a novel type between a white dwarf and a neutron [star]. The name Pulsar is likely to be given to it. Dr. A. Hewish told me yesterday: '... I am sure that today every radio telescope is looking at the Pulsars.' ^[15]

Composite optical/X-ray image of the Crab Nebula, showing synchrotron emission in the surrounding pulsar wind nebula, powered by injection of magnetic fields and particles from the central pulsar.

The existence of neutron stars was first proposed by Walter Baade and Fritz Zwicky in 1934, when they argued that a small, dense star consisting primarily of neutrons would result from a supernova. ^[16] Based on the idea of magnetic flux conservation from magnetic main sequence stars, Lodewijk Woltjer proposed in 1964 that such neutron stars might contain magnetic fields as large as 10¹⁴ to 10¹⁶  gauss (=10¹⁰ to 10¹²  tesla). ^[17] In 1967, shortly before the discovery of pulsars, Franco Pacini suggested that a rotating neutron star with a magnetic field would emit radiation, and even noted that such energy could be pumped into a supernova remnant around a neutron star, such as the Crab Nebula. ^[18] After the discovery of the first pulsar, Thomas Gold independently suggested a rotating neutron star model similar to that of Pacini, and explicitly argued that this model could explain the pulsed radiation observed by Bell Burnell and Hewish. ^[19] In 1968, Richard V. E. Lovelace with collaborators discovered period ${\displaystyle P\approx 33}$ ms of the Crab Nebula pulsar using Arecibo Observatory. ^{[20] [21]} The discovery of the Crab pulsar provided confirmation of the rotating neutron star model of pulsars. ^[22] The Crab pulsar 33-millisecond pulse period was too short to be consistent with other proposed models for pulsar emission. Moreover, the Crab pulsar is so named because it is located at the center of the Crab Nebula, consistent with the 1933 prediction of Baade and Zwicky. ^[23] In 1974, Antony Hewish and Martin Ryle, who had developed revolutionary radio telescopes, became the first astronomers to be awarded the Nobel Prize in Physics, with the Royal Swedish Academy of Sciences noting that Hewish played a "decisive role in the discovery of pulsars". ^[24] Considerable controversy is associated with the fact that Hewish was awarded the prize while Bell, who made the initial discovery while she was his PhD student, was not. Bell claims no bitterness upon this point, supporting the decision of the Nobel prize committee. ^[25]

Milestones

The Vela Pulsar and its surrounding pulsar wind nebula.

In 1974, Joseph Hooton Taylor, Jr. and Russell Hulse discovered for the first time a pulsar in a binary system, PSR B1913+16. This pulsar orbits another neutron star with an orbital period of just eight hours. Einstein's theory of general relativity predicts that this system should emit strong gravitational radiation, causing the orbit to continually contract as it loses orbital energy. Observations of the pulsar soon confirmed this prediction, providing the first ever evidence of the existence of gravitational waves. As of 2010, observations of this pulsar continue to agree with general relativity. ^[26] In 1993, the Nobel Prize in Physics was awarded to Taylor and Hulse for the discovery of this pulsar. ^[27]

In 1982, Don Backer led a group that discovered PSR B1937+21, a pulsar with a rotation period of just 1.6 milliseconds (38,500 rpm). ^[28] Observations soon revealed that its magnetic field was much weaker than ordinary pulsars, while further discoveries cemented the idea that a new class of object, the "millisecond pulsars" (MSPs) had been found. MSPs are believed to be the end product of X-ray binaries. Owing to their extraordinarily rapid and stable rotation, MSPs can be used by astronomers as clocks rivaling the stability of the best atomic clocks on Earth. Factors affecting the arrival time of pulses at Earth by more than a few hundred nanoseconds can be easily detected and used to make precise measurements. Physical parameters accessible through pulsar timing include the 3D position of the pulsar, its proper motion, the electron content of the interstellar medium along the propagation path, the orbital parameters of any binary companion, the pulsar rotation period and its evolution with time. (These are computed from the raw timing data by Tempo, a computer program specialized for this task.) After these factors have been taken into account, deviations between the observed arrival times and predictions made using these parameters can be found and attributed to one of three possibilities: intrinsic variations in the spin period of the pulsar, errors in the realization of Terrestrial Time against which arrival times were measured, or the presence of background gravitational waves. Scientists are currently attempting to resolve these possibilities by comparing the deviations seen between several different pulsars, forming what is known as a pulsar timing array. The goal of these efforts is to develop a pulsar-based time standard precise enough to make the first ever direct detection of gravitational waves. In 2006, a team of astronomers at LANL proposed a model to predict the likely date of pulsar glitches with observational data from the Rossi X-ray Timing Explorer. They used observations of the pulsar PSR J0537−6910, that is known to be a quasi-periodic glitching pulsar. ^[29] However, no general scheme for glitch forecast is known to date. ^[29]

Artist's impression of the planets orbiting PSR B1257+12. The one in the foreground is planet "C".

In 1992, Aleksander Wolszczan discovered the first extrasolar planets around PSR B1257+12. This discovery presented important evidence concerning the widespread existence of planets outside the Solar System, although it is very unlikely that any life form could survive in the environment of intense radiation near a pulsar.

Pulsar-like white dwarfs

White dwarfs can also act as pulsars. Because the moment of inertia of a white dwarf is much higher than that of a neutron star, the white-dwarf pulsars rotate once every several minutes, far slower than neutron-star pulsars.

By 2024, three pulsar-like white dwarfs have been identified.

• In 1998, Nazar Ikhsanov showed that a white dwarf in the binary system AE Aquarii acts like a radio pulsar. ^[30] The confirmation of the pulsar-like properties of the white dwarf in AE Aquarii was provided in 2008 by a discovery of X-ray pulsations, ^[31] which showed that this white dwarf acts not only as a radio pulsar, but also as an X-ray pulsar.

