Glitch

A glitch is a sudden increase (around 1 part in 106) 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 unknown whether 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 and Vela pulsars have been observed and studied extensively.

## Contents

* 1 Cause
* 2 Implications
* 3 See also
* 4 References

## 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 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 a decrease in the measured period.[1]

## Implications

Assuming that the mechanism described above is correct, 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 to extract indirect information on the dense nuclear matter in neutron star interiors, in particular its superfluid properties.[1]

## See also

* Anti-glitch

## References

1. ↑ 1.0 1.1 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, doi:10.1142/9789811220944_0007, ISBN 978-981-12-2093-7

* Link, Bennett; Epstein, Richard I.; Van Riper, Kenneth A. (1992). "Pulsar glitches as probes of neutron star interiors". Nature 359 (6396): 616–618. doi:10.1038/359616a0. Bibcode: 1992Natur.359..616L.
* 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.

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Neutron star

Types|

* Radio-quiet
* Pulsar

Single pulsars|

* Magnetar
* Soft gamma repeater
* Anomalous X-ray
* Rotating radio transient

Binary pulsars|

* Binary
* X-ray pulsar
* X-ray binary
* X-ray burster
* List
* Millisecond
* Be/X-ray
* Spin-up

Properties|

* Blitzar
* Fast radio burst
* Bondi accretion
* Chandrasekhar limit
* Gamma-ray burst
* Glitch
* Neutronium
* 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
* Astroseismology
* Compact star
* Quark star
* Exotic star
* Supernova
* Supernova remnant
* Related links
* Hypernova
* Kilonova
* Neutron star merger
* Quark-nova
* White dwarf
* Related links
* Stellar black hole
* Related links
* Radio star
* Pulsar planet
* Pulsar wind nebula
* Thorne–Żytkow object

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
* Tempo software program
* Astropulse
* The Magnificent Seven

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