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Pulsar

A pulsar (from pulsating radio source) is a highly magnetized rotating neutron star that emits beams of electromagnetic radiation out of its magnetic poles. This radiation can be observed only when a beam of emission is pointing toward Earth (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.)

The periods of pulsars make them very useful tools for astronomers. 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.

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, the fact that the signals always appeared at the same declination and right ascension soon ruled out a terrestrial source. 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. 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.

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?" Even so, they nicknamed the signal LGM-1, for "little green men" (a playful name for intelligent beings of extraterrestrial origin). It was not until a second pulsating source was discovered in a different part of the sky that the "LGM hypothesis" was entirely abandoned. 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.

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.'

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. 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). 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. 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. In 1968, Richard V. E. Lovelace with collaborators discovered period $$P \approx 33$$ ms of the Crab Nebula pulsar using Arecibo Observatory. The discovery of the Crab pulsar provided confirmation of the rotating neutron star model of pulsars. 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. 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". 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.

Milestones

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 continues to agree with general relativity. In 1993, the Nobel Prize in Physics was awarded to Taylor and Hulse for the discovery of this pulsar.

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). 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. However, no general scheme for glitch forecast is known to date.

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. 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, 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 (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.

 * In 2023, it was suggested that the white dwarf eRASSU J191213.9−441044 acts as a pulsar both in radio and X-rays.

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. 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.

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.

Formation, mechanism, turn off
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 (and therefore its moment of inertia is sharply reduced), 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. In rotation-powered pulsars, the beam is the result of the rotational energy of the neutron star, which generates an electrical field from the movement of the 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. 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. 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.

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."

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 power, 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.

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. This velocity decreases slowly but steadily, except for an occasional sudden variation – a "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.

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 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.

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
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. 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.

Pulsar 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. Experimental demonstrations have been reported in 2018.

Precise clocks
Generally, the regularity of pulsar emission does not rival the stability of atomic clocks. They can still be used as external reference. For example, J0437−4715 has a period of $0.006$ s with an error of $1.7 s$. This stability allows millisecond pulsars to be used in establishing ephemeris time or in building pulsar clocks.

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. It is unknown whether timing noise is related to pulsar glitches. According to a study published in 2023, 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.

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.

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:

 * $$\mathrm{DM} = \int_0^D n_e(s) \,ds,$$

where $$D$$ is the distance from the pulsar to the observer, and $$n_e$$ is the electron density of the ISM. The dispersion measure is used to construct models of the free electron distribution in the Milky Way.

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. 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. The exact cause of these density inhomogeneities remains an open question, with possible explanations ranging from turbulence to current sheets.

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. 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; 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*.

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
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.
 * 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.
 * The first white dwarf pulsar AE Aquarii.
 * 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. One of only two pulsars known to have stopped pulsing for more than a few minutes.
 * Swift J0243.6+6124 most magnetic pulsar with $16,000,000,000,000 G$.
 * PSR J0952-0607 heaviest pulsar with $2.35$.
 * PSR J1903+0327, a ~2.15 ms pulsar discovered to be in a highly eccentric binary star system with a Sun-like star.
 * 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.
 * PSR J1311–3430, the first millisecond pulsar discovered via gamma-ray pulsations and part of a binary system with the shortest orbital period.

title: Pulsar


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Talk:Pulsar

Merge Radio pulsar & X-ray pulsar into Pulsar
User:Quarl has suggested merging both accretion powered pulsar and rotation powered pulsar into the general pulsar article on the Astronomy WikiProject talk page.
 * 70.51.8.30 05:21, 3 March 2007 (UTC)

Discussion

 * We have smaller articles on types of pulsars than either X-ray or radio pulsar, they can be expanded to a fair degree, I would keep them separate and make pulsar into a better overview of pulsars in general. It should overview most types of pulsars, including magnetars, AXP, SGR, short duration GRB, millisecond pulsars, etc. 70.51.8.30 05:27, 3 March 2007 (UTC)

I agree, I don't see a reason by those two should be selected out in particular for merging. Why not also merge magnetars since their mechanism of action is different? Rather each of the individual branch articles should be improved and the pulsar article should be grown with material common of all pulsars - pulsar origins, physics involved, observation methods, history,etc. – Meowist 20:28, 8 July 2007 (UTC)

"Religious interpretations"
I took out this:

Some modern Islamic scholars believe that the Qur'an has mentioned the pulsars: "[I swear] by Heaven and the Tariq! And what will convey to you what the Tariq is? The Star Piercing [the darkness]! " (Qur'an, 86:1-3). The Arabic word "Tariq," comes from the root "tarq," whose basic meaning is that of striking hard enough to produce a sound, or hitting. Bearing in mind the word's possible meaning as "beating," "striking hard," our attention may be being drawn to this scientific fact.

Because it's not referenced. The footnote posing as a reference for it read this: This is not the only scientific fact mentioned in the Quran; many other scientific facts in  the variance science fields (e.g. Astronomy, biology, medicine,…etc), which were discovered in the 19th and 20th centuries, are mentioned in the Quran. A website authored by one person is not "some modern Islamic scholars". The claim that people believe that the Qur'an is unequivocally referring to scientific principles for which the ancients had no scientific measures is quite extraordinary, and requires extraordinary citation. As it stands, this reads as one man's theory, if not outright promotion.

I see Harun Yahya already has an article; his theories are more appropriately discussed in that article rather than adding backreferences to every other "scientific fact" supposedly appearing in the Qur'an. 82.95.254.249 13:11, 23 June 2007 (UTC)

 * I deleted a similar block:

Strangely enough the Quran, Muslims' holy book revealed more than 1400 years ago, speaks about pulsars in chapter 86. The original Arabic word used for these stars is 'Tariq'. The verses go on describing the Tariq as the piercing star. Those who translated the word Tariq into other languages did not translate it accurately but most native speakers of Arabic know the meaning of Tariq as 'someone or something knocking on a door or striking with a hammer'.
 * — Preceding unsigned comment added by 70.95.252.126 (talk) 02:26, 1 March 2008 (UTC)

 * WTF? It's back there again! Well, I'm going to delete it now. If it appears for a fourth time, I will request semi-protection. --116.14.34.220 (talk) 14:51, 15 June 2009 (UTC)

 * ;^#) Especially the connection between "Tariq" and "pulsar" seems to be requiring extraordinary proof, or else that tariq stuff requires extraordinarily violent deletion, being a kind of hallucinating double UFO-logy. ... said: Rursus ( m b o r k³ ) 12:33, 14 August 2009 (UTC)

I removed a similar addition to the miscellaneous facts portion of the article today. 66.91.241.126 (talk) 20:30, 18 June 2009 (UTC)

More scientific details needed
A few examples of things that should probably be in this article. I've searched the web, and can't find them, so anyone with knowledge, please contribute: The above would help describe what a pulsar is/does, not just the history behind their discover. Thanks to any who can contribute. —Ryan McDaniel 22:17, 6 July 2007 (UTC)
 * Radiated spectrum: are they broadband pulses, or narrowband? A few articles I found suggested narrowband, but none made any general conclusions.
 * If they're narrowband, are their peak frequencies scattered all over the spectrum? Or do pulsars tend to radiate within a small range?  Also, if narrowband, does the peak frequency remain constant over time?
 * It may also be instructive to include a plot of intensity vs. frequency for an example pulsar.
 * Pulse duration vs. non-radiating period. The article mentions periods of 1.5ms to 8s, but for how much of that time are they "pulsing"?  I realize that that probably depends on distance from the Earth, so maybe a better metric is the solid angle size of the radiated cone.  Is this about the same size for most pulsars, or does it vary greatly?
 * Is there any noticeable precession of the radiation (or rotation) axis?
 * Just flagged this as "attention=yes" on the Physics template; this article needs attention I can't give it. If this is not a proper use of that attribute, I apologize.  —Ryan McDaniel 21:14, 11 July 2007 (UTC)

Discovery of pulsars before Jocelyn
Apparently, the US Air Force detected pulsars a couple of months before Jocelyn Bell discovered them; see. Unfortunately, I can't find a better reference for it than that, hence why I'm commenting here rather than adding it to the article. Mike Peel 10:46, 19 August 2007 (UTC)