• In 2016, a white dwarf in the binary system AR Scorpii was identified as a pulsar ^{[32] [33]} (it is often mistakenly called the first discovered pulsar-like white dwarf). The system displays strong pulsations from ultraviolet to radio wavelengths, powered by the spin-down of the strongly magnetized white dwarf. ^[32]

• In 2023, it was suggested that the white dwarf eRASSU J191213.9−441044 acts as a pulsar both in radio and X-rays. ^{[34] [35]}

There is an alternative tentative explanation of the pulsar-like properties of these white dwarfs. In 2019, the properties of pulsars have been explained using a numerical magnetohydrodynamic model explaining was developed at Cornell University. ^[36] According to this model, AE Aqr is an intermediate polar-type star, where the magnetic field is relatively weak and an accretion disc may form around the white dwarf. The star is in the propeller regime, and many of its observational properties are determined by the disc-magnetosphere interaction. A similar model for eRASSU J191213.9−441044 is supported by the results of its observations at ultraviolet wave lengths, which showed that its magnetic field strength does not exceed 50 MG. ^[37]

Nomenclature

Initially pulsars were named with letters of the discovering observatory followed by their right ascension (e.g. CP 1919). As more pulsars were discovered, the letter code became unwieldy, and so the convention then arose of using the letters PSR (Pulsating Source of Radio) followed by the pulsar's right ascension and degrees of declination (e.g. PSR 0531+21) and sometimes declination to a tenth of a degree (e.g. PSR 1913+16.7). Pulsars appearing very close together sometimes have letters appended (e.g. PSR 0021−72C and PSR 0021−72D).

The modern convention prefixes the older numbers with a B (e.g. PSR B1919+21), with the B meaning the coordinates are for the 1950.0 epoch. All new pulsars have a J indicating 2000.0 coordinates and also have declination including minutes (e.g. PSR J1921+2153). Pulsars that were discovered before 1993 tend to retain their B names rather than use their J names (e.g. PSR J1921+2153 is more commonly known as PSR B1919+21). Recently discovered pulsars only have a J name (e.g. PSR J0437−4715). All pulsars have a J name that provides more precise coordinates of its location in the sky. ^[38]

Formation, mechanism, turn off

Schematic view of a pulsar. The sphere in the middle represents the neutron star, the curves indicate the magnetic field lines, the protruding cones represent the emission beams and the green line represents the axis on which the star rotates.

The events leading to the formation of a pulsar begin when the core of a massive star is compressed during a supernova, which collapses into a neutron star. The neutron star retains most of its angular momentum, and since it has only a tiny fraction of its progenitor's radius, it is formed with very high rotation speed. A beam of radiation is emitted along the magnetic axis of the pulsar, which spins along with the rotation of the neutron star. The magnetic axis of the pulsar determines the direction of the electromagnetic beam, with the magnetic axis not necessarily being the same as its rotational axis. This misalignment causes the beam to be seen once for every rotation of the neutron star, which leads to the "pulsed" nature of its appearance.

Animation of the increased spin of a pulsar as it collapses. It begins with (1) The rotating progenitor (2) The collapse and speedup and (3) The final fast spinning pulsar remnant. The animation demonstrates the conservation of momentum as the star spins faster as it collapses. The angular speed (${\displaystyle \Omega /\Omega _{\text{init}}}$) and radius (${\displaystyle R/R_{\text{init}}}$) relative to the progenitor are shown throughout the process. This does not capture the entire collapse scale as the final star would be too small to see compared to its progenitor.

In rotation-powered pulsars, the beam is the result of the rotational energy of the neutron star, which generates an electrical field and very strong magnetic field, resulting in the acceleration of protons and electrons on the star surface and the creation of an electromagnetic beam emanating from the poles of the magnetic field. ^{[39] [40]} Observations by NICER of PSR J0030+0451 indicate that both beams originate from hotspots located on the south pole and that there may be more than two such hotspots on that star. ^{[41] [42]} This rotation slows down over time as electromagnetic power is emitted. When a pulsar's spin period slows down sufficiently, the radio pulsar mechanism is believed to turn off (the so-called "death line"). This turn-off seems to take place after about 10–100 million years, which means of all the neutron stars born in the 13.6-billion-year age of the universe, around 99% no longer pulsate. ^[43]

Though the general picture of pulsars as rapidly rotating neutron stars is widely accepted, Werner Becker of the Max Planck Institute for Extraterrestrial Physics said in 2006, "The theory of how pulsars emit their radiation is still in its infancy, even after nearly forty years of work." ^[44]

Categories

Three distinct classes of pulsars are currently known to astronomers, according to the source of the power of the electromagnetic radiation:

• rotation-powered pulsars, where the loss of rotational energy of the star provides the power,
• accretion-powered pulsars (accounting for most but not all X-ray pulsars), where the gravitational potential energy of accreted matter is the power source (producing X-rays that are observable from the Earth),
• magnetars, where the decay of an extremely strong magnetic field provides the electromagnetic power.

Although all three classes of objects are neutron stars, their observable behavior and the underlying physics are quite different. There are, however, some connections. For example, X-ray pulsars are probably old rotationally-powered pulsars that have already lost most of their energy, and have only become visible again after their binary companions had expanded and begun transferring matter on to the neutron star.

