Peculiar glitch of PSR J1119−6127 and extension of the vortex creep model

Akbal, Onur; Gügercinoğlu, Erbil; Mus, Sinem Sasmaz; Alpar, M. A.

doi:10.1093/mnras/stv322

Cited by 35 publications

(51 citation statements)

References 48 publications

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“…These vortex numbers are of the same order as inferred for other glitches of the Crab (Alpar et al 1996;Akbal & Alpar 2018) and Vela pulsars (Akbal et al 2017) as well as in PSR J1119−6127 (Akbal et al 2015). Statistical studies show that the associated ratio δΩ s /Ω s also seems to lie in a common range in all pulsars irrespective of age (Alpar & Baykal 1994).…”

Section: Discussionsupporting

confidence: 79%

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The largest Crab glitch and the vortex creep model

Gügercinoğlu

Alpar

2019

Monthly Notices of the Royal Astronomical Society

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The Crab pulsar displayed its largest glitch on 2017 November. An extended initial spin-up phase of this largest glitch was resolved, for the first time with high cadence of observations both in radio and X-rays on a time-scale of 2 days. A combination of crustquake and vortex unpinning models is invoked to account for the extended spin-up, magnitude and post-glitch relaxation characteristics of this glitch. We evaluate the extended spin-up followed by the familiar spin-down as due to the creep response to the initial induced inward motion of some vortex lines pinned to broken crustal plates moving inward towards the rotation axis, together with the common and familiar post-glitch creep response to the sudden outward motion of vortices unpinned at the glitch. Our analysis confirms that the number of unpinned vortices participating in glitches are similar in all Crab glitches, and within an order of magnitude in all glitches from all pulsars. This typical number of unpinned vortices is related to the broken plate size in quakes as triggers for vortex unpinning avalanches. The physical determinant of this universal broken plate size is in turn the critical strain angle in the neutron star crust. Occurrence of this largest Crab glitch after a relatively long inactive period is consistent with accumulation of the pinned vorticity to be tapped.

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Section: Discussionsupporting

confidence: 79%

“…The broken plate size D in a crustquake can be determined from simple geometrical arguments (Akbal et al 2015):…”

Section: Discussionmentioning

confidence: 99%

The largest Crab glitch and the vortex creep model

Gügercinoğlu

Alpar

2019

Monthly Notices of the Royal Astronomical Society

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“…This was the first time that a glitch, or the post-glitch recovery process, has been observed to influence the radio emission process of a normal (non-RRAT) pulsar. A starquake model with crustal plate movement has been proposed to explain the changing emission properties coincident with the glitch (Akbal et al 2015), as well as the unusual glitch recovery (see Antonopoulou et al 2015).…”

Section: Single Pulsesmentioning

confidence: 99%

Peculiar spin frequency and radio profile evolution of PSR J1119−6127 following magnetar-like X-ray bursts

Dai

Johnston

Weltevrede

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the spin frequency and profile evolution of the radio pulsar J1119−6127 following magnetar-like X-ray bursts from the system in 2016 July. Using data from the Parkes radio telescope, we observe a smooth and fast spin-down process subsequent to the X-ray bursts resulting in a net change in the pulsar rotational frequency of ∆ν ≈ −4 × 10 −4 Hz. During the transition, a net spin-down rate increase of ∆ν ≈ −1 × 10 −10 Hz s −1 is observed, followed by a return ofν to its original value. In addition, the radio pulsations disappeared after the X-ray bursts and reappeared about two weeks later with the flux density at 1.4 GHz increased by a factor of five. The flux density then decreased and undershot the normal flux density followed by a slow recovery back to normal. The pulsar's integrated profile underwent dramatic and shortterm changes in total intensity, polarization and position angle. Despite the complex evolution, we observe correlations between the spin-down rate, pulse profile shape and radio flux density. Strong single pulses have been detected after the X-ray bursts with their energy distributions evolving with time. The peculiar but smooth spin frequency evolution of PSR J1119−6127 accompanied by systematic pulse profile and flux density changes are most likely to be a result of either reconfiguration of the surface magnetic fields or particle winds triggered by the X-ray bursts. The recovery of spin-down rate and pulse profile to normal provides us the best case to study the connection between high magnetic-field pulsars and magnetars.

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“…The approximately constant second derivativeΩ c interglitch timing behaviour observed in the Vela and other pulsars (Akbal et al 2017;Yu et al 2013) corresponds to a uniform density of vortices unpinned at the glitch leading to a range of waiting times throughout the superfluid regions. Two component models with linear or nonlinear internal torques have so far been applied to post-glitch or inter-glitch timing behaviour of radio pulsars (Alpar et al 1993(Alpar et al , 1996Akbal et al 2015Akbal et al , 2017Gügercinoglu 2017), where the external torque, with a secular (characteristic) timescale τ c ≡ Ω c /2|Ω c | ∼ 10 3 − 10 6 yr is constant for timescales of observed postglitch relaxation.…”

Section: Two-component Models With Constant External Torquementioning

confidence: 99%

“…There is no evidence that the external torque is changing in pulsar glitches (this may not be the case for the exceptional glitch of PSR J 1119−6127 where the pulsar signature changes at the glitch possibly indicating a change in the external torque (Akbal et al 2015;Archibald et al 2016)). Hence the observed glitch associated offsets ∆Ω c in the crust spindown rate and the subsequent relaxation give a measure of the ratio of moments of inertia of the crust and the superfluid components involved:…”

Section: Introductionmentioning

confidence: 99%

Neutron star dynamics under time-dependent external torques

Alpar

Gügercinoğlu

2017

Monthly Notices of the Royal Astronomical Society

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The two component model describes neutron star dynamics incorporating the response of the superfluid interior. Conventional solutions and applications involve constant external torques, as appropriate for radio pulsars on dynamical timescales. We present the general solution of two component dynamics under arbitrary time dependent external torques, with internal torques that are linear in the rotation rates, or with the extremely non-linear internal torques due to vortex creep. The two-component model incorporating the response of linear or nonlinear internal torques can now be applied not only to radio pulsars but also to magnetars and to neutron stars in binary systems, with strong observed variability and noise in the spin-down or spin-up rates. Our results allow the extraction of the time dependent external torques from the observed spin-down (or spin-up) time series,Ω(t). Applications are discussed.

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Peculiar glitch of PSR J1119−6127 and extension of the vortex creep model

Cited by 35 publications

References 48 publications

The largest Crab glitch and the vortex creep model

The largest Crab glitch and the vortex creep model

Peculiar spin frequency and radio profile evolution of PSR J1119−6127 following magnetar-like X-ray bursts

Neutron star dynamics under time-dependent external torques

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