On the distributions of pulsar glitch sizes and the inter-glitch time intervals

Eya, Innocent O.; Urama, J. O.; Chukwude, A. E.

doi:10.1088/1674-4527/19/6/89

Cited by 17 publications

(23 citation statements)

References 59 publications

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“…Equally, lesser spin-down rates would entail larger time intervals between glitches (i.e. low glitch rate), not essentially a reduction in glitch sizes, as the glitch size depends directly on the number of unpinned vortices (Warszawski & Melatos 2011) and inter-glitch time intervals are size independent (Eya et al 2019b).…”

Section: Discussionmentioning

confidence: 99%

Microglitches in radio pulsars: the role of strange nuggets

Eya

Iyida

Urama

et al. 2020

Astrophys Space Sci

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Strange Nuggets are believed to be among the relics of the early universe. They appear as dark matter due to their low charge-to-mass ratio. Their distribution is believed to be the same as that of dark matter. As such, they could be accreted by high magnetic field objects and their collisions with pulsars are inevitable. Pulsar glitches are commonly seen as sudden spin-ups in pulsar frequency. It is still an open debate with regard to mechanisms giving rise to such a phenomenon. However, there is a class of sudden changes in pulsar spin frequency known as microglitches. These event are characterized by sudden small change in pulsar spin frequency (δν/ν ≈ ±10 −9). Clearly, the negative signature seen in some of the events is inconsistent with the known glitch mechanisms. In this analysis, we suggest that accretion of strange nuggets with pulsars could readily give rise to microglitch events. The signature of the events depends on the energy of the strange nuggets and line of interaction.

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Section: Discussionmentioning

confidence: 99%

Microglitches in radio pulsars: the role of strange nuggets

Eya

Iyida

Urama

et al. 2020

Astrophys Space Sci

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“…The glitch size, ∆ν/ν is in the range 10 −11 − 10 −5 (Espinoza et al 2011;Yu et al 2013), while the interglitch time interval, δt is in the range 20 − 10 4 d (Eya, Urama & Chukwude 2019b). Technically if one assumes glitches as a natural phenomenon, which relives pulsar of stress accumulated over time due to electromagnetic breaking torque, one expects the glitch size to correlate with the inter-glitch time interval, but such is never observed.…”

Section: Introductionmentioning

confidence: 99%

On the pulsar spin frequency derivatives and the glitch activity

Eya,

Alhassan,

Iyida

et al. 2022

Preprint

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The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative, ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of of quantifying the A g with the pulsars main spin frequency derivatives (i.e. ν and ν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ ν2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of |ν|/ ν2 distribution appear to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ ν2 ) 0.23 . The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir

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“…Macroglitches are unusual spectacular events usually characterized by recovery of the pulsar spin down rate on wide range of timescales (Flanagan 1990;1995;Urama 2002;Eya et al, 2017;Eze et al, 2018). Microglitches (|∆ν/ν| < 10 −9 ) on the other hand, are not well understood, less attractive and described by variable signatures (Cordes & Downs, 1985;Chukwude & Urama, 2010;Eya et al, 2019). Generally, glitches are posited to originate from either the release of built up tension within the neutron star's crust by starquakes (Ruderman, 1969), or the unpinning of superfluid vortices from the crustal lattice (Anderson & Itoh, 1975;Alpar et al, 1984;Melatos et al, 2008).…”

Section: Introductionmentioning

confidence: 99%

Diagnostics of interstellar medium parameters on non-discrete timing irregularities of pulsars

Iyida

Eze

2021

IJAA

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In this paper, a large homogenous sample of Jodrell Bank Observatory (JBO) radio pulsars was used to investigate the statistical effects of interstellar medium (ISM) parameters: dispersion and rotation measure (DM and RM, respectively) on non-discrete timing irregularities of our sample (whose observed timing activity timescales span over 40 years). This is done by using the correlations between the measured DM and RM, and some parameters that have been commonly used to measure non-discrete timing irregularities [timing activity parameter (A), the amount of timing fluctuations absorbed by the cubic term (σR23), measure of pulsar rotational stability (σz ) and stability parameter (∆8)]. Our results show that ISM parameters positively correlate (r > 0.60) with the pulsar timing irregularities parameters of our sample. The significant relationships observed are discussed.

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On the distributions of pulsar glitch sizes and the inter-glitch time intervals

Cited by 17 publications

References 59 publications

Microglitches in radio pulsars: the role of strange nuggets

Microglitches in radio pulsars: the role of strange nuggets

On the pulsar spin frequency derivatives and the glitch activity

Diagnostics of interstellar medium parameters on non-discrete timing irregularities of pulsars

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