Patrick1982 added some interesting new text about Charles Schisler's discovery of pulsars pre-dating that of Bell & Hewish. While there is nothing to doubt Schisler's claim, his result is not unique. Several other groups had discovered pulsars beforehand, but either had not realized what they had found, or did not follow up on it - see for example. I think a discussion of Schisler's and other preceding work (not the least of which would be Minkowski's identification of the stellar remnant in the Crab Nebula in 1942) has a place somewhere in this article, but certainly the main credit for the discovery should go to those who followed through with their discovery and who were in a position to publish their result. Let's discuss this further on the talk page before changing the main article. Tubbs334 11:36, 7 September 2007 (UTC)

 * I can understand your reasons for reverting back to the previous version. However in my opinion it is wrong to just leave this new information out of the article, treating it like it "did not happen". I think that my formulation did not weaken the credit atribution towards Bell & Hewish. In fact, I did not even change that paragraph, I simply added a new one.
 * But perhaps it would be best to add a small paragraph at the bottom of the discovery section, or perhaps even at the end of Subsequent history, as an 'additional footnote in history'. I think a publication in Nature, and the subsequent media coverage that was given to it (it was in every newspaper), justifies this. And this can be extended/reformulated to include other pre-discovery's. --Patrick1982 23:16, 8 September 2007 (UTC)

 * Patrick1982, I agree with you 100%. This should be in the article, and I am not concerned about protecting Bell & Hewish's legacy. But it shouldn't be presented as "we used to say that Bell discovered pulsars but the correct answer is now Schisler", since the full situation is more complex. I think a subsequent "footnote" is a good way to do it, as you propose. Tubbs334 14:12, 9 September 2007 (UTC)

To resuscitate this discussion—I removed a sentence placed at the start of the discovery section noting that the optical counterpart of the Crab Pulsar was discovered in 1899. While these archival data of pulsars are interesting, the coverage in the literature clearly supports the fact that Jocelyn Bell Burnell's observations mark the discovery of pulsars. Some coverage of archival data might be added, but it should not be in the first post-lead sentence. James McBride (talk) 21:50, 1 October 2012 (UTC)

While I understand the desire to include more information about the history of pulsars, I think there's blurring happening here between two different things. Detection and discovery. Without a doubt people detected the results of pulsars long before Bell. Just like nearly every living thing detected gravity before Einstein's work. But what's special, interesting, and useful is realizing what causes the thing that's being detected. The emissions weren't covered, the reality behind them was. So if you want to say the energy emissions of pulsars were *detected* by others before Bell, that's fine. But only someone who understood what they were finding should be said to have *discovered* pulsars. 72.79.76.198 (talk) 17:26, 25 January 2021 (UTC)

Time standard?
Shouldn't something be said in this article about how pulsars have been proposed for use as an independent check (or alternative time standard) on terrestrial atomic clocks? (See Barycentric Coordinate Time.) I would say it myself if I knew how, but I was trying to do some initial research and found nothing in this article; I think there used to be something about this in one of the various articles about various sorts of pulsars, but haven't found it yet, and really, this is the article that I think it ought to be mentioned in. arkuat (talk) 07:32, 21 February 2008 (UTC)
 * Now some at Pulsar and Millisecond pulsar, both refing the same source. - Rod57 (talk) 12:12, 4 April 2015 (UTC)

First gamma-ray only pulsar
Now a new type of pulsar that emits gamma ray radiation has been discovered as well.

http://www.universetoday.com/2008/10/17/fermi-telescope-makes-first-big-discovery-gamma-ray-pulsar/ -- Chupon (talk) 14:30, 21 October 2008 (UTC)

"The gamma-ray-only pulsar lies within a supernova remnant known as CTA 1, ... in the constellation Cepheus.  Its lighthouse-like beam sweeps Earth’s way every 316.86 milliseconds."
 * — Preceding unsigned comment added by Rod57 (talk • contribs) 08:38, 11 April 2015 (UTC)

Visual?
For X years ago, where X is at most 50 years, only a couple of pulsars where visually identified. What's the current status? I.e.: could the article relate to visual identification. I know for sure that the Crab pulsar is visually identified, but more? ... said: Rursus ( m b o r k³ ) 13:00, 14 August 2009 (UTC)
 * Maybe, we should consider merging the too small Optical pulsar into this article? ... said: Rursus ( m b o r k³ ) 13:07, 14 August 2009 (UTC)

how many neutron stars are pulsars?
What neither this article or "Neutron Stars" makes clear is WHAT PROPORTION of neutron stars are pulsars. Reading the ambiguous text on the "lighthouse effect", readers could well conclude that ALL neutron stars are pulsars, and that we don't see more of them pulse only because the beam from most of them does not sweep across the Earth. It amazes me how such obvious questions do not cross the minds of those who write this stuff. I gather that most neutron stars are NOT pulsars, though why some are and some are not finds no answer here. The following quote from WP article "Neutron Star" is about as close as we get.

If the surface temperature exceeds 106 kelvin (as in the case of a young pulsar), the surface should be fluid instead of the solid phase observed in cooler neutron stars (temperature <106 kelvin)[10]. Myles325a (talk) 04:37, 26 September 2009 (UTC)

 * "106 kelvin" = 10^6 kelvin ? - Rod57 (talk) 13:55, 31 May 2022 (UTC)

 * This is a difficult question to answer properly, as there are many neutron stars observed by other means (e.g. X-rays), which we (scientists) don't know if they are radio pulsars or not. And there are other objects which appear to be radio pulsars at some times, and not to be radio pulsars at other times--some are magnetars (http://adsabs.harvard.edu/abs/2006Natur.442..892C), and some intermittently accrete in binary systems (http://adsabs.harvard.edu/abs/2009Sci...324.1411A).   However, one can make a simple estimate; as the average pulsar lasts probably ~30 million years (see http://www.cv.nrao.edu/course/astr534/Pulsars.html, Fig. 4), but neutron stars have been formed throughout the age of the universe (13.6 billion years), thus of order ~500 times more neutron stars must exist than pulsars--probably more than ~1000 times more, as the star formation rate was higher earlier in our Galaxy's history.  The fraction of neutron stars that are spun up in binary systems to become millisecond radio pulsars is quite small, but they radiate as pulsars for billions of years; the numbers for millisecond pulsars may be similar to the number of pulsars, though that isn't certain.  Craigheinke (talk) 19:05, 29 November 2009 (UTC)

CTA 1
I can't find any evidence of X-ray emission changes in CTA 1, either in the referenced Atkinson article, or in the science literature (see http://www.iop.org/EJ/article/0004-637X/612/1/398/60375.html). So I took that out, and rephrased its notability to be its pulsations only being seen in the gamma-ray. There's a good chance that X-ray pulsations will be detected in the near future, since the existing X-ray pulsation constraints are weak and further observations are being performed. Craigheinke (talk) 19:14, 29 November 2009 (UTC)

PSR J0108-1431 contradiction
Some wiki-styled sources refer to the pulsar as being 280 light years away, however http://chandra.harvard.edu/photo/2009/j0108/ gives an estimate of 770 ly. Can someone doublecheck? —Preceding unsigned comment added by 216.239.79.193 (talk) 04:40, 1 December 2009 (UTC)
 * The recent VLBI parallax measurements by Deller et al give a distance of 240 parsecs, which is about 770 ly. However, the original discovery paper by Tauris et al gives a distance of < 100 parsecs, which is presumably the source of the 280 lightyear figure. Scog (talk) 08:44, 8 December 2009 (UTC)

Pulsar wind?
This article has no explanation of what the pulsar wind is, and pulsar wind simply redirects back here. 99.55.136.210 (talk) 04:47, 1 March 2010 (UTC)

 * I was going to make this exact same comment. Who decided to redirect Pulsar Wind to this article without actually giving an explanation of it? Very frustrating! --InvaderXan (talk) 13:22, 15 July 2010 (UTC)

Again myself too, I was redirected here searching pulsar wind, and there was no explanation of what it actually is. Infringement153 (talk) 09:09, 6 December 2010 (UTC)

 * While this is an ancient section, the objection is still accurate. There is a link to pulsar wind, but no article save the redirect to the pulsar article. There is also no mention of what a pulsar wind is, its mechanisms of operation, etc. If there is no objection, I'll remove the link to the non-existent article.Wzrd1 (talk) 00:52, 9 November 2013 (UTC)

