International Journal of Astrophysics and Space Science
Volume 6, Issue 4, August 2018, Pages: 62-72
Received: Sep. 12, 2018;
Accepted: Sep. 28, 2018;
Published: Oct. 25, 2018
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Christian Ikechukwu Eze, Department of Physics and Astronomy, Faculty of Physical sciences, University of Nigeria, Nsukka, Nigeria
Evaristus Uzochukwu Iyida, Department of Physics and Astronomy, Faculty of Physical sciences, University of Nigeria, Nsukka, Nigeria
Finbarr Chidi Odo, Department of Physics and Astronomy, Faculty of Physical sciences, University of Nigeria, Nsukka, Nigeria
Johnson Ozoemena Urama, Department of Physics and Astronomy, Faculty of Physical sciences, University of Nigeria, Nsukka, Nigeria
Detailed long-term timing observations have revealed that the expected smooth spin- down of many pulsars is prone to a variety of discrete disruptions often referred to as glitches. Although the nature and behaviour of small glitches are still poorly understood compared to large glitches, it is widely believed that both originate from some complex dynamical changes within the neutron star interior and their study could provide valuable information about the internal structure and dynamics of the neutron stars. In this paper, the distribution of glitch sizes, glitch patterns and possible relationships between glitch parameters and pulsar rotational parameters were statistically investigated using 482 glitches reported in 168 pulsars. The distribution of glitch sizes showed predominance of large glitches for J0537-6910, J0835-4510, J1341-6220 and J18001-2304; small glitches for J0534+2200, J0631+1036 and J1740-3015 and continuous glitch size distribution for J0534+2200, J1341-6220, J1740-3015 and J1801-2304. PSRs J0537-6910 and J0835-4510 showed specific regular pattern with J1740-3015 showing a quasi-regular pattern. The mean glitch size of these pulsars relates considerably with rotational frequency (ν) and spin down rate (
) in simple power laws. Similarly, variation of glitch activity with the characteristic age (τ
) traces a curve that peaks at τ
yr and decays with age for older pulsars with τ
yr. The angular momentum transfer resulting to glitches appears to be maximum at youthful age (≈ 104
yr) of pulsars when certain rotational properties as well as temperature of the star best supports vortex pinning and unpinning of the superfluid of the star interior.
Christian Ikechukwu Eze,
Evaristus Uzochukwu Iyida,
Finbarr Chidi Odo,
Johnson Ozoemena Urama,
Statistical Study of Glitch Behaviours of Glitching Pulsars, International Journal of Astrophysics and Space Science.
Vol. 6, No. 4,
2018, pp. 62-72.
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