The process of accretion can, in turn, transfer enough angular momentum to the neutron star to "recycle" it as a rotation-powered millisecond pulsar. As this matter lands on the neutron star, it is thought to "bury" the magnetic field of the neutron star (although the details are unclear), leaving millisecond pulsars with magnetic fields 1000–10,000 times weaker than average pulsars. This low magnetic field is less effective at slowing the pulsar's rotation, so millisecond pulsars live for billions of years, making them the oldest known pulsars. Millisecond pulsars are seen in globular clusters, which stopped forming neutron stars billions of years ago. ^[43]

Of interest to the study of the state of the matter in a neutron star are the glitches observed in the rotation velocity of the neutron star. ^[29] This velocity decreases slowly but steadily, except for an occasional sudden variation known as "glitch". One model put forward to explain these glitches is that they are the result of "starquakes" that adjust the crust of the neutron star. Models where the glitch is due to a decoupling of the possibly superconducting interior of the star have also been advanced. In both cases, the star's moment of inertia changes, but its angular momentum does not, resulting in a change in rotation rate. ^[29]

Neutron star types (24 June 2020)

Disrupted recycled pulsar

When two massive stars are born close together from the same cloud of gas, they can form a binary system and orbit each other from birth. If those two stars are at least a few times as massive as the Sun, their lives will both end in supernova explosions. The more massive star explodes first, leaving behind a neutron star. If the explosion does not kick the second star away, the binary system survives. The neutron star can now be visible as a radio pulsar, and it slowly loses energy and spins down. Later, the second star can swell up, allowing the neutron star to suck up its matter. The matter falling onto the neutron star spins it up and reduces its magnetic field.

This is called "recycling" because it returns the neutron star to a quickly-spinning state. Finally, the second star also explodes in a supernova, producing another neutron star. If this second explosion also fails to disrupt the binary, a double neutron star (neutron star binary) is formed. Otherwise, the spun-up neutron star is left with no companion and becomes a "disrupted recycled pulsar", spinning between a few and 50 times per second. ^[45]

Applications

The discovery of pulsars allowed astronomers to study an object never observed before, the neutron star. This kind of object is the only place where the behavior of matter at nuclear density can be observed (though not directly). Also, millisecond pulsars have allowed a test of general relativity in conditions of an intense gravitational field.

Maps

Relative position of the Sun to the center of the Galaxy and 14 pulsars with their periods denoted, shown on a Pioneer plaque

Pulsar maps have been included on the two Pioneer plaques as well as the Voyager Golden Record. They show the position of the Sun, relative to 14 pulsars, which are identified by the unique timing of their electromagnetic pulses, so that Earth's position both in space and time can be calculated by potential extraterrestrial intelligence. ^[46] Because pulsars are emitting very regular pulses of radio waves, its radio transmissions do not require daily corrections. Moreover, pulsar positioning could create a spacecraft navigation system independently, or be used in conjunction with satellite navigation. ^{[47] [48]}

Pulsar navigation

Main article: X-ray pulsar-based navigation

X-ray pulsar-based navigation and timing (XNAV) or simply pulsar navigation is a navigation technique whereby the periodic X-ray signals emitted from pulsars are used to determine the location of a vehicle, such as a spacecraft in deep space. A vehicle using XNAV would compare received X-ray signals with a database of known pulsar frequencies and locations. Similar to GPS, this comparison would allow the vehicle to calculate its position accurately (±5 km). The advantage of using X-ray signals over radio waves is that X-ray telescopes can be made smaller and lighter. ^{[49] [50] [51]} Experimental demonstrations have been reported in 2018. ^[52]

Precise clocks

Generally, the regularity of pulsar emission does not rival the stability of atomic clocks. ^[53] They can still be used as external reference. ^[54] For example, J0437−4715 has a period of 0.005757451936712637 s with an error of 1.7×10⁻¹⁷ s. This stability allows millisecond pulsars to be used in establishing ephemeris time ^[55] or in building pulsar clocks. ^[56]

Timing noise is the name for rotational irregularities observed in all pulsars. This timing noise is observable as random wandering in the pulse frequency or phase. ^[57] It is unknown whether timing noise is related to pulsar glitches. According to a study published in 2023, ^[58] the timing noise observed in pulsars is believed to be caused by background gravitational waves. Alternatively, it may be caused by stochastic fluctuations in both the internal (related to the presence of superfluids or turbulence) and external (due to magnetospheric activity) torques in a pulsar. ^[59]

Probes of the interstellar medium

The radiation from pulsars passes through the interstellar medium (ISM) before reaching Earth. Free electrons in the warm (8000 K), ionized component of the ISM and H II regions affect the radiation in two primary ways. The resulting changes to the pulsar's radiation provide an important probe of the ISM itself. ^[60]

Because of the dispersive nature of the interstellar plasma, lower-frequency radio waves travel through the medium slower than higher-frequency radio waves. The resulting delay in the arrival of pulses at a range of frequencies is directly measurable as the dispersion measure of the pulsar. The dispersion measure is the total column density of free electrons between the observer and the pulsar:

${\displaystyle \mathrm {DM} =\int _{0}^{D}n_{e}(s)\,ds,}$

where ${\displaystyle D}$ is the distance from the pulsar to the observer, and ${\displaystyle n_{e}}$ is the electron density of the ISM. The dispersion measure is used to construct models of the free electron distribution in the Milky Way. ^[61]

Additionally, density inhomogeneities in the ISM cause scattering of the radio waves from the pulsar. The resulting scintillation of the radio waves—the same effect as the twinkling of a star in visible light due to density variations in the Earth's atmosphere—can be used to reconstruct information about the small scale variations in the ISM. ^[62] Due to the high velocity (up to several hundred km/s) of many pulsars, a single pulsar scans the ISM rapidly, which results in changing scintillation patterns over timescales of a few minutes. ^[63] The exact cause of these density inhomogeneities remains an open question, with possible explanations ranging from turbulence to current sheets. ^[64]

Probes of space-time

Pulsars orbiting within the curved space-time around Sgr A*, the supermassive black hole at the center of the Milky Way, could serve as probes of gravity in the strong-field regime. ^[65] Arrival times of the pulses would be affected by special- and general-relativistic Doppler shifts and by the complicated paths that the radio waves would travel through the strongly curved space-time around the black hole. In order for the effects of general relativity to be measurable with current instruments, pulsars with orbital periods less than about 10 years would need to be discovered; ^[65] such pulsars would orbit at distances inside 0.01 pc from Sgr A*. Searches are currently underway; at present, five pulsars are known to lie within 100 pc from Sgr A*. ^[66]

