Gross-Pitaevskii model of pulsar glitches

Warszawski, Lila; Melatos, A.

doi:10.1111/j.1365-2966.2011.18803.x

Cited by 89 publications

(152 citation statements)

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“…Example of results for the spin down of the crust in different numerical experiments, with varying ratio of occupied to free pinning sites, npin/nF, as described in Warszawski & Melatos (2011) [23]. One can clearly see that the spin-down is more spasmodic for a higher number of pinned vortices.…”

Section: Figmentioning

confidence: 99%

“…Warszawski and Melatos [23,24,164] have shown that pulsar glitches may by a manifestation of SOC, which would explain many aspects of the phenomenon and describe how collective motion of vortices can trigger glitches of varying size. In particular two different mechanisms have been considered as the source of scale-invariant dynamics in pulsars: vortex avalanches [23,24] and coherent noise processes [165]. Let us analyse both these mechanisms in more detail.…”

Section: Scale Invariance and Vortex Avalanchesmentioning

confidence: 99%

“…To study this problem Warszawski and Melatos [23] evolve a two-dimensional, decelerating, pinned superfluid by solving the two-dimensional dissipative Gross-Pitaevskii equation (GPE)…”

Section: Gross-pitaevskii Simulationsmentioning

confidence: 99%

“…Warszawski and Melatos [23] carried out a series of numerical experiments with different parameters. In general, collective motion of vortices is observed, with vortex avalanches giving rise to glitches in the spin-down and distributions of sizes which obey power laws, with exponentially distributed waiting times.…”

Section: Gross-pitaevskii Simulationsmentioning

confidence: 99%

“…recent simulations based on this scenario have successfully described several aspects of Vela giant glitches [22] and the statistics of the glitching populations as a whole [23,24]. Nevertheless several issues still need to resolved before the vortex picture attains the status of a self-consistent, predictive, falsifiable theory.…”

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confidence: 99%

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Models of pulsar glitches

Haskell

Melatos

2015

Int. J. Mod. Phys. D

319

304

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Radio pulsars provide us with some of the most stable clocks in the universe. Nevertheless several pulsars exhibit sudden spin-up events, known as glitches. More than forty years after their first discovery, the exact origin of these phenomena is still open to debate. It is generally thought that they an observational manifestation of a superfluid component in the stellar interior and provide an insight into the dynamics of matter at extreme densities. In recent years there have been several advances on both the theoretical and observational side, that have provided significant steps forward in our understanding of neutron star interior dynamics and possible glitch mechanisms. In this article we review the main glitch models that have been proposed and discuss our understanding, in the light of current observations.Radio pulsars are thought to be rotating magnetised neutron stars (NS). The huge moment of inertia (of the order of 10 45 g cm 2 ) leads to exceptionally stable rotation rates and provides us with some of the most precise clocks in the universe. The best timed millisecond pulsars are stable to a precision which rivals that of atomic clocks [1]. Nevertheless radio pulsars exhibit several timing irregularities, the most striking of which are the so-called glitches. While most objects are observed to steadily spin-down due to the emission of electromagnetic and, possibly, gravitational waves, many pulsars show sudden increases in their spin, in some cases followed by an increase in their spin-down rate, i.e. glitches. Most pulsars also show slower, long-term, stochastic deviations from a regular spin-down law, that are generally classed as 'timing noise' and are not the main focus of this review article.Soon after the discovery of the first glitches in the Vela [2,3] and Crab [4,5] pulsars in 1969, several mechanisms were suggested to explain these phenomena. Although some initial suggestions featured external mechanisms, such as plasma explosions in the magnetosphere [6] or planets around the pulsar [7], the lack of radiative and pulse profile changes associated with these events was taken as evidence for an internal origin. The situation is different for rotating radio transients (RRATs) and magnetars, which are now known to glitch and do exhibit, amongst other peculiar traits, radiative changes associated with these events [8][9][10][11]. Magnetospheric activity is likely to play a role in these objects, as we discuss below.There are two main internal glitch mechanisms that have been examined in the literature. The first set of models relies on the fact that the outer layers of a neutron star form a crystalline crust that can support stress. As the NS spins down, the liquid core adjusts its shape to the rotation rate, while the solid crust maintains the shape appropriate for the previous, higher, spin rate. This leads to an increasing amount of strain building up in the crust, which is eventually released in the form of a star quake. The quake causes a sudden rearrangement of the moment of inertia and...

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Section: Figmentioning

confidence: 99%

Section: Scale Invariance and Vortex Avalanchesmentioning

confidence: 99%

“…To study this problem Warszawski and Melatos [23] evolve a two-dimensional, decelerating, pinned superfluid by solving the two-dimensional dissipative Gross-Pitaevskii equation (GPE)…”

Section: Gross-pitaevskii Simulationsmentioning

confidence: 99%

Section: Gross-pitaevskii Simulationsmentioning

confidence: 99%

mentioning

confidence: 99%

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Models of pulsar glitches

Haskell

Melatos

2015

Int. J. Mod. Phys. D

319

304

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Gravitational Waves from Single Neutron Stars: An Advanced Detector Era Survey

Glampedakis

Gualtieri

2018

The Physics and Astrophysics of Neutron Stars

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With the doors beginning to swing open on the new gravitational wave astronomy, this review provides an up-to-date survey of the most important physical mechanisms that could lead to emission of potentially detectable gravitational radiation from isolated and accreting neutron stars. In particular we discuss the gravitational wave-driven instability and asteroseismology formalism of the f -and r-modes, the different ways that a neutron star could form and sustain a non-axisymmetric quadrupolar "mountain" deformation, the excitation of oscillations during magnetar flares and the possible gravitational wave signature of pulsar glitches. We focus on progress made in the recent years in each topic, make a fresh assessment of the gravitational wave detectability of each mechanism and, finally, highlight key problems and desiderata for future work.

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Superfluidity and Superconductivity in Neutron Stars

Haskell

Sedrakian

2018

Astrophysics and Space Science Library

106

115

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This review focuses on applications of the ideas of superfluidity and superconductivity in neutron stars in a broader context, ranging from the microphysics of pairing in nucleonic superfluids to macroscopic manifestations of superfluidity in pulsars. The exposition of the basics of pairing, vorticity and mutual friction can serve as an introduction to the subject. We also review some topics of recent interest, including the various types of pinning of vortices, glitches, and oscillations in neutron stars containing superfluid phases of baryonic matter.

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Gross-Pitaevskii model of pulsar glitches

Cited by 89 publications

References 57 publications

Models of pulsar glitches

Models of pulsar glitches

Gravitational Waves from Single Neutron Stars: An Advanced Detector Era Survey

Superfluidity and Superconductivity in Neutron Stars

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