 * Even better, I'll change the link to go to the article Pulsar wind nebula, which explains pulsar wind briefly.Wzrd1 (talk) 04:28, 10 November 2013 (UTC)

How Is It Possible?
How is it possible for Neutron Stars (which are supposedly electrically neutral) to have charged particles around them and emit radio pulses? Shouldn't the super strong gravitational field pull the particles into the star and neutralize them? I know that everything with a surface temperature different from it's immediate environment radiates; what is a pulsar's surface temperature?JeepAssembler (talk) 20:48, 7 August 2010 (UTC)JeepAssemblerJeepAssembler (talk) 20:48, 7 August 2010 (UTC)

 * Well, if you look at the equation of state of a neutron star, you see that the star isn't simply a solid ball of neutrons. Yes, the inside of the star is made up entirely of neutrons (most likely in a superfluid state), but the crust of the star is not. At the surface of the star it is mostly composed of iron (Fe). As you move into the star, the ever increasing pressure pushes more and more of the electrons into the nuclei of the atoms, thus forming increasingly absurdly heavy isotopes of the 'lighter' element, until the pressure becomes so high that all the electrons are pushed into the nuclei, and the entire mass becomes homogeneously neutron material. In short, this means that at the surface of the neutron star there are atoms with magnetically charged components, which can be acted on by the extremely strong induced electric field (specifically the component of it perpendicular to the magnetic field). This electric field is strong enough to pull charged particles out of the surface (against the strong gravitational field), and accelerate them to very high speeds in a comparatively short distance (as shown by Goldreich & Julian (1969)). The models of how these particles are accelerated etc., predict that their speeds will be ultra-relativistic (i.e., super close to the speed of light) after only a few millimeters of motion (as little as 3mm or so). This doesn't happen everywhere, however, only over the polar regions of the pulsars (magnetic poles, not rotational poles). The magnetosphere of the pulsar is divided into two regions, the closed region and the open region. The boundary between these two regions is delimited by the last field line that closes inside the so-called light cylinder. Basically any field line closer to the magnetic pole than this line would have to close at a distance farther from the pulsar than the distance at which something would need to move at the speed of light just to co-rotate with the pulsar (like a geostationary satellite staying over a certain spot on the Earth's surface). Because all the field lines in the closed region are, well, closed inside the light cylinder, no charged particles can escape this region, and the charged particle plasma nullifies the accelerating electric field in this region. Thus, the closed region consists of a cloud of charged particles co-rotating with the neutron star. In the open region the particles can escape through the light cylinder, meaning that there is a continual stream of charged particles flowing out from the neutron star surface at the magnetic polar caps. It's radiation from these particles that we see, and it is this geometry (open and closed regions) which is responsible for the beamed-ness of the emission. About the surface temperature of pulsars: Well this is a slightly more involved topic, but the basic fact is that the polar caps are much hotter than the rest of the neutron stars surface, and are the sources of some of the radiation we see in x-ray pulsars (the so-called thermal x-ray component). I'm not going to describe how the heating actually happens, because that's way more detail than I want to go into here, but what I've put down should be interesting enough. Tjips (talk) 13:37, 19 November 2012 (UTC)

How is it possible for a pulsar's magnetic axis to be at a high angle from the axis of rotation? SEppley (talk) 18:33, 29 April 2012 (UTC)

For 46 years scientists have been perfecting this incomplete model of the Pulsar oscillating source. Did anyone once stop to ask why the 'rotating lighthouse' idea still continues? I seems perfectly inane for intelligent humans to be discussing a mechanical principle left over from 200 years ago when modern engineers can do flashing sources far more simply. In fact the first radio transmitters used the simple tuned spark gap which utilises the non-linear ionised air (plasma) as the feedback loop. No moving parts and ultimately very efficient to have an electrical resonance, hence most modern lighthouses convert to strobes or flashing LEDs. Two charged stars, a bit of plasma atmosphere and resonant lightning does the trick. Find an x-ray machine that uses gravity rather than electricity, I think not!

The trouble is Cosmologists and Particle Physicists have been patching up their wonderful theories for decades. No-one can prove them wrong, although you have to laugh at the list of entities they have cooked up! I recommend a read of this page for more straight talking.Cigarshaped (talk) 21:04, 19 January 2014 (UTC)

 * That's all we have until we can go out there and visit the things up close. And by then, expect to have your cherished assumptions dashed asunder. Kortoso (talk) 21:42, 21 October 2014 (UTC)

 * @Cigarshaped maybe some Pulsar uses an oscillator to flash. But you have to explain where the energy for the signals comes, and if you use gravitational energy you have to explain how the frequecy decreases with radius. And you have to bring other references from someone seriously exploring this possibility, because repeating "this or that is mostly unlikely", as in your holoscience page, doesn't mean serious science per se 194.174.76.21 (talk) 19:19, 28 February 2017 (UTC) Marco Pagliero Berlin

Pulsar life history
Please tell what the life cycle of a pulsar is. Article tells how they form. Since they keep giving off energy, what's the long term fate of them? —Preceding unsigned comment added by 72.83.70.206 (talk) 22:43, 1 May 2011 (UTC)

 * It depends on the system; binaries will obviously evolve differently from lone pulsars. However, for all cases, they will eventually cool off (i.e. run out of energy) since they are no longer engaged in nuclear fusion, and as they do their emitted energy drops over time until it becomes undetectable. siafu (talk) 23:34, 1 May 2011 (UTC)

Pulsar Wind
This article could be improved by adding a section explaining Pulsar Winds. The only article with information regarding it, is the 'pulsar wind nebula' page. A pulsar wind is a significant aspect of the Pulsars, hence adding a section on it should be prioritized on further expansions of the article.

Pulsar wind nebula - page: http://en.wikipedia.org/wiki/Pulsar_wind_nebula  — Preceding unsigned comment added by Fredrikdn (talk • contribs) 14:12, 29 July 2012 (UTC)

New research
'The scientists identified a pulsar that is able to dramatically change the way in which it shines. In just a few seconds, the star can quiet its radio waves while at the same time it makes its X-ray emissions much brighter. The research “challenges all proposed pulsar emission theories,” the team writes in the Jan. 25 edition of the journal Science and reopens a decades-old debate about how these stars work." ' From http://www.sciencedaily.com/releases/2013/01/130124183444.htm. -- Jo3sampl (talk) 19:33, 25 January 2013 (UTC)

 * Seems anthropomorphic to me. Kortoso (talk) 21:43, 21 October 2014 (UTC)

Significant pulsars
The section on significant pulsars section has been tagged as "trivia" for awhile. It was just removed today (though I restored it) with the comment "no criterion for 'significance'". I think there are pretty clearly two criteria that encompass the majority of listed pulsars: "firsts" and record holders of various types. There are probably a couple of pulsars that don't really belong (and perhaps I'll just go ahead and trim the list a little after this), but for the most part it seems to be a fairly selectively populated list, and thus isn't truly a trivia section. I think the content and layout of the section could be improved, but disagree completely with removing it entirely. James McBride (talk) 04:54, 17 April 2013 (UTC)

pioneer plaque
To root this article in something practical, how about talking about how the earth's position compared to 14 pulsars was the method used on the Pioneer plaques to describe our location to "aliens"? I think a pic of the plaque would be a good graphic here as well. It would show a newby one reason they are so important. Pb8bije6a7b6a3w (talk) 15:54, 14 May 2013 (UTC)
 * Isn't this already in Pulsar?  Reatlas  (talk)  14:46, 15 May 2013 (UTC)
 * Statistically how many of the "aliens" would see any of these 14 pulsars as pulsating? 194.174.76.21 (talk) 18:35, 28 February 2017 (UTC) Marco Pagliero Berlin

Discovery
The sentence "It was not until a second pulsating source was discovered in a different part of the sky that the 'LGM hypothesis' was entirely abandoned" makes it sound like the little green men theory was disproven because there was more than one pulsar discovered. I'm pretty sure there's more science to it than that, but the cite given is not available to ordinary earthlings. Can someone summarize the science that tells us that pulsars are natural phenomena? Kortoso (talk) 17:22, 11 December 2013 (UTC)
 * The entire article explains that.50.111.50.200 (talk) 13:07, 24 June 2020 (UTC)

Pulsar/neutron star connection - non-rotating fringe-theory
The organization and clarity of this article still leave much to be desired. I hope my recent edit clarifies the evidence connecting neutron stars and pulsars, since that issue seemed to underlie the recent edits by User:Cigarshaped. I reverted these edits, because I am not aware of any credible source that argues for an alternative to rotating neutron stars as the source of pulsar emission, and no such source was provided in the edits of User:Cigarshaped. I would like to avoid any edit warring, so if there is more that could be done to improve this area of the article, suggestions are welcome, and I can try to improve the article further. James McBride (talk) 06:14, 20 January 2014 (UTC)

I don't have time for Revert Wars, however, I would ask what is necessary to provide a credible source? There is an extremely promising proposal which follows on from "magnetospheric disk-field-aligned-current transmission line system as the origin of the observed radiation". Healy and Peratt were approaching the pulsar emission from an telecommunication/ electrical engineering POV. Anthony Peratt is a world expert on plasma and knows its emissions well. Since 99.999% of visible universe is plasma Hannes Alfven it suprises me that not more research explores astrophysical phenomena in plasma terms.