Gravitational wave detectors

There are four consortia around the world which use pulsars to search for gravitational waves: the European Pulsar Timing Array (EPTA) in Europe, the Parkes Pulsar Timing Array (PPTA) in Australia, the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) in Canada and the US, and the Indian Pulsar Timing Array (InPTA) in India. Together, the consortia form the International Pulsar Timing Array (IPTA). The pulses from Millisecond Pulsars (MSPs) are used as a system of galactic clocks. Disturbances in the clocks will be measurable at Earth. A disturbance from a passing gravitational wave will have a particular signature across the ensemble of pulsars, and will be thus detected.

Significant pulsars

See also: Neutron star § Examples of neutron stars

Pulsars within 300 pc ^[67]

PSR	Distance (pc)	Age (Myr)
J0030+0451	244	7,580
J0108−1431	238	166
J0437−4715	156	1,590
J0633+1746	156	0.342
J0659+1414	290	0.111
J0835−4510	290	0.0113
J0453+0755	260	17.5
J1045−4509	300	6,710
J1741−2054	250	0.387
J1856−3754	161	3.76
J2144−3933	165	272

Gamma-ray pulsars detected by the Fermi Gamma-ray Space Telescope.

The pulsars listed here were either the first discovered of its type, or represent an extreme of some type among the known pulsar population, such as having the shortest measured period.

• The first radio pulsar "CP 1919" (now known as PSR B1919+21), with a pulse period of 1.337 seconds and a pulse width of 0.04-second, was discovered in 1967. ^[6]
• The first binary pulsar, PSR 1913+16, whose orbit is decaying due to the emission of gravitational radiation at the exact rate predicted by general relativity.
• The brightest radio pulsar, the Vela Pulsar.
• The first millisecond pulsar, PSR B1937+21
• The brightest millisecond pulsar, PSR J0437−4715
• The first X-ray pulsar, Cen X-3
• The first accreting millisecond X-ray pulsar, SAX J1808.4−3658
• The first pulsar with planets, PSR B1257+12
• The first pulsar observed to have been affected by asteroids: PSR J0738−4042
• The first double pulsar binary system, PSR J0737−3039
• The shortest period pulsar, PSR J1748−2446ad, with a period of ~0.0014 seconds or ~1.4 milliseconds (716 times a second).
• The longest period neutron star pulsar, PSR J0901-4046, with a period of 75.9 seconds.
• The longest period pulsar, at 118.2 seconds, as well as one of the only known two white dwarf pulsars, AR Scorpii. ^[68]
• The first white dwarf pulsar AE Aquarii. ^{[69] [70]}
• The pulsar with the most stable period, PSR J0437−4715
• The first millisecond pulsar with 2 stellar mass companions, PSR J0337+1715
• PSR J1841−0500, stopped pulsing for 580 days. One of only two pulsars known to have stopped pulsing for more than a few minutes.
• PSR B1931+24, has a cycle. It pulses for about a week and stops pulsing for about a month. ^[71] One of only two pulsars known to have stopped pulsing for more than a few minutes.
• Swift J0243.6+6124 most magnetic pulsar with 1.6×10¹³  G . ^{[72] [73]}
• PSR J0952-0607 heaviest pulsar with 2.35+0.17
  −0.17M_☉. ^{[74] [75]}
• PSR J1903+0327, a ~2.15 ms pulsar discovered to be in a highly eccentric binary star system with a Sun-like star. ^[76]
• PSR J2007+2722, a 40.8-hertz 'recycled' isolated pulsar was the first pulsar found by volunteers on data taken in February 2007 and analyzed by distributed computing project Einstein@Home. ^[77]
• PSR J1311–3430, the first millisecond pulsar discovered via gamma-ray pulsations and part of a binary system with the shortest orbital period. ^[78]

Gallery

• 
  Video – Crab Pulsar – bright pulse and interpulse.
• Video – Vela pulsar – X-ray light.
• Video – Artist's impression of AR Scorpii.

See also

• Anomalous X-ray pulsar
• Black hole
• Double pulsar
• Magnetar
• Neutron star
• Optical pulsar
• Pulsar clock
• Pulsar planet
• Pulsar timing array
• Pulsar wind nebula
• Quasar
• Radio astronomy
• Radio star
• Rotating radio transient
• Soft gamma repeater
• Supernova remnant
• X-ray pulsar

