Long-term statistics of pulsar glitches triggered by a Brownian stress accumulation process

Carlin, J. B.; Melatos, A.

doi:10.1093/mnras/staa935

Cited by 14 publications

(17 citation statements)

References 56 publications

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“…Note, the p-value for the backward cross-correlation is an artefact of the significant scatter and corresponding lack of correlation. The moderate forward cross-correlation is consistent with previously reported values (Melatos et al 2018;Fuentes et al 2019;Carlin & Melatos 2020). The marginal auto-correlations for the glitch wait time, 𝜌 𝑠, Δ𝑇 𝑔 = −0.0048 (p-value 0.98), and size, 𝜌 𝑠, Δ𝜈 = −0.26 (p-value 0.15), are consistent with the BSA process.…”

Section: Statistics Of Glitches In Psrs J1341−6220 and J1413−6141supporting

confidence: 92%

The impact of glitches on young pulsar rotational evolution

Lower,

Johnston,

Dunn

et al. 2021

Preprint

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We report on a timing programme of 74 young pulsars that have been observed by the Parkes 64-m radio telescope over the past decade. Using modern Bayesian timing techniques, we have measured the properties of 124 glitches in 52 of these pulsars, of which 74 are new. We demonstrate that the glitch sample is complete to fractional increases in spin-frequency greater than Δ𝜈 90%𝑔 /𝜈 ≈ 9.3 × 10 −9 . We measure values of the braking index, 𝑛, in 33 pulsars. In most of these pulsars, their rotational evolution is dominated by episodes of spin-down with 𝑛 > 10, punctuated by step changes in the spin-down rate at the time of a large glitch. The step changes are such that, averaged over the glitches, the long-term 𝑛 is small. We find a near one-to-one relationship between the inter-glitch value of 𝑛 and the change in spin-down of the previous glitch divided by the inter-glitch time interval. We discuss the results in the context of a range of physical models.

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Section: Statistics Of Glitches In Psrs J1341−6220 and J1413−6141supporting

confidence: 92%

The impact of glitches on young pulsar rotational evolution

Lower,

Johnston,

Dunn

et al. 2021

Preprint

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“…In order to produce statistically useful numbers of glitches, computational constraints require spin-down rates far greater than those observed in even the most rapidly decelerating pulsars. The models with negative autocorrelations in waiting time and size are inconsistent with the Brownian meta-model, and are consistent with the statedependent Poisson model only in a restricted subset of parameter space (Carlin & Melatos 2019, 2020.…”

Section: Size-waiting Time Correlationsmentioning

confidence: 74%

“…The astrophysical details of the feedback mechanism lie outside the scope of this paper. We assume here for simplicity that it is instantaneous and lossless (Fulgenzi, Melatos & Hughes 2017;Carlin & Melatos 2020).…”

Section: Feedbackmentioning

confidence: 99%

Simulating pulsar glitches: an N-body solver for superfluid vortex motion in two dimensions

Howitt

Melatos

Haskell

2020

Monthly Notices of the Royal Astronomical Society

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A rotating superfluid forms an array of quantized vortex lines that determine its angular velocity. The spasmodic evolution of the array under the influence of deceleration, dissipation, and pinning forces is thought to be responsible for the phenomenon of pulsar glitches, sudden jumps in the spin frequency of rotating neutron stars. We describe and implement an N-body method for simulating the motion of up to 5000 vortices in two dimensions and present the results of numerical experiments validating the method, including stability of a vortex ring and dissipative formation of an Abrikosov array. Vortex avalanches occur routinely in the simulations, when chains of unpinning events are triggered collectively by vortex–vortex repulsion, consistent with previous, smaller scale studies using the Gross–Pitaevskii equation. The probability density functions of the avalanche sizes and waiting times are consistent with both exponential and lognormal distributions. We find weak correlations between glitch sizes and waiting times, consistent with astronomical data and meta-models of pulsar glitch activity as a state-dependent Poisson process or a Brownian stress-accumulation process, and inconsistent with a threshold-triggered stress-release model with a single, global stress reservoir. The spatial distribution of the effective stress within the simulation volume is analysed before and after a glitch.

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“…Table 9 in Warszawski & Melatos (2011) and Table 2 in Howitt et al (2020). The same is true in meta-models, where glitch activity is modeled as a state-dependent Poisson process without specializing to a particular version of the microphysics (Fulgenzi et al 2017;Carlin & Melatos 2019a;Melatos & Drummond 2019;Carlin & Melatos 2020).…”

Section: Physical Motivationmentioning

confidence: 96%

An updated glitch rate law inferred from radio pulsars

Millhouse,

Melatos,

Howitt

et al. 2022

Preprint

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Radio pulsar glitches probe far-from-equilibrium processes involving stress accumulation and relaxation in neutron star interiors. Previous studies of glitch rates have focused on individual pulsars with as many recorded glitches as possible. In this work we analyze glitch rates using all available data including objects that have glitched never or once. We assume the glitch rate follows a homogeneous Poisson process, and therefore exclude pulsars which exhibit quasiperiodic glitching behavior. Calculating relevant Bayes factors shows that a model in which the glitch rate 𝜆 scales as a power of the characteristic age 𝜏 is preferred over models which depend arbitrarily on powers of the spin frequency 𝜈 and/or its time derivative 𝜈. For 𝜆 = 𝐴(𝜏/𝜏 ref ) −𝛾 , where 𝜏 ref = 1 yr is a reference time, the posterior distributions are unimodal with 𝐴 = 0.0066 +0.003 −0.002 yr −1 , and 𝛾 = 0.27 +0.03 −0.03 . Importantly, the data exclude with 99% confidence the possibility 𝛾 = 1 canvassed in the literature. When objects with zero recorded glitches are included, the age-based rate law is still preferred and the posteriors change to give 𝐴 = 0.0099 +0.004 −0.003 yr −1 , and 𝛾 = 0.31 +0.03 −0.03 . The updated estimates still support increased glitch activity for younger pulsars, while demonstrating that the large number of objects with zero glitches contain important statistical information about the rate, provided that they are part of the same population as opposed to a disjoint population which never glitches for some unknown physical reason.

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Long-term statistics of pulsar glitches triggered by a Brownian stress accumulation process

Cited by 14 publications

References 56 publications

The impact of glitches on young pulsar rotational evolution

The impact of glitches on young pulsar rotational evolution

Simulating pulsar glitches: an N-body solver for superfluid vortex motion in two dimensions

An updated glitch rate law inferred from radio pulsars

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