The characteristic form of pulsars strangely mimics the signature of lightning strikes. Surely an electrical discharge is a far more plausible explanation for a regular em pulse, particularly when the frequency exceeds 600Hz. I'll say it again. The earliest radio transmitters employed tuned spark gaps in all their noisy glory. Students easily knock up a relaxation oscillator with a pair of capacitors (stars) and a non-linear resistor (plasma). Why should Nature be any different. Modern lighthouse operators are binning their rotating mirrors in favour of strobes or flashing LEDs. What is more efficient? What makes practical sense?

I recommend a read of this page for more straight talking. Cigarshaped (talk) 18:55, 20 January 2014 (UTC)

 * The article that you cite by Healy & Peratt is a credible source. In my first comment, I should have linked to WP:Reliability, which provides criteria for sources that are considered reliable. The link to holoscience.com does not meet the criteria for reliability, as it is self-published.

 * I will not claim to understand all details of the Healy & Peratt article, but their model is still clearly based on a system with a rotating neutron star at its center. Their model draws upon ideas related to transmission lines, and they even provide a simple demonstration of the core ideas of their model using a transmission line system they built, but these ideas are being applied to the conditions of a plasma surrounding a rotating neutron star.

 * Theoretical efforts to understand pulsars are certainly not ignoring plasma physics. In fact, the theoretical astrophysicists that I can think of that work on pulsars describe themselves as studying plasma astrophysics. They are trying to understand in greater detail how a plasma behaves when there is rapidly rotating powerful magnetic dipole at the center of the plasma. As far as I know, the only such object that has been proposed that can spin as rapidly as necessary to excite the surrounding plasma and produce pulsar pulses is a neutron star, or very similar stars in which neutrons have split up into their fundamental particle constituents. I've just scanned the astronomy literature for a model that does not fit this description, and was unable to find anything. Though that doesn't mean such a model doesn't exist, I think that reframing the article in order to cast doubt on the consensus in the astrophysics community that pulsars are powered by neutron stars would place undue weight on alternative models.

 * As for terrestrial origins of pulsars, the observations firmly rule out that possibility. Telescopes in different parts of the Earth at different times are able to observe identical pulsation properties from objects at the same celestial coordinates. There is no way to reproduce this with lightning strikes. James McBride (talk) 19:43, 20 January 2014 (UTC)

It's a bit unfortunate that I could not read the full paper as I would have been more reluctant to quote anything with moving parts at its centre. It is also extremely disturbing that an entire disciplne has failed to come up with a much simpler alternative such as the plasma discharge model. My reference to terrestrial lightning was meant to lead on to cosmic lightning on a stellar scale. As plasma is scalable to 28 orders of magnitude [], any laboratory or terrestrial phenomema can be transferred to the star (or even galactic) situation.

"I think that reframing the article in order to cast doubt on the consensus in the astrophysics community that pulsars are powered by neutron stars would place undue weight on alternative models." Well if you don't give them a kick, they will continue to waste valuable time and resources on this fruitless mechanical hypothesis. Meanwhile the world heads for various crises, totally unprepared for the effects of a galactic mutation of our solar configuration. Our only hope is to start respecting the electrical nature of this delicate universe. I am convinced that our ignorance is being deliberately orchestrated, in order that we will be completely helpless when something serious happens. Anyway you are in a powerful position to influence the next generation of scientists. Breed morons indoctrinated with Einsteinian/mathematical thinking OR free-thinking engineering-based researchers. Here's [] a possible hope.Cigarshaped (talk) 21:44, 20 January 2014 (UTC)

 * Wikipedia is an encyclopedia not a manifesto to influence young scientists. - Rod57 (talk) 14:03, 31 May 2022 (UTC)

Crab Pulsar GIF/video slow-down rate
Hello! In looking up pulsars, I saw the GIF Crab_Lucky_video2.gif (used in both the Pulsar and Crab Pulsar articles) caption simply saying that the GIF's animation speed was slowed down to illustrate the Crab Pulsar's pulses. The articles state that the Crab Pulsar's rotation period is 33 milliseconds, which is 1980 rotations per minute. What I can't seem to find, either on Wikipedia or via Googling other sources, is roughly how much the GIF is slowed down. The GIF appears to be about 1.5 seconds long to me, using Firefox. I think it would be both interesting and informative to have the caption state how much it was slowed down. I don't think '33 milliseconds' would be easy to grasp for the average person, while (for example, if my guess and math are right) 'slowed down by 45 times/4500%' would be more illustrative. Thanks! - Lafin T. Jack 23:34, 27 March 2014 (UTC)

Where are pulse shapes and spectra
What shape and duty cycle are the pulses, and what frequency spectra (of the various type of pulsar). How does pulse width compare to the dispersion ? How do they compare to fast radio bursts ? - Where to look ? - Rod57 (talk) 12:18, 4 April 2015 (UTC)
 * Shapes of 16 mS pulsars in 47 Tuc shown p1360 in Further results from the timing of the millisecond pulsars in 47 Tucanae. Freire et al. 2003. - Rod57 (talk) 08:59, 7 April 2015 (UTC)

Yes! For individual neutron stars (pulsars or not), what are the frequencies of the radio emissions? A spectrum analyzer plot should show. The radio frequencies could identify particles and processes.173.56.18.42 (talk) 18:31, 8 February 2016 (UTC)BG

Good plot of dispersion measure vs galactic latitude
For all pulsars known in 2013 : See fig S2 on p8 of Supplementary materials for 'A Population of Fast Radio Bursts at Cosmological Distances', inc from Magellanic clouds. - Rod57 (talk) 01:21, 7 April 2015 (UTC)

How are pulsar ages calculated
Since there is a table of pulsar ages, can we say how they are calculated - What does it depend on apart from period ? - Rod57 (talk) 01:29, 7 April 2015 (UTC)

No mention of giant pulses
On the origin of a highly dispersed coherent radio burst (doi: 10.1111/j.1745-3933.2012.01306.x) says at least 14 of the pulsars (known in 2012) are known to exhibit giant pulses (inc the crab nebula pulsar). - Rod57 (talk) 01:46, 7 April 2015 (UTC)

Red shifts and faster than light
I have a vague memory of pulsars being considered as an indication of superluminal velocities in 1967, just after the little green men hypothesis was detroyed. It went something like this:

In 1967, the only objects thought to exist with the same energy as pulsars were quasars and, for a time, they were thought of as a type of quasars. Pulsars, as well as quasars, had a redshift which meant (in 1967) they were several million light-years away. However, they pulsed with a frequency of something like a second. Therefore, the generation mechanism couldn't be greater than one light-second across. Thus pulsars (A) must have enough energy to be detectible from millions of light-years (way less than one yocto-arc) and (B) must fit into a space not larger than the distance from Earth to the Moon. So we must examine new sources of energy and the possibility of FTL communication.

Of course, pulsars turned out to be neutron stars (mostly in our galaxy) and the red shift was due to their deep gravitational wells. But if someone could find sources, it would be a nice addendum to the Discovery section. Even if you can't, we should say something about pulsar's redshift. --RoyGoldsmith (talk) 11:12, 23 December 2017 (UTC)

Pulsars definitely do not rival atomic clocks in their accuracy in keeping time
That's not what the cited NYT article says and that sentence doesn't even make any sense. Atomic clocks are accurate to the nanosecond. How can pulsars be used as clocks that are accurate to the nanosecond!? — Preceding unsigned comment added by Emilgul (talk • contribs) 21:29, 19 September 2018 (UTC)

 * Yes some do. The best known is J0437-4715 which has a period of 0.005757451936712637 with an error of $1.7$. Jim77742 (talk) 00:17, 9 January 2019 (UTC)

Significant pulsars update
Since recent discovery the longest period neutron star pulsar isnt PSR J2144-3933 anymore but PSR J0250+5854 with a period of 23.5 s.