References

1. https://www.collinsdictionary.com/de/worterbuch/englisch/pulsar
2. "NASA's NICER Delivers Best-ever Pulsar Measurements, 1st Surface Map". 11 December 2019.
3. Sullivan, Walter (9 February 1983). "Pulsar Termed Most Accurate 'Clock' in Sky". The New York Times . Retrieved 2024-08-30.
4. Proudfoot, Ben (July 27, 2021). "She Changed Astronomy Forever. He Won the Nobel Prize For It - In 1967, Jocelyn Bell Burnell made an astounding discovery. But as a young woman in science, her role was overlooked". The New York Times . Retrieved July 27, 2021.
5. "I Changed Astronomy Forever. He Won the Nobel Prize for It. | 'Almost Famous' by Op-Docs". YouTube . 29 July 2021.
6. Hewish, A., Bell, S. J., et al. "Observation of a Rapidly Pulsating Radio Source Archived 2021-08-04 at the Wayback Machine ". Nature, Volume 217, 1968 (pp. 709–713).
7. Hewish, A.; Bell, S. J.; Pilkington, J. D. H.; Scott, P. F.; Collins, R. A. (February 1968). "Observation of a Rapidly Pulsating Radio Source". Nature. 217 (5130): 709–713. Bibcode:1968Natur.217..709H. doi:10.1038/217709a0. ISSN   1476-4687. S2CID   4277613.
8. Hobbs, George; Johnston, Simon; Conversation, The (November 28, 2017). "Fifty years ago, Jocelyn Bell discovered pulsars and changed our view of the universe". phys.org. Retrieved August 4, 2021.
9. Ghosh, Pranab (April 2007). Rotation and Accretion Powered Pulsars. World Scientific Series in Astronomy and Astrophysics. Vol. 10. World Scientific. p. 2. Bibcode:2007rapp.book.....G. doi:10.1142/4806. ISBN   978-981-02-4744-7.
10. Longair, Malcolm S. (1996). Our evolving universe. Cambridge [England] ; New York : Cambridge University Press. p. 72. ISBN   978-0-521-55091-8.
11. Longair, Malcolm S. (1992). High energy astrophysics (2nd ed.). Cambridge New York Port Chester [etc.]: Cambridge university press. p. 99. ISBN   978-0-521-38374-5.
12. S. Jocelyn Bell Burnell (1977). "Little Green Men, White Dwarfs or Pulsars?". Cosmic Search Magazine. Retrieved 2008-01-30. (after-dinner speech with the title of Petit Four given at the Eighth Texas Symposium on Relativistic Astrophysics; first published in Annals of the New York Academy of Science, vol. 302, pp. 685–689, Dec. 1977).
13. Bell Burnell, S. Jocelyn (23 April 2004). "So Few Pulsars, So Few Females". Science. 304 (5670): 489. doi: 10.1126/science.304.5670.489 . PMID   15105461.
14. Courtland, Rachel. "Pulsar Detected by Gamma Waves Only Archived 2015-07-02 at the Wayback Machine ". New Scientist, 17 October 2008.
15. Daily Telegraph, 21/3, 5 March 1968.
16. Baade, W.; Zwicky, F. (1934). "Remarks on Super-Novae and Cosmic Rays" (PDF). Physical Review. 46 (1): 76. Bibcode:1934PhRv...46...76B. doi:10.1103/PhysRev.46.76.2.
17. Woltjer, L. (1964). "X-rays and Type I Supernova Remnants". Astrophysical Journal. 140: 1309. Bibcode:1964ApJ...140.1309W. doi: 10.1086/148028 .
18. Pacini, F. (1967). "Energy Emission from a Neutron Star". Nature. 216 (5115): 567–568. Bibcode:1967Natur.216..567P. doi:10.1038/216567a0. S2CID   4282721.
19. Gold, T. (1968). "Rotating Neutron Stars as the Origin of the Pulsating Radio Sources". Nature. 218 (5143): 731–732. Bibcode:1968Natur.218..731G. doi:10.1038/218731a0. S2CID   4217682.
20. Comella, J. M.; Craft, H. D.; Lovelace, R. V. E.; Sutton, J. M.; Tyler, G. Leonard (February 1969). "Crab Nebula Pulsar NP 0532". Nature. 221 (5179): 453–454. Bibcode:1969Natur.221..453C. doi:10.1038/221453a0. ISSN   0028-0836.
21. Lovelace, R. V. E.; Sutton, J. M.; Salpeter, E. E. (April 1969). "Digital Search Methods for Pulsars". Nature. 222 (5190): 231–233. Bibcode:1969Natur.222..231L. doi:10.1038/222231a0. ISSN   0028-0836.
22. Lovelace, R. V. E.; Tyler, G. L. (2012-06-01). "On the discovery of the period of the Crab Nebular pulsar". The Observatory. 132 (3): 186–188. Bibcode:2012Obs...132..186L. ISSN   0029-7704.
23. Lyne & Graham-Smith, pp. 1–7 (1998).
24. "Press Release: The Nobel Prize in Physics 1974". 15 October 1974. Retrieved 2014-01-19.
25. Bell Burnell, S. Jocelyn. "Little Green Men, White Dwarfs, or Pulsars?" Archived 2019-06-07 at the Wayback Machine . Annals of the New York Academy of Science, vol. 302, pp. 685–689, Dec. 1977.
26. Weisberg, J.M.; Nice, D.J. & Taylor, J.H. (2010). "Timing measurements of the relativistic binary pulsar PSR B1913+ 16". The Astrophysical Journal. 722 (2): 1030–1034. arXiv: 1011.0718 . Bibcode:2010ApJ...722.1030W. doi:10.1088/0004-637X/722/2/1030. S2CID   118573183.
27. "Nobel Prize in Physics 1993" . Retrieved 2010-01-07.
28. D. Backer; Kulkarni, Shrinivas R.; Heiles, Carl; Davis, M. M.; Goss, W. M. (1982). "A millisecond pulsar". Nature. 300 (5893): 315–318. Bibcode:1982Natur.300..615B. doi:10.1038/300615a0. S2CID   4247734.
29. Antonelli, Marco; Montoli, Alessandro; Pizzochero, Pierre (November 2022), "Insights into the Physics of Neutron Star Interiors from Pulsar Glitches", Astrophysics in the XXI Century with Compact Stars, pp. 219–281, arXiv: 2301.12769 , doi:10.1142/9789811220944_0007, ISBN   978-981-12-2093-7
30. Ikhsanov, Nazar R. (1998). "The pulsar-like white dwarf in AE Aquarii". Astronomy and Astrophysics . 338: 521–526. Bibcode:1998A&A...338..521I.
31. Terada, Yukikatsu; Hayashi, Takayuki; Ishida, Manabu; Mukai, Koji; Dotani, Tadayasu; Okada, Shunsaku; Nakamura, Ryoko; Naik, Sachindra; Bamba, Aya; Makishima, Kazuo (2008-04-25). "Suzaku Discovery of Hard X-Ray Pulsations from a Rotating Magnetized White Dwarf, AEAquarii". Publications of the Astronomical Society of Japan. 60 (2): 387–397. arXiv: 0711.2716 . Bibcode:2008HEAD...10.1003T. doi: 10.1093/pasj/60.2.387 . ISSN   0004-6264.
