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In astronomy, a glitch is a sudden small increase of around 1 part in 1 million in the rotational frequency of a pulsar, which usually decreases steadily due to braking provided by the emission of radiation and high-energy particles. It is not known whether glitches are related to the timing noise which all pulsars exhibit. Following a glitch is a period of gradual recovery where the observed periodicity slows to a period close to that observed before the glitch. These gradual recovery periods have been observed to last from days to years. As of 2024^[update] only multiple glitches of the Crab and Vela pulsars have been observed and studied extensively.

Cause

While the exact cause of glitches is unknown, they are thought to be caused by an internal process within the pulsar. This differs from the steady decrease in the pulsar's rotational frequency, which is caused by external processes. Although the details of the glitch process are unknown, it is thought that the resulting increase in the pulsar's rotational frequency is caused by a brief coupling of the pulsar's faster-spinning superfluid core to the crust, to which it is usually not coupled. This brief coupling transfers angular momentum from core to surface, which causes a decrease in the measured period.^[1]

Implications

If the mechanism is as suggested above, observed pulsar glitches set a limit on the moment of inertia of the pulsar being observed and, thus, the mass-radius relation possible in dense nuclear matter. More generally, observations of pulsar glitches allow indirect information on the dense nuclear matter in neutron star interiors to be inferred, in particular its superfluid properties.^[1]

References

^ ^a ^b Antonelli, Marco; Montoli, Alessandro; Pizzochero, Pierre (November 2022), "Insights into the Physics of Neutron Star Interiors from Pulsar Glitches", Astrophysics in the XXI Century with Compact Stars, pp. 219–281, arXiv:2301.12769, doi:10.1142/9789811220944_0007, ISBN 978-981-12-2093-7, S2CID 256390487

Link, Bennett; Epstein, Richard I.; Van Riper, Kenneth A. (1992). "Pulsar glitches as probes of neutron star interiors". Nature. 359 (6396): 616–618. Bibcode:1992Natur.359..616L. doi:10.1038/359616a0. S2CID 4346989.
https://web.archive.org/web/20051018233130/http://www.saao.ac.za/~wgssa/as4/urama.html http://www.saao.ac.za/~wgssa/as4/urama.html
Rowan, L. (2000). "ASTRONOMY: Pulsar Glitches". Science. 289 (5476): 13c–13. doi:10.1126/science.289.5476.13c. S2CID 122316928.

[:0-1] Antonelli, Marco; Montoli, Alessandro; Pizzochero, Pierre (November 2022), "Insights into the Physics of Neutron Star Interiors from Pulsar Glitches", Astrophysics in the XXI Century with Compact Stars, pp. 219–281, arXiv:2301.12769, doi:10.1142/9789811220944_0007, ISBN 978-981-12-2093-7, S2CID 256390487