Source: http://iopscience.iop.org/article/10.3847/1538-4357/aade88/meta https://phys.org/news/2018-10-student-slowest-pulsar-star.html —SuperErten (talk) 21:29, 23 October 2018 (UTC)

PSR J0002+6216
Attracting much press attention. Jim.henderson (talk) 02:21, 26 March 2019 (UTC)

spider stars
Currently, spider stars are not described in Wikipedia. However, this seems just a proposed name as I found it in the following preprint:
 * Deneva et al.: Timing of Eight Binary Millisecond Pulsars Found with Arecibo in Fermi-LAT Unidentified Sources (2021-01-01)
 * Rafi Letzter: Now-dead radio telescope finds bizarre venomous-spider star. On: LiveScience. 2021-01-18

The article uses also further designations: black widow (special kind of spider star), redback systems, ...

Maybe worth to mention in the article? --Ernsts (talk) 18:50, 19 January 2021 (UTC)

Wiki Education Foundation-supported course assignment
This article is or was the subject of a Wiki Education Foundation-supported course assignment. Further details are available on the course page. Student editor(s): VinnyPizz.

Above undated message substituted from Template:Dashboard.wikiedu.org assignment by PrimeBOT (talk) 07:30, 17 January 2022 (UTC)

A new ultra-long period pulsar with low duty cycle
"PSR J0901-4046" Discovery of a radio-emitting neutron star with an ultra-long spin period of 76s with unusual spin properties. Notable ? - Rod57 (talk) 13:31, 31 May 2022 (UTC)

The Pulsar 5G
The Pulsar is mentioned in the Iskamic Holly book Al-Quran. There are 113 Suras in the Quran each containes a certain number of verses and has it's own titke.. One of those Suras is titled The Pulsar and starts with the verse" The Pulsar and you woulden't know what is the Pulsar. IT is the piercing star" 108.7.231.165 (talk) 00:43, 3 July 2024 (UTC)

license: Creative Commons - Attribution Share-Alike - https://creativecommons.org/licenses/by-sa/4.0/

title: Talk:Pulsar


text: Category:Nepalese mountain climbers

title: Category:Nepalese mountain climbers


text:
Talk:Eugene Onegin (opera)

{{Ticket confirmation|id=2005110510001389|source=opera japnica|license=gfdl|note=(Permission was granted for GFDL only, but content is dually licensed following the license migration of June 2009.}}}

Pronunciation of Onegin
Does anybody know how to pronounce "Onegin"? I've heard OWN-a-gin (hard 'g') and "AWN-a-gin" (soft 'g') and everything in between. If the stress is capable of being moved--"o-NEE-gin"--the possibilities are endless. Thanks.

 * The one I have heard most often is o-NYAY-gin (hard g), but I don't know if it is right--only commonly used (for instance, by the announcers on the Metropolitan Opera broadcasts) Antandrus 18:28, 30 Nov 2004 (UTC]

 * The way it's pronounced in Russian is close to o-nE-gin (G as in 'goose').

S0lnishk0

 * I'm just guessing that in User:S0lnishk0's "o-nE-gin" that "nE" is meant to represent something like a general European é sound, or perhaps a shorter e such as in Spanish, rather than how an English speaker would interpret "NEE" - so that would make it close to "NAY". It wouldn't surprise me if there's something like an ñ sound in there, as suggested by Antandrus's "NYAY", but I really have no idea. Milkunderwood (talk) 08:25, 6 February 2013 (UTC)

Translation
Can anyone translate what was just added by S0lnishk0? I don't think we should have the article written in Russian. --BaronLarf 16:29, Apr 2, 2005 (UTC)

 * I just listed this on Pages needing translation into English. There are several fluent Russian-speakers who are regular (contributors here (alas, I'm not one of them!)  Antandrus 17:30, 2 Apr 2005 (UTC)

The title Eugene Onegin
We have some inconsistencies here - Lensky and Lenski for example.

It seems out of date to be still calling the opera Eugene Onegin. The New Grove Dictionary of Opera - the best authority for opera - gives Yevgeny Onegin. It also gives Tat'yana, Ol'ga, Filipp'yevna, and Lensky.

(Please note that I don't have Russian!) Kleinzach 17:09, 3 December 2005 (UTC)

 * It's my general impression that the "y" form (Lensky) tends to be the usual Russian transliteration, while the "i" form (Lenski) is Polish. I'd guess that these names are taken from liner notes or CD booklets to recordings, which are always unreliable as sources. As to moving the article to Yevgeny Onegin, I'd be all for it, but don't have the energy to get into another title argument. Milkunderwood (talk) 05:59, 6 February 2013 (UTC)

German pronunciation of Eugene
Even though the opera was never, to my knowledge, regularly performed in German in English-speaking countries, it was for a very long time referred to as "Eugen Onegin" - with the German pronunciation that sounds like "oygen". I still occasionally hear radio broadcasters using that pronunciation, even though whenever it's performed here, it's either in English or Russian, never German. Has anyone else encountered this, and is there a case for mentioning this in the article? -- JackofOz (talk) 05:24, 2 February 2008 (UTC)

Nabokov
"world-weary St Petersburg 'drawing-room automaton' (Nabokov)" Can someone explain the meaning of the  "(Nabokov)" ? Diggers2004 (talk) 08:24, 10 May 2012 (UTC)
 * User:Kleinzach posted this in 2005. Vladimir Nabokov translated Pushkin's Eugene Onegin into English verse, and in his Introduction to the book described Onegin, using the exact phrase "drawing-room automaton". "World-weary" appears to be Kleinzach's phrasing from Nabokov's more extensive discussion of the character. I do not have this book, and can't give a reference, but the phrase is searchable in Google Books. Milkunderwood (talk) 05:31, 6 February 2013 (UTC)

Synopsis
I'd suggest reworking the synopsis as it's been taken directly from the Opera Japonica site (which is no longer accessible). Please let me know if there'd be any objections. Thanks, OperaBalletRose (talk) 11:21, 14 September 2012 (UTC)
 * User:Kleinzach specifically stated in his adding the synopsis "[This synopsis by Simon Holledge was first published on Opera japonica http://www.operajaponica.org and appears here by permission.]" It's my understanding that Kleinzach was associated with the Opera Japonica website, and may have been a major contributor himself. I don't see any need for his synopsis to be rewritten now. Milkunderwood (talk) 05:49, 6 February 2013 (UTC)
 * Thanks for your feedback on this. I was referred by User:Voceditenore to this discussion about the Opera Japonica synopses. Following this, I expanded the synopsis here so that it's more detailed, and amended the footnote so that it now states 'Parts of this synopsis were first published on Opera japonica'. OperaBalletRose (talk) 11:22, 6 February 2013 (UTC)

Bad phrase
"The libretto was written by Konstantin Shilovsky and the composer and his brother Modest" isn't a well-written or clear phrase. Did all three write the libretto? If so, why two "and"'s? beej (talk) 15:38, 26 November 2012 (UTC)
 * No, they didn't. Tchaikovsky, together with Shilovsky, made as much use of the words of Pushkin's verse novel as they could.  The only additional major contributions to the libretto are a) Shilovsky's verses for M. Triquet and b) Tchaikovsky's for Lensky's arioso in the first scene of the opera, plus Prince Gremin's aria in the first scene of Act 3.  Modest Tchaikovsky wasn't involved at all in this opera, though he wrote the libretto of Iolanta and collaborated with his brother on The Queen of Spades.  I'll make some changes to the article based on the above (and with a reference). --GuillaumeTell 17:51, 26 November 2012 (UTC)
 * Fixed - comments welcome. Article could be improved. --GuillaumeTell 18:29, 26 November 2012 (UTC)

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title: Talk:Eugene Onegin (opera)


text:
Tommy Bond

Thomas Ross Bond (September 16, 1926 – September 24, 2005) was an American actor, director, producer and writer. He was best known for his work as a child actor for two nonconsecutive periods in Our Gang (Little Rascals) comedies (first as "Tommy" and later as "Butch"). Also, he is noted for being the first actor to appear onscreen as DC Comics character Jimmy Olsen, in the film serials Superman (1948) and Atom Man vs. Superman (1950).

