Statistical studies of pulsar glitches

By Andrew G. Lyne, S. Shemar, F. Smith. 2000

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Subfields: Astronomy and Astrophysics, Biomedical Engineering, Oceanography

View Paper: https://www.semanticscholar.org/paper/4faf42954b4b5c1489b0aeab1d1c45c1088cc66d

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Citations in the corpus

Detection of 107 glitches in 36 southern pulsars (2012, background): “Fractional glitch sizes ∆νg/ν show a bimodal distribution with peaks at ∼ 10−9 and ∼ 10−6 (Lyne et al. 2000; Wang et al. 2000; Yuan et al. 2010a).”
Avalanche Dynamics of Radio Pulsar Glitches (2007, background): “The ‘‘staircase’’ described by equation (20) has been noted previously (Shemar & Lyne 1996; Lyne et al. 2000), both in quasi-periodic glitchers such as PSR J0537 6910 (e.g., Figure 8 in Middleditch et al. 2006), where the reservoir effect is obvious, and in Poisson glitchers such as PSR J0534+2200,…”
An analysis of the timing irregularities for 366 pulsars (2009, background): “No model currently predicts the time between glitches or the size of any given event although pulsars with large glitches tend to show larger intervals between glitches (Lyne et al. 2000).”
The Parkes multi-beam pulsar survey - I. Observing and data analysis systems, discovery and timing of 100 pulsars (2001, background): “Lyne et al. (2000) announced the discovery of PSR J1811–1736, a pulsar with a period of 104 ms in a highly eccentric orbit of a period of 18.8 d with a companion of minimum mass 0.7 M(, most probably a neutron star, making this the fourth or fifth double neutron star system known in the Galactic…”
The Parkes Pulsar Timing Array Project (2006, background): “It is well known that large positive values of ν̈ are observed after glitches in young pulsars (Lyne et al. 2000; Yuan et al. 2010).”
The glitch-induced identity changes of PSR J1119−6127 (2010, methodology): “The parameter Q = ∆νd/∆νg is used to quantify the degree of recovery of the spin frequency (e.g. Shemar & Lyne 1996) and it is observed that pulsars exhibit Q < 1 for most glitches (e.g. Lyne et al. 2000).”
A study of 315 glitches in the rotation of 102 pulsars (2011, methodology): “Following Lyne et al. (2000), the glitch spin-up rate of a group of pulsars is defined as ν̇glitch = ∑ i ∑ j νij∑ i Ti , (2) where the double sum runs over every frequency jump ν ij due to the glitch j on the pulsar i, and the sum in the denominator is the accumulated years of observation of all…”
Discovery of Two High Magnetic Field Radio Pulsars (2000, background): “The glitch observed in PSR J1119[6127 is small compared with most glitches in most pulsars, with *l/ l\ (4.4^ 0.4)] 10~9 (Table 1), but it is of similar fractional size as three of the Ðve glitches observed in the Crab pulsar over 23 yr (Lyne et al. 2000b).”