The Jodrell bank glitch catalogue: 106 new rotational glitches in 70 pulsars

Abstract

Pulsar glitches are rapid spin-up events that occur in the rotation of neutron stars, providing a valuable probe into the physics of the interiors of these objects. Long-term monitoring of a large number of pulsars facilitates the detection of glitches and the robust measurements of their parameters. The Jodrell Bank pulsar timing programme regularly monitors more than 800 radio pulsars and has accrued, in some cases, over 50 years of timing history on individual objects. In this paper we present 106 new glitches in 70 radio pulsars as observed up to the end of 2018. For 70 per cent of these pulsars, the event we report is its only known glitch. For each new glitch we provide measurements of its epoch, amplitude and any detected changes to the spin-down rate of the star. Combining these new glitches with those listed in the Jodrell Bank glitch catalogue we analyse a total sample of 543 glitches in 178 pulsars. We model the distribution of glitch amplitudes and spin-down rate changes using a mixture of two Gaussian components. We corroborate the known dependence of glitch rate and activity on pulsar spin-down rates and characteristic ages, and show that younger pulsars tend to exhibit larger glitches. Pulsars with spin-down rates between 10−14 Hz s−1 and 10−10.5 Hz s−1 show a mean reversal of 1.8 per cent of their spin-down as a consequence of glitches. Our results are qualitatively consistent with the superfluid vortex unpinning models of pulsar glitches.

Detection of 16 Small Glitches in Nine Pulsars

“…The glitch epoch was kept halfway between the last pre-glitch observation and the first post-glitch observation, with an uncertainty of a quarter of the observation gap. In table 1, all these pulsars have been observed with glitches before (Basu et al, 2022;Lower et al, 2021;Yu et al, 2013;Espinoza et al, 2011;Yuan et al, 2010). There are 10 glitches reported in Lower et al (2021) and Basu et al (2022) were also detected by us.…”

Thermal and non-thermal X-ray emission from the rotation-powered radio/$γ$-ray pulsar PSR J1740+1000

“…However, such rather small probability favours the possibility that the stellar properties might have slightly changed. This could be related to the glitch that occurred in 2012 (Basu et al 2022), between the old and the new XMM-Newton observations. We note also that long term variations in the soft X-ray emission of isolated NS has been observed also in RX J0720.…”

“…The pulsar exhibits significant red spin noise which prevents us from extrapolating the timing of the pulsar back to earlier X-ray observations, and so the previously published ephemeris was used for the 2006 observation, also listed in Table 2. They are significantly different because of a glitch that occurred in 2012 (Basu et al 2022).…”

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

“…This glitch is in the expected size range of the UTMOST undetected events, which was set to 4.1 × 10 −11 − 2.7 × 10 −7 based on injection studies performed by Dunn et al (2022). According to the multiple statistical studies of the glitch behaviours (see, e.g., Dang et al (2020); Basu et al (2022)), a striking aspect is that the observed event sizes of pulsars with large τc show a clear trend towards being smaller. For old pulsars with τc > 1 Myr, ∆ν/ν of almost all glitches are smaller than 10 −7 (Liu et al 2021b) and their occurrence rate is much lower than that of young pulsars (Dang et al 2020).…”