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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
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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.
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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
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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.
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Antonelli, Marco; Montoli, Alessandro; Pizzochero, Pierre (November 2022), "Insights into the
Physics of Neutron Star Interiors from Pulsar Glitches",
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thought that the resulting increase in the pulsar's rotational frequency is caused by a brief coupling of the pulsar's faster-spinning
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Link, Bennett; Epstein, Richard I.; Van Riper, Kenneth A. (1992). "Pulsar glitches as probes of neutron star interiors".
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which all pulsars exhibit. Following a glitch is a period of gradual recovery where the observed
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If the mechanism is as suggested above, observed pulsar glitches set a limit on the
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is a sudden small increase of around 1 part in 10 in the rotational
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Timeline of white dwarfs, neutron stars, and supernovae
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pulsars have been observed and studied extensively.
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46:. Unsourced material may be challenged and removed.
210:Astrophysics in the XXI Century with Compact Stars
302:Rowan, L. (2000). "ASTRONOMY: Pulsar Glitches".
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297:http://www.saao.ac.za/~wgssa/as4/urama.html
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44:adding citations to reliable sources
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568:Tolman–Oppenheimer–Volkoff limit
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751:Fermi Gamma-ray Space Telescope
31:needs additional citations for
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777:X-ray pulsar-based navigation
756:Compton Gamma Ray Observatory
316:10.1126/science.289.5476.13c
746:Rossi X-ray Timing Explorer
589:Gamma-ray burst progenitors
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543:Quasi-periodic oscillation
228:10.1142/9789811220944_0007
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761:Chandra X-ray Observatory
841:Rotation-powered pulsars
528:Neutron-star oscillation
417:Rotating radio transient
55:"Glitch" astronomy
782:Tempo software program
792:The Magnificent Seven
697:Thorne–Żytkow object
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40:improve this article
648:Neutron star merger
508:Chandrasekhar limit
475:Hulse–Taylor pulsar
402:Soft gamma repeater
271:1992Natur.359..616L
692:Pulsar wind nebula
670:Stellar black hole
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411:Ultra-long period
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173:moment of inertia
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51:Find sources:
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29:This article
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599:Compact star
573:Urca process
563:Timing noise
548:Relativistic
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443:X-ray binary
438:X-ray pulsar
362:Neutron star
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167:Implications
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136:timing noise
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38:Please help
33:verification
30:
658:White dwarf
643:Microquasar
609:Exotic star
538:Pulsar kick
460:Millisecond
376:Radio-quiet
186:Anti-glitch
140:periodicity
787:Astropulse
702:QCD matter
682:Radio star
653:Quark-nova
604:Quark star
553:Rp-process
484:Properties
219:2301.12769
192:References
161:superfluid
96:March 2016
66:newspapers
737:Satellite
711:Discovery
633:Hypernova
616:Supernova
558:Starquake
324:122316928
246:256390487
128:frequency
120:astronomy
835:Category
810:Category
638:Kilonova
465:Be/X-ray
397:Magnetar
180:See also
820:Commons
582:Related
533:Optical
491:Blitzar
470:Spin-up
304:Science
287:4346989
267:Bibcode
80:scholar
518:Glitch
433:Binary
381:Pulsar
322:
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259:Nature
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132:pulsar
124:glitch
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770:Other
718:LGM-1
369:Types
320:S2CID
283:S2CID
242:S2CID
214:arXiv
154:Cause
130:of a
87:JSTOR
73:books
453:List
232:ISBN
148:Vela
146:and
144:Crab
122:, a
59:news
312:doi
308:289
275:doi
263:359
224:doi
118:In
42:by
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