Early years and Our Gang
Born in Dallas, Texas, Bond got his start in 1931 at the age of 4 when a talent scout for Hal Roach studios approached him as he was leaving a Dallas cinema.

Bond was hired at Hal Roach Studios for the Our Gang series in the summer of 1931 to begin work that upcoming fall, at around the same time as George "Spanky" McFarland was hired. Bond worked in Our Gang for three years, alternately appearing as a supporting character and a background actor. His speaking roles increased by 1934, including his most substantive role up to that point, as the gang's band conductor in Mike Fright. In late 1934, Bond left the series and returned to public school, still earning periodic bit parts in Hollywood productions. After leaving the gang for the first time, Bond also worked as a voice actor, most notably in several of Tex Avery's Merrie Melodies cartoons for Warner Bros. His best known voice role was as the speaking voice of "Owl Jolson" in Tex Avery's 1936 Merrie Melodies cartoon, I Love to Singa.

Bond returned to Our Gang on a recurring basis late in 1936, when Roach hired him to play "Butch", the neighborhood bully. In the film Practical Jokers, his mother calls him "Tommy", apparently indicating that "Butch" was a nickname. Bond's first short as Butch was Glove Taps. Besides filling the role of the archetypal Our Gang bully, the Butch character also regularly competed with meek Alfalfa (Carl Switzer) for the affections of his sweetheart Darla (Darla Hood). While in Our Gang, Bond appeared in a number of outside films, such as those featuring fellow Hal Roach Studios comedians Charley Chase and Laurel and Hardy.

By the late 1930s Bond was so established as a juvenile actor that other studios recruited him for feature films. He was a regular in Columbia's Five Little Peppers series of children's stories in 1939-40. He also appeared opposite singing star Gloria Jean in Universal's A Little Bit of Heaven (1940).

When the Our Gang series moved to Metro-Goldwyn-Mayer in 1938, Bond remained with the group. His final Our Gang short was Bubbling Troubles (1940). Bond continued to work in other MGM productions following his departure from Our Gang. In total, Bond appeared in 27 Our Gang shorts – 13 as "Tommy" and 14 as "Butch".

Later years
After serving in the U.S. Navy during World War II, Bond returned to acting, and appeared in two Gas House Kids features alongside former on-screen rival Carl Switzer. In the late 1940s, Bond became the first actor to portray cub reporter Jimmy Olsen in two Superman film serials: Superman (1948) and Atom Man vs. Superman (1950).

In 1951, Bond graduated from college and quit acting, but remained in show business in the areas of television directing and production, and worked with individuals such as Norman Lear, George Schlatter, and many others. He worked at KTTV in Los Angeles from the 1950s to the early 1970s. He then went to work for KFSN in Fresno from the early 1970s to 1991. Bond also worked as a production manager on Rowan & Martin's Laugh-In.

During the 1960s, Bond was an active member of Emmanuel Lutheran Church in North Hollywood where a number of his Hollywood friends and colleagues attended. Together, they were instrumental in the production and presentation of the annual Christmas Pageant presented on the grounds of Emmanuel's school Laurel Hall. The production, which involved a cast of several hundred, a chariot and horses, numerous other animals and professional Hollywood sets and lighting, was presented each year during the Christmas season for several weeks leading up to Christmas. Grandstand-style bleachers were installed that seated about 1000 guests. Highlights of the pageant included a horse-driven chariot and Roman soldiers on horseback riding through the gates of Bethlehem to proclaim the census requiring Jews to register in their hometowns. Bond was instrumental in arranging for the production to be filmed and aired on Metromedia-owned Channel 11, KTTV in about 1965.

In 1972, he appeared as a guest on I've Got a Secret while working as a production assistant on the show. Bond retired from television in 1991. In his latter years he lived in the Fresno and Madera Ranchos area, and served as a spokesman for a number of Our Gang-related materials. Bond published his autobiography, Darn Right It's Butch: Memories of Our Gang/The Little Rascals, with the help of Fresno teacher, film historian and co-author Ron Genini, in 1994. Tommy's son, Thomas R. Bond II "Butch, Jr.", who is a film and television producer, worked with his father in their family production company, Biograph Company. The senior Bond also hosted The Rascals, a documentary on the life and times of the Little Rascals.

Throughout his lifetime, Bond appeared in 73 films, was a charter member of the Screen Actors Guild, joining in 1937, and worked with many Hollywood stars in the years of 1933 to 1951, including James Stewart, Eleanor Powell, Ray Bolger, Frank Morgan, and Eddie Cantor among many others.

Death
Bond died on September 24, 2005, at age 79 due to complications from heart disease in Northridge, California. He is buried at U.S. Veterans Riverside National Cemetery in Riverside, California.

Books

 * Bond, Tommy, w. Genini, Ron (1994). Darn Right It's Butch: Memories of Our Gang/The Little Rascals. Delaware: Morgan Press. ISBN 0-9630976-5-2.

title: Tommy Bond


text:
Percy Hansen

Brigadier Percy Howard Hansen, (26 October 1890 – 12 February 1951) was a British Army officer and recipient of the Victoria Cross (VC), the highest award for gallantry in the face of the enemy that can be awarded to personnel of the British and Commonwealth forces.

Early life
Hansen was born into a wealthy and well-connected Danish family that settled first in South Africa then, after 1900, in London. He was educated at preparatory schools in Hazelwood, Limpsfield, Surrey and Oxted, Surrey; then at Eton College (from 20 September 1904). His father, Viggo Julius Hansen, was naturalised as a British subject in 1910, so that his son could join the British Army.

Military career
After officer training at the Royal Military College, Sandhurst, Hansen was commissioned into the Lincolnshire Regiment on 4 March 1911.

First World War
Hansen was appointed as a temporary captain shortly after the outbreak of war in 1914, as adjutant in the 6th (Service) Battalion of the Lincolnshire Regiment, and his promotion was made permanent in the following April. He fought with his battalion, a recently created Kitchener's Army unit composed of civilian volunteers, during the Gallipoli campaign in the summer of 1915. On 9 August 1915 at Yilghin Bumu, Hansen's battalion was forced to withdraw while assaulting Scimitar Hill. Hansen and volunteers repeatedly moved back and forth under heavy fire to successfully rescue six wounded men from capture, or death by burning. Hansen was consequently awarded the Victoria Cross.

A month later, Hansen won the Military Cross for performing a reconnaissance mission at Suvla Bay. On the night of 9 September 1915, he carried out a solo reconnaissance of the coast, carrying only a revolver and a blanket for disguise. He successfully located an important Turkish firing position.

Due to ill-health, Hansen was eventually transferred to France and appointed brigade major to the 170th (2/1st North Lancashire) Brigade. He remained a staff officer for the rest of the war, during which he served with the II Anzac Corps. He was made a Companion of the Distinguished Service Order (DSO) for another daring reconnaissance mission during the Battle of Passchendaele in 1917.

Between the wars
Remaining in the army after the war, Hansen attended the Staff College, Camberley and, for most of the interwar period, served in numerous staff positions. After graduating, he then served as a brigade major with the 8th Infantry Brigade, part of the 3rd Infantry Division, then serving in Southern Command, before becoming a brigade major with the 4th Infantry Division's 12th Infantry Brigade. His next assignment was as a General Staff Officer Grade 2 (GSO2) to the 55th (West Lancashire) Division, a Territorial Army (TA) formation, and then a GSO2 in Jamaica, before returning to the United Kingdom and being made Deputy Assistant Adjutant-General (DAAG) with Western Command. He was then posted to the 2nd Battalion, Lincolnshire Regiment, initially as the battalion's second-in-command. The battalion was serving in Palestine, then the scene of an Arab revolt. The battalion was in Palestine for five months before it was sent back to England, and in September 1937 Hansen became the Commanding Officer (CO). He continued to command of the battalion until the outbreak of the Second World War in September 1939.

