Repeated State Change of Variable Gamma-Ray Pulsar PSR J2021+4026

Takata, Jumpei; Wang, Hui Hui; Lin, L.; Hu, Chin-Ping; Hui, C. Y.; Kong, Albert; Tam, Pak-Hin Thomas; Li, K. L.; Cheng, K. S.

doi:10.3847/1538-4357/ab67b1

Cited by 17 publications

(7 citation statements)

References 34 publications

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“…The first state change (jump) was observed in October 2011 [5], when the flux dropped by ∼ 18% and the spin-down rate increased by ∼ 5.6% in a timescale < 7 days. After a slow recovery, occurred over ∼ 100 days around December 2014 [6] [7], a similar jump occurred in February 2018 [8]. Previous works also studied the variations of the γ-ray spectrum and of the pulse profile.…”

Section: Introductionmentioning

confidence: 99%

Study of the gamma-ray state changes of PSR J2021+4026 with Fermi-LAT

Fiori¹,

Razzano²,

Parkinson³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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The peculiar radio-quiet PSR J2021+4026, in the Gamma Cygni supernova remnant, is one of the brightest of the over 250 pulsars detected by Fermi-LAT. It is unique in being the only known isolated gamma-ray pulsar to undergo abrupt flux changes, which are also simultaneous with spin-down variations. The first change was observed by Fermi-LAT in October 2011, and it was followed by a recovery over a timescale of 100 days around December 2014. A second change occurred in February 2018. In the last few years, PSR J2021+4026 has been widely studied at different wavelengths. We report our latest results on this source, based on a Fermi-LAT analysis of its gamma-ray variability. In particular, we have studied the changes in the spectral and timing parameters on different timescales. Our results are essential to relate the observed events to changes in the geometry of the particle acceleration regions in the pulsar magnetosphere. Therefore, this study will allow us to enhance our knowledge of this source and its behavior.

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Section: Introductionmentioning

confidence: 99%

Study of the gamma-ray state changes of PSR J2021+4026 with Fermi-LAT

Fiori¹,

Razzano²,

Parkinson³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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“…A large glitch with two exponential recoveries in PSR J1119-6227 was found to be coincident with the appearance of additional pulse components with intermittent or RRAT-like behaviour (Weltevrede et al 2011). Repeated state changes have been detected in the only known variable gamma-ray pulsar PSR J2021+4026 (Takata et al 2020). The gamma-ray pulsar PSR J1124-5916 has also experienced spin-down rate transition with no significant difference between the pulse profiles in different states (Ge et al 2020b).…”

Section: Introductionmentioning

confidence: 88%

“…Nevertheless, the scenario that the measurable changes in spin-down rate, flux, and pulse shape of pulsars is driven by a shift in the magnetic inclination angle α as a consequence of a glitch, has gradually become a consensus (Link & Epstein 1997;Akbal et al 2015;Ng et al 2016;Liu et al 2021b). In this work, motivated by the interesting repeated mode-changing behaviours in several pulsars (Kou et al 2018;Takata et al 2020) and a potential for periodical variations in the emission profile and ν of PSR J0738-4042 (Brook et al 2014), we carry out data analysis of PSR J0738-4042 by using the combined UTMOST and Parkes timing observations conducted between March 2008 and September 2020 to keep track of the long-term rotational history and pulse profile evolution for this pulsar. Along the way a new glitch is identified associated with the pulse profile changes in PSR J0738-4042.…”

Section: Introductionmentioning

confidence: 97%

“…Their emission mode-changing featuressudden changes to the pulse profile shape or the total flux density, are associated with irregularities in the spin properties (Brook et al 2016). During this period, the spin-down rate usually jumps up to a higher state (Takata et al 2020;Shaw et al 2022). Not surprisingly, the observed sizes of glitches coupled with emission mode switching decrease with increasing characteristic age τc.…”

Section: Introductionmentioning

confidence: 99%

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New pulse profile variability associated with the glitch of PSR J0738-4042

Zhou¹,

E.²,

Yuan³

et al. 2022

Preprint

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The close correlation observed between emission state and spin-down rate change of pulsars has many implications both for the magnetospheric physics and the neutron star interior. The middle-aged pulsar PSR J0738-4042, which had been observed to display variations in the pulse profile associated with its spin-down rate change due to external effects, is a remarkable member of this class. In this study, based on the 12.5-yr combined public timing data from UTMOST and Parkes, we have detected a new emission-rotation correlation in PSR J0738-4042 concurrent with a glitch. The first glitch occurred in this pulsar at MJD 57359(5) (December 3, 2015) is considered to be underlying reason of the variability. Unlike the usual glitch behaviours, the braking torque on the pulsar has continued to increase over 1380 d since small spin-up event (∆ν/ν ∼ 0.36(4) × 10 −9 ), corresponding to a significant decrease in ν. As for changes in the pulse profile after the glitch, the relative amplitude of the leading component weakens drastically, while the middle component becomes stronger. A combined model of crustquake induced platelet movement and vortex creep response is invoked to account for this rare correlation. In this scenario, magnetospheric statechange is naturally linked to the pulsar-intrinsic processes that give rise to a glitch.

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“…The discoveries of RBs show that the properties of MSPs can vary considerably in different wavelengths as they switch between a rotationpowered state and an accretion-powered state (e.g., Papitto et al 2013a;Takata et al 2014). On the other hand, evidence of variable X-ray/γ-ray emission has also been observed from some isolated pulsars in GF (e.g., Hermsen et al 2013;Takata et al 2020;Lin et al 2021).…”

Section: Variability Analysismentioning

confidence: 99%

A Comparison of Millisecond Pulsar Populations between Globular Clusters and the Galactic Field

Lee

Hui

Takata

et al. 2023

ApJ

Self Cite

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We have performed a systematic study of the rotational, orbital, and X-ray properties of millisecond pulsars (MSPs) in globular clusters (GCs) and compared their nature with those of the MSPs in the Galactic field (GF). We found that GC MSPs generally rotate slower than their counterparts in the GF. Different from the expectation of a simple recycling scenario, no evidence for the correlation between the orbital period and the rotation period can be found in the MSP binaries in GCs. There is also an indication that the surface magnetic field of GC MSPs is stronger than those in the GF. All these suggest dynamical interactions in GCs can alter the evolution of MSPs/their progenitors, which can leave an imprint on their X-ray emission properties. While the MSPs in both GF and GCs have similar distributions of X-ray luminosity and hardness, our sample supports the notion that these two populations follow different relations between the X-ray luminosity and spin-down power. We discuss this in terms of both the pulsar emission model and the observational bias.

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Repeated State Change of Variable Gamma-Ray Pulsar PSR J2021+4026

Cited by 17 publications

References 34 publications

Study of the gamma-ray state changes of PSR J2021+4026 with Fermi-LAT

Study of the gamma-ray state changes of PSR J2021+4026 with Fermi-LAT

New pulse profile variability associated with the glitch of PSR J0738-4042

A Comparison of Millisecond Pulsar Populations between Globular Clusters and the Galactic Field

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