Query : 2017A&A...608A.131F

2017A&A...608A.131F - Astronomy and Astrophysics, volume 608A, 131-131 (2017/12-1)

The glitch activity of neutron stars.


Abstract (from CDS):

We present a statistical study of the glitch population and the behaviour of the glitch activity across the known population of neutron stars. An unbiased glitch database was put together based on systematic searches of radio timing data of 898 rotation-powered pulsars obtained with the Jodrell Bank and Parkes observatories. Glitches identified in similar searches of 5 magnetars were also included. The database contains 384 glitches found in the rotation of 141 of these neutron stars. We confirm that the glitch size distribution is at least bimodal, with one sharp peak at approximately 20 µHz, which we call large glitches, and a broader distribution of smaller glitches. We also explored how the glitch activity νg, defined as the mean frequency increment per unit of time due to glitches, correlates with the spin frequency ν, spin-down rate |ν|, and various combinations of these, such as energy loss rate, magnetic field, and spin-down age. It is found that the activity is insensitive to the magnetic field and that it correlates strongly with the energy loss rate, though magnetars deviate from the trend defined by the rotation-powered pulsars. However, we find that a constant ratio νg/|ν|=0.010±0.001 is consistent with the behaviour of all rotation-powered pulsars and magnetars. This relation is dominated by large glitches, which occur at a rate directly proportional to |ν|. For low |ν|, only small glitches have been detected, making the inferred glitch activity formally lower than that predicted by the constant ratio, in many cases zero. However, we can attribute this to the low predicted rate for large glitches, together with the insufficient observing time, which makes it unlikely to detect any large glitches in this range. Taking this into consideration, we show that the behaviour of each rotation-powered pulsar and magnetar is statistically consistent with the above relationship, including those objects where no glitches have been detected so far. The only exception are the rotation-powered pulsars with the highest values of |ν|, such as the Crab pulsar and PSR B0540-69, which exhibit a much smaller glitch activity, intrinsically different from each other and from the rest of the population. The activity due to small glitches also shows an increasing trend with |ν|, but this relation is biased by selection effects.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: neutron - stars: magnetars - pulsars: general - stars: rotation - stars: rotation

Errata: erratum vol. 618, art. C1 (2018)

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4940 1
2 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5800 4
3 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 243 1
4 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 820 3
5 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1149 2
6 PSR J1119-6127 Psr 11 19 14.30 -61 27 49.5           ~ 357 1
7 PSR J1420-6048 Psr 14 20 08.190 -60 48 14.85           ~ 171 0
8 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 317 2

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