Second World War
On 2 September 1939, the day before the war began, Hansen was posted to the 55th (West Lancashire) Infantry Division, a TA formation which he had served with before, and was made Assistant Adjutant-General & Quartermaster-General (AA&QMG). He held this post until late January 1941, when he became Deputy Assistant & Quartermaster-General (DA&QMG) with XII Corps, then commanded by Lieutenant General Andrew Thorne. The corps, which was commanded from late April by Lieutenant General Bernard Montgomery, had responsibility for the defence of Kent in the event of a German invasion of the United Kingdom.

Hansen continued in this role until February 1942 when he was made an Area Commander of Belfast Area, before being made a Sub-District Commander, Ashford Area until serving on the staff of Supreme Headquarters Allied Expeditionary Force (SHAEF). He remained in this position until the war's end in 1945, and he retired from the army in January 1946.

Hansen died on 12 February 1951, at the relatively young age of sixty. He is one of only fourteen men, other than Gurkhas born in Nepal, not born as a British subject to have received the Victoria Cross.

Awards and decorations

 * Victoria Cross (1 October 1915) "For most conspicuous bravery on 9th August, 1915, at Yilghin Burnu, Gallipoli Peninsula. After the second capture of the "Green Knoll" his Battalion was forced to retire, leaving some wounded behind, owing to the intense heat from the scrub which had been set on fire. When the retirement was effected Captain Hansen, with three or four volunteers, on his own initiative, dashed forward several times some 300 to 400 yards over open ground into the scrub under a terrific fire, and succeeded in rescuing from inevitable death by burning, no less than six wounded men."
 * Distinguished Service Order (16 September 1918) "For conspicuous gallantry and devotion to duty. He volunteered to carry out a reconnaissance, and brought back valuable information obtained under heavy artillery and machine-gun fire, which had been unprocurable from other sources. Throughout he did fine work."
 * Military Cross (29 October 1915) "For conspicuous gallantry at Suvla Bay on 9th September, 1915. He made a reconnaissance of the coast, stripping himself and carrying only a revolver and a blanket for disguise. He swam and scrambled over rocks, which severely cut and bruised him, and obtained some valuable information and located a gun which was causing much damage. The undertaking was hazardous. On one occasion he met a patrol of 12 Turks who did not see him, and later a single Turk whom he lulled. He returned to our lines in a state of great exhaustion."
 * Mentioned in dispatches five times
 * Croix de Guerre with Bronze Star (France)
 * Officer of the Legion of Merit (14 November 1947, United States)
 * Commander of the Royal Order of St Olav (Norway)

Birthplace and place of death controversy
There is disagreement concerning the places of Hansen's birth and death. Some sources state that he was born in Durban, South Africa; another says "Dresden, Germany (where his parents were taking a cure)". Similarly, one source gives his place of death as "Kensington, London", and subsequent burial at Garrison Cemetery, Copenhagen, while another says he died in Copenhagen.

The Danish "folketælling 1895" (cencus) have him writen in the papers when he was 4 years old. His birthplace is "Dresden". His mom "Else Hansen" and his father "Viggo Hansen" is born in Copenhagen. His farther had a grocery store. Their house was on "Kongens Nytorv" (matrikel 34). (reference: Folketælling 1895, hovedliste, løbenummer 353, familie nr 98)

title: Percy Hansen


text:
List of automobile races in Italy

Grand Prix and other major automobile races in Italy.
 * 10 Hours of Messina
 * Adriana Grand Prix
 * Alessandria Grand Prix
 * Bari Grand Prix
 * Circuito di Avellino
 * Circuito del Garda
 * Coppa Acerbo
 * Pescara Grand Prix
 * Coppa Ciano
 * Coppa della Toscana
 * Coppa Florio
 * Coppa d'Oro di Sicilia
 * Coppa d'Oro delle Dolomiti
 * Giro di Sicilia automobilistico
 * Giro d'Italia automobilistico
 * International Rally of Messina
 * Monza Circuit
 * Grand Prix of Italy
 * Grand Prix of Modena
 * Grand Prix of Naples
 * Grand Prix of Rome
 * Grand Prix of Turin
 * Mediterranean Grand Prix
 * Messina Grand Prix
 * Milan Grand Prix
 * Mille Miglia
 * Mugello Circuit
 * Grand Prix of Mugello
 * Rally d'Italia
 * Rally di Sanremo (1970–2003)
 * Rally di Sardegna (2004–2018)
 * Sardegna Rally Race
 * Imola Circuit
 * San Marino Grand Prix
 * San Remo Grand Prix
 * Syracuse Grand Prix
 * Targa Florio

title: List of automobile races in Italy


text:
Lewis Halliday

General Sir Lewis Stratford Tollemache Halliday, (14 May 1870 – 9 March 1966) was an English Royal Marine officer and a recipient of the Victoria Cross, the highest award for gallantry in the face of the enemy that can be awarded to British and Commonwealth forces.

Early life
Halliday was born in Medstead, Hampshire on 14 May 1870. He was commissioned into the Royal Marines in 1889.

Victoria Cross
Halliday was 30 years old, and a captain in the Royal Marine Light Infantry, during the Boxer Rebellion in China when the following deed took place for which he was awarded the VC.

On 24 June 1900 at Peking, China, an attack was made on the British Legation by the Boxers who set fire to the stables and occupied some of the other buildings. It being imperative to drive the enemy out, a hole was knocked in the Legation wall and 20 men of the RMLI went in. Captain Halliday, leading a party of six men, was involved in desperate fighting and was severely wounded but despite his injuries, he killed four of the enemy. Finally, unable to carry on any further, he ordered his men to go on without him, after which he returned to the legation alone, telling his men 'carry on and not mind him', so as not to diminish the number of men engaged in the sortie. He walked 100 yards unaided to the hospital although his shoulder was half blown out and his left lung punctured.

His citation reads: "Captain (now Brevet Major) Lewis Stratford Tollemache Halliday, Royal Marine Light Infantry

On the 24th June, 1900, the enemy, consisting of Boxers and Imperial troops, made a fierce attack on the west wall of the British Legation, setting fire to the West Gate of the south stable quarters, and taking cover in the buildings which adjoined the wall. The fire, which spread to part of the stables, and through which and the smoke a galling fire was kept up by the Imperial troops, was with difficulty extinguished, and as the presence of the enemy in the adjoining buildings was a grave danger to the Legation, a sortie was organised to drive them out. A hole was made in the Legation Wall, and Captain Halliday, in command of twenty Marines, led the way into the buildings and almost immediately engaged a party of the enemy. Before he could use his revolver, however, he was shot through the left shoulder, at point blank range, the bullet fracturing the shoulder and carrying away part of the lung. Notwithstanding the extremely severe nature of his wound, Captain Halliday killed three of his assailants, and telling his men to 'carry on and not mind him,' walked back unaided to the hospital, refusing escort and aid so as not to diminish the number of men engaged in the sortie."

He was promoted to brevet major for his part in the legation's defence, and returned to the United Kingdom to receive the VC from King Edward VII during an investiture at Marlborough House on 25 July 1901.

Later service
Having recovered from his wound he returned to duty at the end of 1901. He commanded the Marine detachment aboard HMS Galatea (1887), and then commanded the Marines aboard HMS Empress of India, the flagship of the home fleet, from late 1902. In 1907 having completed staff college at Camberley, he was appointed staff officer to the Portsmouth Division of his corps. He then commanded a company of Gentleman Officer Cadets at the Royal Military College, Sandhurst for four years during which time he was promoted to major. Among his cadets was the future Field Marshal Earl Alexander of Tunis. In early 1915 he was promoted to brevet lieutenant colonel and on 14 July of that year he was made lieutenant colonel. In November 1915 he joined GHQ, Home Forces as General Staff Officer. He was appointed colonel second Commandant of the Royal Marine Light Infantry in 1920 and colonel commandant on 1 January 1923. Halliday was promoted to major general on 11 December 1925, to lieutenant general on 11 June 1927 and to general on 1 October 1928. He served as ADC to King George V in 1924 and 1925, and he held the post of Adjutant-General Royal Marines from December 1927 until his voluntary retirement in June 1930. He was invested as a Companion of the Order of the Bath on 3 June 1913, he was elevated as a Knight Commander of the Order of the Bath on 1 January 1930.

The medal
His Victoria Cross is displayed at the Royal Marines Museum in Southsea, England.

title: Lewis Halliday


text:
Howard Levy

Howard Levy (born July 31, 1951) is an American multi-instrumentalist. A keyboardist and virtuoso harmonica player, Levy "has been realistically presented as one of the most important and radical harmonica innovators of the twentieth century."