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-{{expand|date=February 2008}}
+{{more citations needed|date=March 2016}}
-A '''glitch''' is a sudden increase (up to 1 part in 10<sup>6</sup>) in the rotational [[frequency]] of a [[rotation-powered pulsar]], which usually decreases steadily due to braking provided by the emission of radiation and high-energy particles.  It is unknown whether or not they are related to the [[timing noise]] which all pulsars exhibit.  Following a glitch is a period of gradual recovery where the observed [[periodicity]] slows to a period close to that observed before the glitch.  These gradual recovery periods have been observed to last from days to years.  Currently, only multiple glitches of the [[Crab Pulsar|Crab]] and [[Vela Pulsar|Vela]] pulsars have been observed and studied extensively
+In [[astronomy]], a '''glitch''' is a sudden small increase of around 1 part in 1 million in the rotational [[frequency]] of a [[pulsar]], which usually decreases steadily due to braking provided by the emission of radiation and high-energy particles.  It is not known whether glitches are related to the [[timing noise]] which all pulsars exhibit.  Following a glitch is a period of gradual recovery where the observed [[Frequency|periodicity]] slows to a period close to that observed before the glitch.  These gradual recovery periods have been observed to last from days to years. {{As of|2024}} only multiple glitches of the [[Crab Pulsar|Crab]] and [[Vela Pulsar|Vela]] pulsars have been observed and studied extensively.
 == Cause ==
-While the exact cause of glitches is unknown, they are thought to be caused by an internal process within the pulsar.  This differs from the steady decrease in the star's rotational frequency which is caused by external processes.  Although the details of the glitch process are unknown, it is thought that the resulting increase in the pulsar's rotational frequency is caused by a brief coupling of the the pulsar's faster-spinning [[superfluid]] core to the crust, which are usually decoupled.  This brief coupling transfers angular momentum from core to the surface, which causes an increase in the measured periodicity.  It is thought that the coupling could be caused by a breaking of the pulsar's magnetic dipole, which would apply a torque to the crust causing a brief coupling between the two parts.
+While the exact cause of glitches is unknown, they are thought to be caused by an internal process within the pulsar.  This differs from the steady decrease in the pulsar's rotational frequency, which is caused by external processes.  Although the details of the glitch process are unknown, it is thought that the resulting increase in the pulsar's rotational frequency is caused by a brief coupling of the pulsar's faster-spinning [[superfluid]] core to the crust, to which it is usually not coupled.  This brief coupling transfers angular momentum from core to surface, which causes a decrease in the measured period.<ref name=":0">{{Citation |last1=Antonelli |first1=Marco |title=Astrophysics in the XXI Century with Compact Stars |date=November 2022 |pages=219–281 |arxiv=2301.12769 |last2=Montoli |first2=Alessandro |last3=Pizzochero |first3=Pierre|chapter=Insights into the Physics of Neutron Star Interiors from Pulsar Glitches |doi=10.1142/9789811220944_0007 |isbn=978-981-12-2093-7 |s2cid=256390487 }}</ref>
-== References ==
+==Implications==
-* http://www.nature.com/nature/journal/v359/n6396/abs/359616a0.html
-* http://www.saao.ac.za/~wgssa/as4/urama.html
-* http://www.sciencemag.org/cgi/content/summary/289/5476/13c
+If the mechanism is as suggested above, observed pulsar glitches set a limit on the [[moment of inertia]] of the pulsar being observed and, thus, the mass-radius relation possible in dense nuclear matter. More generally, observations of pulsar glitches allow indirect information on the dense nuclear matter in neutron star interiors to be inferred, in particular its superfluid properties.<ref name=":0" />
-{{var-star-stub}}
-{{physics-stub}}
+== See also ==
+* [[Neutron star#Anti-glitches|Anti-glitch]]
+== References ==
+{{Reflist}}
+* {{Cite journal | doi=10.1038/359616a0| title=Pulsar glitches as probes of neutron star interiors| journal=Nature| volume=359| issue=6396| pages=616–618| year=1992| last1=Link| first1=Bennett| last2=Epstein| first2=Richard I.| last3=Van Riper| first3=Kenneth A.| bibcode=1992Natur.359..616L| s2cid=4346989}}
+* https://web.archive.org/web/20051018233130/http://www.saao.ac.za/~wgssa/as4/urama.html http://www.saao.ac.za/~wgssa/as4/urama.html
+* {{Cite journal | doi=10.1126/science.289.5476.13c| title=ASTRONOMY: Pulsar Glitches| journal=Science| volume=289| issue=5476| pages=13c–13| year=2000| last1=Rowan| first1=L.| s2cid=122316928}}
+{{Neutron star}}
-[[ru:Глитч (астрономия)]]
 [[Category:Rotation-powered pulsars]]

v t e Neutron star
Types	Radio-quiet Pulsar
Single pulsars	Magnetar Soft gamma repeater Anomalous X-ray Ultra-long period Rotating radio transient
Binary pulsars	Binary X-ray pulsar X-ray binary X-ray burster List Millisecond Be/X-ray Spin-up Hulse–Taylor pulsar
Properties	Blitzar Fast radio burst Bondi accretion Chandrasekhar limit Gamma-ray burst Glitch Neutron matter Neutron-star oscillation Optical Pulsar kick Quasi-periodic oscillation Relativistic Rp-process Starquake Timing noise Tolman–Oppenheimer–Volkoff limit Urca process
Related	Gamma-ray burst progenitors Asteroseismology Compact star Quark star Exotic star Supernova Supernova remnant Related links Hypernova Kilonova Microquasar Neutron star merger Quark-nova White dwarf Related links Stellar black hole Related links Radio star Pulsar planet Pulsar wind nebula Thorne–Żytkow object QCD matter
Discovery	LGM-1 Centaurus X-3 Timeline of white dwarfs, neutron stars, and supernovae
Satellite investigation	Rossi X-ray Timing Explorer Fermi Gamma-ray Space Telescope Compton Gamma Ray Observatory Chandra X-ray Observatory
Other	X-ray pulsar-based navigation The Magnificent Seven List of neutron stars Most massive neutron stars Neutron stars in fiction
Category Commons