32. Buckley, D. A. H.; Meintjes, P. J.; Potter, S. B.; Marsh, T. R.; Gänsicke, B. T. (2017-01-23). "Polarimetric evidence of a white dwarf pulsar in the binary system AR Scorpii". Nature Astronomy. 1 (2): 0029. arXiv: 1612.03185 . Bibcode:2017NatAs...1E..29B. doi:10.1038/s41550-016-0029. ISSN   2397-3366. S2CID   15683792.
33. Marsh, T. R.; Gänsicke, B. T.; Hümmerich, S.; Hambsch, F.-J.; Bernhard, K.; Lloyd, C.; Breedt, E.; Stanway, E. R.; Steeghs, D. T. (September 2016). "A radio-pulsing white dwarf binary star". Nature. 537 (7620): 374–377. arXiv: 1607.08265 . Bibcode:2016Natur.537..374M. doi:10.1038/nature18620. PMID   27462808. S2CID   4451512.
34. Schwope, Axel; Marsh, R.; Standke, A.; Pelisoli, I.; Potter, S.; Buckley, D.; Munday, J.; Dhillon, V. (2023). "X-ray properties of the white dwarf pulsar eRASSU J191213.9−441044". Astronomy and Astrophysics. 674: 387–397. arXiv: 0711.2716 . Bibcode:2023A&A...674L...9S. doi: 10.1093/pasj/60.2.387 . ISSN   0004-6264.
35. Pelisoli, Ingrid; Marsh, T. R.; Buckley, David A. H.; Heywood, I.; Potter, Stephen B.; Schwope, Axel; Brink, Jaco; Standke, Annie; Woudt, P. A.; Parsons, S. G.; Green, M. J.; Kepler, S. O.; Munday, James; Romero, A. D.; Breedt, E. (2023-06-15). "A 5.3-min-period pulsing white dwarf in a binary detected from radio to X-rays". Nature Astronomy. 7 (8): 931–942. arXiv: 2306.09272 . Bibcode:2023NatAs...7..931P. doi:10.1038/s41550-023-01995-x. ISSN   2397-3366. S2CID   259164753.
36. Blinova, A. A.; Romanova, M. M.; Ustyugova, G. V.; Koldoba, A. V.; Lovelace, R. V. E. (2019). "Comparisons of MHD propeller model with observations of cataclysmic variable AE Aqr". Monthly Notices of the Royal Astronomical Society. 487 (2): 1754–1763. arXiv: 1804.10105 . Bibcode:2019MNRAS.487.1754B. doi: 10.1093/mnras/stz1314 .
37. Pelisoli, Ingrid; Sahu, Snehalata; Lyutikov, Maxim; Barkov, Maxim; Gänsicke, Boris T.; Brink, Jaco; Buckley, David A. H.; Potter, Stephen B.; Schwope, Axel; Ramírez, S. H. (2024). "Unveiling the white dwarf in J191213.72 - 441045.1 through ultraviolet observations". Monthly Notices of the Royal Astronomical Society. 527 (2): 3826–3836. arXiv: 2311.05558 . Bibcode:2024MNRAS.527.3826P. doi: 10.1093/mnras/stad3442 .
38. Lyne, A. G.; Graham-Smith, Francis (2006). Pulsar astronomy. Cambridge astrophysics series (3rd ed.). Cambridge: Cambridge University Press. ISBN   978-0-521-83954-9. OCLC   59353151.
39. "Pulsar Beacon Animation" . Retrieved 2010-04-03.
40. "Pulsars" . Retrieved 2010-04-03.
41. Arzoumanian, Zaven; Gendreau, Keith (December 2019). "Focus on NICER Constraints on the Dense Matter Equation of State". The Astrophysical Journal Letters. Retrieved 14 December 2019.
42. Garner, Rob (11 December 2019). "NASA's NICER Delivers Best-ever Pulsar Measurements, 1st Surface Map". NASA. Retrieved 14 December 2019.
43. "Pulsars". www.cv.nrao.edu. Archived from the original on 2020-11-12. Retrieved 2018-09-15.
44. "Old Pulsars Still Have New Tricks to Teach Us". Staff. ESA. 26 July 2006. Retrieved 30 April 2013.
45. "Einstein@Home 'citizen scientists' in the U.S.A. and Germany discover a new pulsar in Arecibo telescope data" (PDF). Albert Einstein Institut (Press release). Hannover, DE: Max Planck Institut für Gravitationsphysik. 2010-08-12. Archived from the original (PDF) on 2010-08-14. Retrieved 2010-09-23. – Background material on "disrupted recycled pulsar" PSR J2007+2722 .
46. "Voyager – The Spacecraft". voyager.jpl.nasa.gov.
47. Marissa Cevallos, Science News, "How to Use a Pulsar to Find Starbucks" Archived 2012-07-31 at the Wayback Machine , Discovery News, Nov 24, 2010.
48. Angelo Tartaglia; Matteo Luca Ruggiero; Emiliano Capolongo (2011). "A null frame for spacetime positioning by means of pulsating sources". Advances in Space Research. 47 (4): 645–653. arXiv: 1001.1068 . Bibcode:2011AdSpR..47..645T. doi:10.1016/j.asr.2010.10.023. S2CID   118704955.
49. Commissariat, Tushna (4 June 2014). "Pulsars map the way for space missions". Physics World.
50. "An Interplanetary GPS Using Pulsar Signals". MIT Technology Review. 23 May 2013. Archived from the original on 29 November 2014. Retrieved 13 March 2021.
51. Becker, Werner; Bernhardt, Mike G.; Jessner, Axel (2013). "Autonomous Spacecraft Navigation With Pulsars". Acta Futura. 7 (7): 11–28. arXiv: 1305.4842 . Bibcode:2013AcFut...7...11B. doi:10.2420/AF07.2013.11. S2CID   118570784.
52. Witze, Alexandra (2018). "NASA test proves pulsars can function as a celestial GPS". Nature. 553 (7688): 261–262. Bibcode:2018Natur.553..261W. doi: 10.1038/d41586-018-00478-8 .
53. John G. Hartnett; Andre Luiten (2011). "Colloquium: Comparison of Astrophysical and Terrestrial Frequency Standards". Reviews of Modern Physics. 83 (1): 1–9. arXiv: 1004.0115 . Bibcode:2011RvMP...83....1H. doi:10.1103/RevModPhys.83.1. S2CID   118396798.
54. Matsakis, D. N.; Taylor, J. H.; Eubanks, T. M. (1997). "A Statistic for Describing Pulsar and Clock Stabilities" (PDF). Astronomy and Astrophysics. 326: 924–928. Bibcode:1997A&A...326..924M. Archived from the original (PDF) on 2011-07-25. Retrieved 2010-04-03.
55. Backer, Don (1984). "The 1.5 Millisecond Pulsar". Annals of the New York Academy of Sciences. 422 (Eleventh Texas Symposium on Relativistic Astrophysics): 180–181. Bibcode:1984NYASA.422..180B. doi:10.1111/j.1749-6632.1984.tb23351.x. S2CID   120371785. Archived from the original on 2013-01-05. Retrieved 2010-02-14.
56. "World's most accurate clock to be built in Gdańsk". Polska Agencja Prasowa. 2010. Retrieved 2012-03-20.^{[ permanent dead link ‍]}
57. "African Skies 4 – Radio Pulsar Glitch Studies".
58. "Pulsar timing irregularities reveals hidden gravitational-wave background". Physics World. 2023-06-29. Retrieved 2023-07-11.