In 1988, Levy was a founding member of Béla Fleck and the Flecktones, with whom he won a 1997 Grammy Award for Best Pop Instrumental Performance for the song "The Sinister Minister". He also won a Grammy for Best Instrumental Composition in 2012 for "Life in Eleven", a song written with Béla Fleck for the Flecktones' album Rocket Science (2011). He has worked with Arab-fusion musician Rabih Abou-Khalil, Latin jazz saxophonist Paquito D'Rivera, Donald Fagen, and Paul Simon.

Music career
Levy was born in Brooklyn, New York, and attended the Manhattan School of Music, where he studied piano and pipe organ. For two years, he went to Northwestern University in Evanston, Illinois, and participated in the jazz band. He is the Harmonica Lessons instructor for ArtistWorks.

Harmonica innovator
Levy plays in many genres: jazz, classical, rock, folk, Latin, blues, country, and world music. He drew attention for his chromatic playing style on a regular diatonic harmonica. He discovered the overblow and overdraw techniques for chromatic playing in 1970. These allow a harmonica player to obtain all the missing chromatic notes in the Richter-tuned diatonic harmonica.

In 1995, he performed the "Harmonia Mundi Suite for Harmonica and Chamber Ensemble" in Chicago. He composed a concerto for harmonica in 2001 and performed it with orchestras in the U.S. and Europe.

Forming groups
In 1988, Levy co-founded Béla Fleck and the Flecktones. He won a Grammy for Pop Instrumental for the song "The Sinister Minister". He left the band in 1992. Levy toured with Kenny Loggins and appeared on his album Outside from the Redwoods. Levy returned to the Flecktones in 2011, touring and recording the album Rocket Science (2011).

In the 1990s Levy founded Trio Globo with Eugene Friesen and Glen Velez. He leads another band, Acoustic Express and is music director of the Latin jazz group Chévere de Chicago.

He is the founder of Balkan Samba Records. The roster includes Chévere de Chicago, Alberto Mizrahi and Trio Globo, Fox Fehling, and Norman Savitt.

Touring and recording with others
Levy has toured or recorded with Kenny Loggins, John Prine, Ben Sidran, Bob Gibson, Bobby McFerrin, Bryan Bowers, Chris Siebold, Chuck Mangione, Claudio Roditi, David Bromberg, Styx, Dennis DeYoung, Dolly Parton, Donald Fagen, Holly Cole, Jerry Butler, Mark Nauseef, Miroslav Tadic, Paquito D'Rivera, Pete Seeger, Steve Goodman, Terry Callier, and Tom Paxton.

Gear
Levy favors an equal temperament tuning and plays harmonicas customized by Joe Filisko.

Awards and honors

 * Joseph Jefferson Award, Best Original Music for a Play (1986)
 * Grammy Award for Best Pop Instrumental, "The Sinister Minister", Béla Fleck and the Flecktones (1997)
 * Grammy Award for Best Instrumental Composition, "Life in Eleven" (2012)

Discography
As leader or co-leader
 * Carnival of Souls (Silver Wave, 1995)
 * The Old Country (M.A., 1996)
 * The Stranger's Hand (Tone Center, 1999) with Jerry Goodman, Oteil Burbridge, and Steve Smith
 * Cappuccino with Fox Fehling (Balkan Samba, 2004)
 * Secret Dream (Balkan Samba, 2005)
 * Howard Levy & Paul Sprawl (Balkan Samba, 2005)
 * Time Capsules (Balkan Samba, 2009)
 * Tonight and Tomorrow (CD Baby/Chicago Sessions, 2009)
 * Silver & Black (Enja, 2009)
 * Concerto for Diatonic Harmonica & Orchestra (Balkan Samba, 2010)
 * Alone and Together (Balkan Samba, 2010)
 * Steering by the Stars (Stonecutter, 2010)
 * Out of the Box (Balkan Samba, 2012)
 * Matzah to Menorah (Balkan Samba, 2012)
 * First Takes (Balkan Samba, 2014)
 * Tango and Jazz (Balkan Samba, 2016)
 * Art + Adrenaline with Chris Siebold (Balkan Samba, 2018)

With Béla Fleck and the Flecktones
 * Béla Fleck and the Flecktones (1990)
 * Flight of the Cosmic Hippo (1991)
 * UFO Tofu (1992)
 * Live Art (1996)
 * Rocket Science (2011)

With Rabih Abou-Khalil With Samo Salamon
 * The Sultan's Picnic (Enja, 1994)
 * Odd Times (Enja, 1997)
 * Peaks of Light (Samo Records, 2018)

title: Howard Levy


text:
Illinois Service

The Illinois Service, branded Amtrak Illinois, comprises three passenger rail routes operated by Amtrak in the American state of Illinois. The Illinois Service is funded primarily by the Illinois Department of Transportation (IDOT) and falls under the broader Amtrak Midwest brand.

Chicago is a terminus for all three Illinois Service routes, which all have multiple daily round trips:
 * Chicago–Quincy: two round trips daily, the Illinois Zephyr and the Carl Sandburg
 * Chicago–St. Louis Lincoln Service: four round trips daily and the only route that serves another state
 * Chicago–Carbondale: two round trips daily, the Illini and the Saluki, and the only route whose trains have checked baggage service

Proposed expansion
Two proposed Illinois Service routes have been accepted by the Corridor Identification and Development Program, both in December 2023:
 * Chicago–Peoria Prairie Marksman via Joliet, Morris, Ottawa, and LaSalle-Peru
 * Chicago–Moline Quad Cities: uses the existing Chicago–Quincy route between Chicago and Princeton, branching from it west of Wyanet to serve the Quad Cities via Geneseo

The Quad Cities and the Rockford-Chicago portion of the Black Hawk were to have been added in late 2015 but were put on hold by then-Governor Bruce Rauner. They were resurrected and funded in 2019 as part of a transportation bill supported by Governor J.B. Pritzker. In 2023, Pritzker announced that the Rockford-Chicago train will be operated by Metra.

In addition to the two new routes, a committee was formed in late 2021 to study and promote extending the Chicago–Quincy route to Hannibal, Missouri.

title: Illinois Service


text:
Talk:Chetwode

The Manor in Chetwode has been occupied by the Collins Family since (I believe) the 1950's when they lived at the Grange in Chetwode. --Daedelus 18:29, 30 Nov 2004 (UTC)

 * How did they come into possession of the manor? If it was through inheritance that statement in the article is still correct. -- Graham  ☺ | Talk 20:58, 30 Nov 2004 (UTC)

Mr JEH Collins moved to Chetwode Manor in the 1980s. He married the current owner of the house who has no relation to the Chetwode family. The manor was sold in the 1960s.

Chetwode Family
How could there be an article on Chetwode without mentioning the Chetwode Family. John de Chetwode, Lord of Chetwode founded the Priory of Chetwood when? That's why I looked this up. The manor "belonged to a Chetwode before the Conquest" is the best I can find elsewhere.Dangnad (talk) 01:14, 29 July 2011 (UTC)
 * Well the answer is very simple. Wikipedia is an encyclopaedic project compiled by editors. Nothing would exist without the efforts of these users. No one has got around to the Chetwodes as they have been busy elsewhere in the project so why not join in and have a go at compiling the information on the Chetwodes yourself.Tmol42 (talk) 01:34, 29 July 2011 (UTC)
 * You might find it useful to add info to this page also Baron ChetwodeTmol42 (talk) 01:38, 29 July 2011 (UTC)

According to an article in the first issue of Records of Buckinghamshire, a publication of the Buckinghamshire Archaeological Society -- a PDF of the article is available online here: http://www.bucksas.org.uk/rob/rob_1_6_206.pdf -- "Sir J.N.L. Chetwode" had records relating to the Manor House and the history of the village. He was undoubtedly Sir John Newdigate-Ludford-Chetwode, 5th Baronet (1788–1873). So the house was still in the family at that time. Although it has been mentioned in the Talk section that the Manor House was sold "in the 1960s", I suspect that it may have been more likely to have been sold shortly after the death of the 1st Baron Chetwode in 1950 to pay death duties. This would require further investigation. — Preceding unsigned comment added by 69.47.167.219 (talk) 15:30, 26 October 2014 (UTC)

title: Talk:Chetwode