Timing and emission variation of PSR J1733−3716

Hu, Yue; Lin, Li; Yuan, Jianping; Dang, S. J.; Wang, S.Q; Wang, Z.J; Yuen, R.

doi:10.1007/s10509-020-03849-8

Cited by 4 publications

(3 citation statements)

References 38 publications

(44 reference statements)

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“…Figure 3 illustrates the correlation between period derivative ( . P) and spectral index, as reported in previous studies and this study [42][43][44][45]. It suggests that pulsars with higher .…”

Section: Discussionsupporting

confidence: 87%

Characterizing Timing Noise in Normal Pulsars with the Nanshan Radio Telescope

Yuan,

Wang,

Dang

et al. 2024

Universe

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We present a decade of observations of pulse arrival times for 85 pulsars using the Nanshan radio telescope from July 2002 to March 2014. The Cholesky method can accurately estimate the covariance function of the timing residuals, significantly improving the parameter’s estimation accuracy when red noise is prominent. We utilize the Cholesky method to determine positions and basic timing parameters of these pulsars, as well as to obtain timing residuals. Most of these sources showed evidence of significant timing irregularities, which are described. The spectral analyses of timing residuals are presented for pulsars showing obvious red noise. Our results show that timing residuals in half of these pulsars are attributed to rotational irregularities. The red noise in normal pulsars may originate from a random walk in spin frequency or spin-down rate.

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Section: Discussionsupporting

confidence: 87%

Characterizing Timing Noise in Normal Pulsars with the Nanshan Radio Telescope

Yuan,

Wang,

Dang

et al. 2024

Universe

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“…Decades of pulsar monitoring and glitch searches have also been carried out with the Nanshan 25-m radio telescope at Urumqi in China (e.g. [86,87]) and at the Pushchino Observatory in Russia (e.g. [88,89]).…”

Section: Pulse Arrival Times and Pulsar Monitoring Programsmentioning

confidence: 99%

Pulsar glitches: observations and physical interpretation

Antonopoulou¹,

Haskell²,

Espinoza³

2022

Rep. Prog. Phys.

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The interpretation of pulsar rotational glitches, the sudden increase in spin frequency of neutron stars, is a half-century-old challenge. The common view is that glitches are driven by the dynamics of the stellar interior, and connect in particular to the interactions between a large-scale neutron superfluid and the other stellar components. This thesis is corroborated by observational data of glitches and the post-glitch response seen in pulsars' rotation, which often involves very long timescales, from months to years. As such, glitch observables combined with consistent models incorporating the rich physics of neutron stars -- from the lattice structure of their crust to the equation of state for matter beyond nuclear densities -- can be very powerful at placing limits on, and reduce uncertainties of, the internal properties. This review summarises glitch observations, current data, and recent analyses, and connects them to the underlying mechanisms and microphysical parameters in the context of the most advanced theoretical glitch models to date.

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“…The leading component is brighter and modulates strongly, both components switch off simultaneously and the nulls are quasiperiodic and of short duration. A single pulse study of this pulsar is given in Hu et al (2020). PSR J1745-3040: This pulsar also has a peculiar profile which consists of a small leading component almost disjoint from a complex trailing component.…”

Section: Pulse Profile Variabilitymentioning

confidence: 99%

Two years of pulsar observations with the Ultra-Wideband Receiver on the Parkes radio telescope

Johnston,

Sobey,

Dai

et al. 2021

Preprint

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The major programme for observing young, non-recycled pulsars with the Parkes telescope has transitioned from a narrow-band system to an ultra-wideband system capable of observing between 704 and 4032 MHz. We report here on the initial two years of observations with this receiver. Results include dispersion measure (DM) and Faraday rotation measure (RM) variability with time, determined with higher precision than hitherto, flux density measurements and the discovery of several nulling and mode changing pulsars. PSR J1703-4851 is shown to be one of a small subclass of pulsars that has a weak and a strong mode which alternate rapidly in time. PSR J1114-6100 has the fourth highest |RM| of any known pulsar despite its location far from the Galactic Centre. PSR J1825-1446 shows variations in both DM and RM likely due to its motion behind a foreground supernova remnant.

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Timing and emission variation of PSR J1733−3716

Cited by 4 publications

References 38 publications

Characterizing Timing Noise in Normal Pulsars with the Nanshan Radio Telescope

Characterizing Timing Noise in Normal Pulsars with the Nanshan Radio Telescope

Pulsar glitches: observations and physical interpretation

Two years of pulsar observations with the Ultra-Wideband Receiver on the Parkes radio telescope

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