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.
Lorimer, D. R. and Kramar, M. 2005. Handbook of pulsar astronomy. UK: Cambridge University Press.
McKenna, J., and Lyne, A. G. PSRI737 – 30 and period discontinues in young pulsars. Nature, 343, 1990, 349–350.
Manchester, R. N., and Taylor, J. H. 1977, Pulsars. United states: W. H. Freeman and Company, San Francisco.
Lyne, A. G. Pritchard, R. S. and Shemar, S. Timing Noise and glitches Astronomy and Astrophysics, 16, 1995, 179–190.
Chamel, N. and Haensel, P. Physics of neutron star crusts. Living rev. relativity II, 10, 2008, 1433–1451.
Hobbs, G., Lyne, A. G., and Kramar M. An analysis of the timing irregularities for 366 pulsars. Mon. Not. R. Astron. Soc., 402, 2010, 1027–1048.
Lyne, A. G., Shemar, S. L., and Graham Smith, F. Statistical Studies of Pulsar glitches. Mon. Not. R. Astron. Soc., 315, 2000, 534–542.
Ruderman, M., Zhu, T., and Chen, K. Neutron star magnetic field evolution, crust movement, and glitches. Astrophysical Journal, 492, 1998, 267–280.
Cordes, J. M., Downs, G. S., and Krause P. J. JPL pulsar timing observation. V. – Micro and Macrojumps in the Vela pulsar 0835–455. Astrophysical Journal, 330, 1988, 847–869.
Jones, P. B. The origin of pulsar glitches Mon. Not. R. Astron. Soc., 296, 1998, 217-224.
Espinoza, C. M., Lyne, A. G., Stappers, B. W. and Kramer, M. A study of 315 glitches in the rotation of 102 pulsars. Mon. Not. R. Astron. Soc., 414, 2011, 1679–1704.
Eya, I. O. and Urama, J. O. Statistical study of neutron star glitches. International Journal of Astrophysics and space science. 2, 2014, 16–21. doi: 10.11648/j.ijass.20140202.11.
Chukwude A. E. and Urama J. O. Observation of microglitches in HartRAO radio pulsars. Mon. Not. R. Astron. Soc., 406, 2010, 1907–1917.
Urama, J. O. Glitch monitoring in PSR, B1046 – 58 and B1737 – 30. Mon. Not. R. Astron. Soc., 330, 2002, 58–62.
Melatos, A., Peralta, L., and Wyithe S. B. Avalanche dynmacis of radio pulsar glitches. Astrophysical Journal, 672, 2008, 737–1297.
Onuchukwu, C. C. and Chukwude, A. E. A study of microglitches in Hartebecsthock radio pulsar. Astrophyics& Space Sci., 361, 2016, 1-12.
Wang, N. and Yuan, J. Observation features of pulsar glitches. Science China, 5, 2010, 3-8.
Alpar, M. A. The largest pulsar glitches and the university of glitch behaviour. AIP Confproc., 1379, 2010, 166–174.
Haskell, B., and Melatos, A. Models of pulsar glitches. International Journal of Modern Physics D.24, 2015, 1530008-15300059.
Urama, J. O. and Okeke, P. N. Vela-size glitch rates in youthful pulsars. Mon. Not. R. Astron. Soc., 310, 1999, 313–316.
Wang, N., Manchester, R. N. Pace, R. T., Bailes, M., Kaspi, V. M., Stappers, B. W. and Lyne, A. G. Glitches in Southern Pulsars. Mon Not. R. Astron. Soc., 317, 2000, 843–860.
Janssen, G. H. and Stappers, B. W. 30 glitches in slow pulsars. Astronomy and Astrophysics, 457, 2006, 611–618.
Eya, I. O., Urama, J. O. and Chukwude, A. E. Angular momentum transfer and fractional moment of inertia in pulsar glitches. Astrophysical Journal, 840, 2017, 56-63.
Zou, W. Z., Wang, N., Wang, H. X., Manchester, R. N., Wu, X. J. and Zhang, J. Unusual glitch behaviours of two young pulsars. Mon Not. R. Astron. Soc., 354, 2004, 811-814.
Dib, R., Kaspi, V. M., and Gavriil, F. P. Glitches in anomalous x-ray pulsars. Astrophysical Journal, 673, 2008, 1044-1061.
Shemar, S. L., and Lyne, A. G. Observations of pulsar glitches Mon. Not. R. Astron. Soc., 282, 1996, 677–690.