59. Antonelli, Marco; Basu, Avishek; Haskell, Brynmor (2023-02-07). "Stochastic processes for pulsar timing noise: fluctuations in the internal and external torques". Monthly Notices of the Royal Astronomical Society. 520 (2): 2813–2828. arXiv: 2206.10416 . doi: 10.1093/mnras/stad256 . ISSN   0035-8711.
60. Ferrière, Katia (2001). "The Interstellar Environment of Our Galaxy". Reviews of Modern Physics. 73 (4): 1031–1066. arXiv: astro-ph/0106359 . Bibcode:2001RvMP...73.1031F. doi:10.1103/RevModPhys.73.1031. S2CID   16232084.
61. Taylor, J. H.; Cordes, J. M. (1993). "Pulsar Distances and the Galactic Distribution of Free Electrons". Astrophysical Journal. 411: 674. Bibcode:1993ApJ...411..674T. doi: 10.1086/172870 .
62. Rickett, Barney J. (1990). "Radio Propagation Through the Turbulent Interstellar Plasma". Annual Review of Astronomy and Astrophysics. 28: 561–605. Bibcode:1990ARA&A..28..561R. doi:10.1146/annurev.aa.28.090190.003021.
63. Rickett, Barney J.; Lyne, Andrew G.; Gupta, Yashwant (1997). "Interstellar Fringes from Pulsar B0834+06". Monthly Notices of the Royal Astronomical Society . 287 (4): 739–752. Bibcode:1997MNRAS.287..739R. doi: 10.1093/mnras/287.4.739 .
64. Pen, Ue-Li; Levin, Yuri (2014). "Pulsar scintillations from corrugated reconnection sheets in the interstellar medium". Monthly Notices of the Royal Astronomical Society . 442 (4): 3338–3346. arXiv: 1302.1897 . doi: 10.1093/mnras/stu1020 .
65. Angelil, R.; Saha, P.; Merritt, D. (2010). "Towards relativistic orbit fitting of Galactic center stars and pulsars". The Astrophysical Journal. 720 (2): 1303–1310. arXiv: 1007.0007 . Bibcode:2010ApJ...720.1303A. doi:10.1088/0004-637X/720/2/1303. S2CID   118449684.
66. Deneva, J. S.; Cordes, J. M.; Lazio, T. J. W. (2009). "Discovery of Three Pulsars from a Galactic Center Pulsar Population". The Astrophysical Journal Letters. 702 (2): L177–182. arXiv: 0908.1331 . Bibcode:2009ApJ...702L.177D. doi:10.1088/0004-637X/702/2/L177. S2CID   14133127.
67. Abt, Helmut A. (May 2011). "The Age of the Local Interstellar Bubble". The Astronomical Journal. 141 (5): 165. Bibcode:2011AJ....141..165A. doi: 10.1088/0004-6256/141/5/165 .
68. Buckley, D. A. H.; Meintjes, P. J.; Potter, S. B.; Marsh, T. R.; Gänsicke, B. T. (2017-01-23). "Polarimetric evidence of a white dwarf pulsar in the binary system AR Scorpii". Nature Astronomy. 1 (2): 0029. arXiv: 1612.03185 . Bibcode:2017NatAs...1E..29B. doi:10.1038/s41550-016-0029. ISSN   2397-3366. S2CID   15683792.
69. Ikhsanov, Nazar R. (1998). "The pulsar-like white dwarf in AE Aquarii". Astronomy and Astrophysics. 338: 521–526. Bibcode:1998A&A...338..521I.
70. Terada, Yukikatsu; Hayashi, Takayuki; Ishida, Manabu; Mukai, Koji; Dotani, Tadayasu; Okada, Shunsaku; Nakamura, Ryoko; Naik, Sachindra; Bamba, Aya; Makishima, Kazuo (2008-04-25). "Suzaku Discovery of Hard X-Ray Pulsations from a Rotating Magnetized White Dwarf, AEAquarii". Publications of the Astronomical Society of Japan. 60 (2): 387–397. arXiv: 0711.2716 . Bibcode:2008HEAD...10.1003T. doi: 10.1093/pasj/60.2.387 . ISSN   0004-6264.
71. O'Brien, Tim. "Part-time pulsar yields new insight into inner workings of cosmic clocks | Jodrell Bank Centre for Astrophysics". www.jb.man.ac.uk. Retrieved 23 July 2017.
72. Kong, Ling-Da; Zhang, Shu; Zhang, Shuang-Nan; Ji, Long; Doroshenko, Victor; Santangelo, Andrea; Chen, Yu-Peng; Lu, Fang-Jun; Ge, Ming-Yu; Wang, Peng-Ju; Tao, Lian; Qu, Jin-Lu; Li, Ti-Pei; Liu, Cong-Zhan; Liao, Jin-Yuan (2022-07-01). "Insight-HXMT Discovery of the Highest-energy CRSF from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124". The Astrophysical Journal Letters. 933 (1): L3. arXiv: 2206.04283 . Bibcode:2022ApJ...933L...3K. doi: 10.3847/2041-8213/ac7711 . ISSN   2041-8205. S2CID   249538417.
73. "Astronomers measure strongest magnetic field ever detected". New Atlas. 2022-07-15. Retrieved 2022-08-22.
74. Croswell, Ken (2022-07-22). "The heaviest neutron star on record is 2.35 times the mass of the sun". Science News. Retrieved 2022-07-25.
75. Romani, Roger W.; Kandel, D.; Filippenko, Alexei V.; Brink, Thomas G.; Zheng, WeiKang (2022-07-11). "PSR J0952−0607: The Fastest and Heaviest Known Galactic Neutron Star". The Astrophysical Journal Letters. 934 (2): L17. arXiv: 2207.05124 . Bibcode:2022ApJ...934L..17R. doi: 10.3847/2041-8213/ac8007 . S2CID   250451299.
76. Champion, David J.; Ransom, S. M.; Lazarus, P.; Camilo, F.; Bassa, C.; Kaspi, V. M.; Nice, D. J.; Freire, P. C. C.; Stairs, I. H.; Van Leeuwen, J.; Stappers, B. W.; Cordes, J. M.; Hessels, J. W. T.; Lorimer, D. R.; Arzoumanian, Z.; Backer, D. C.; Bhat, N. D. R.; Chatterjee, S.; Cognard, I.; Deneva, J. S.; Faucher-Giguere, C.-A.; Gaensler, B. M.; Han, J.; Jenet, F. A.; Kasian, L.; Kondratiev, V. I.; Kramer, M.; Lazio, J.; McLaughlin, M. A.; et al. (2008). "An Eccentric Binary Millisecond Pulsar in the Galactic Plane". Science. 320 (5881): 1309–1312. arXiv: 0805.2396 . Bibcode:2008Sci...320.1309C. doi:10.1126/science.1157580. PMID   18483399. S2CID   6070830.
77. Knispel, B.; Allen, B; Cordes, JM; Deneva, JS; Anderson, D; Aulbert, C; Bhat, ND; Bock, O; et al. (2010). "Pulsar Discovery by Global Volunteer Computing". Science. 329 (5997): 1305. arXiv: 1008.2172 . Bibcode:2010Sci...329.1305K. doi:10.1126/science.1195253. PMID   20705813. S2CID   29786670.
78. Pletsch, H. J.; Guillemot; Fehrmann, H.; Allen, B.; Kramer, M.; Aulbert, C.; Ackermann, M.; Ajello, M.; De Angelis, A.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; et al. (2012). "Binary millisecond pulsar discovery via gamma-ray pulsations". Science. 338 (6112): 1314–1317. arXiv: 1211.1385 . Bibcode:2012Sci...338.1314P. doi:10.1126/science.1229054. PMID   23112297. S2CID   206544680.

Further reading

• Lorimer, Duncan R.; Kramer, Michael (2004). Handbook of Pulsar Astronomy. Cambridge University Press. ISBN   978-0-521-82823-9.
• Lorimer, Duncan R. (2008). "Binary and Millisecond Pulsars". Living Reviews in Relativity. 11 (1): 8. arXiv: 0811.0762 . Bibcode:2008LRR....11....8L. doi: 10.12942/lrr-2008-8 . PMC   5256074 . PMID   28179824.
• Lyne, Andrew G.; Graham-Smith, Francis (1998). Pulsar Astronomy. Cambridge University Press. ISBN   978-0-521-59413-4.
• Manchester, Richard N.; Taylor, Joseph H. (1977). Pulsars . W. H. Freeman and Company. ISBN   978-0-7167-0358-7.
• Stairs, Ingrid H (2003). "Testing General Relativity with Pulsar Timing". Living Reviews in Relativity. 6 (1): 5. arXiv: astro-ph/0307536 . Bibcode:2003LRR.....6....5S. doi: 10.12942/lrr-2003-5 . PMC   5253800 . PMID   28163640.

External links

• "A Pulsar Discovery: First Optical Pulsar Archived 2007-10-03 at the Wayback Machine ". Moments of Discovery, American Institute of Physics, 2007 (Includes audio and teachers guides).
• Discovery of Pulsars: Interview with Jocelyn Bell Burnell. Jodcast, June 2007 (Low Quality Version).
• Audio: Cain/Gay – Astronomy Cast. Pulsars – Nov 2009
• Australia National Telescope Facility: Pulsar Catalogue
• Johnston, William Robert. "List of Pulsars in Binary Systems". Johnston Archive, 22 March 2005.