Statistical Study of Glitch Behaviours of Glitching Pulsars

Christian Ikechukwu Eze; Evaristus Uzochukwu Iyida; Finbarr Chidi Odo; Johnson Ozoemena Urama

doi:doi:10.11648/j.ijass.20180604.11

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Statistical Study of Glitch Behaviours of Glitching Pulsars

Christian Ikechukwu Eze, Evaristus Uzochukwu Iyida, Finbarr Chidi Odo, Johnson Ozoemena Urama

Published in International Journal of Astrophysics and Space Science (Volume 6, Issue 4)

Received: 12 September 2018 Accepted: 28 September 2018 Published: 25 October 2018

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Abstract

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 = 10⁴ yr and decays with age for older pulsars with τ ≥ 10⁴yr. The angular momentum transfer resulting to glitches appears to be maximum at youthful age (≈ 10⁴-10⁶yr) 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.

Published in	International Journal of Astrophysics and Space Science (Volume 6, Issue 4)
DOI	10.11648/j.ijass.20180604.11
Page(s)	62-72
Creative Commons	This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.
Copyright	Copyright © The Author(s), 2018. Published by Science Publishing Group

Keywords

Pulsar, General- Stars, Neutron-Methods, Statistical

References

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APA Style

Christian Ikechukwu Eze, Evaristus Uzochukwu Iyida, Finbarr Chidi Odo, Johnson Ozoemena Urama. (2018). Statistical Study of Glitch Behaviours of Glitching Pulsars. International Journal of Astrophysics and Space Science, 6(4), 62-72. https://doi.org/10.11648/j.ijass.20180604.11

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ACS Style

Christian Ikechukwu Eze; Evaristus Uzochukwu Iyida; Finbarr Chidi Odo; Johnson Ozoemena Urama. Statistical Study of Glitch Behaviours of Glitching Pulsars. Int. J. Astrophys. Space Sci. 2018, 6(4), 62-72. doi: 10.11648/j.ijass.20180604.11

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AMA Style

Christian Ikechukwu Eze, Evaristus Uzochukwu Iyida, Finbarr Chidi Odo, Johnson Ozoemena Urama. Statistical Study of Glitch Behaviours of Glitching Pulsars. Int J Astrophys Space Sci. 2018;6(4):62-72. doi: 10.11648/j.ijass.20180604.11

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@article{10.11648/j.ijass.20180604.11,
  author = {Christian Ikechukwu Eze and Evaristus Uzochukwu Iyida and Finbarr Chidi Odo and Johnson Ozoemena Urama},
  title = {Statistical Study of Glitch Behaviours of Glitching Pulsars},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {6},
  number = {4},
  pages = {62-72},
  doi = {10.11648/j.ijass.20180604.11},
  url = {https://doi.org/10.11648/j.ijass.20180604.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20180604.11},
  abstract = {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 = 104 yr and decays with age for older pulsars with τ ≥ 104yr. The angular momentum transfer resulting to glitches appears to be maximum at youthful age (≈ 104-106yr) 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.},
 year = {2018}
}

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TY  - JOUR
T1  - Statistical Study of Glitch Behaviours of Glitching Pulsars
AU  - Christian Ikechukwu Eze
AU  - Evaristus Uzochukwu Iyida
AU  - Finbarr Chidi Odo
AU  - Johnson Ozoemena Urama
Y1  - 2018/10/25
PY  - 2018
N1  - https://doi.org/10.11648/j.ijass.20180604.11
DO  - 10.11648/j.ijass.20180604.11
T2  - International Journal of Astrophysics and Space Science
JF  - International Journal of Astrophysics and Space Science
JO  - International Journal of Astrophysics and Space Science
SP  - 62
EP  - 72
PB  - Science Publishing Group
SN  - 2376-7022
UR  - https://doi.org/10.11648/j.ijass.20180604.11
AB  - 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 = 104 yr and decays with age for older pulsars with τ ≥ 104yr. The angular momentum transfer resulting to glitches appears to be maximum at youthful age (≈ 104-106yr) 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.
VL  - 6
IS  - 4
ER  -

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Author Information

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

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Plain Text BibTeX RIS

APA Style

Christian Ikechukwu Eze, Evaristus Uzochukwu Iyida, Finbarr Chidi Odo, Johnson Ozoemena Urama. (2018). Statistical Study of Glitch Behaviours of Glitching Pulsars. International Journal of Astrophysics and Space Science, 6(4), 62-72. https://doi.org/10.11648/j.ijass.20180604.11

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ACS Style

Christian Ikechukwu Eze; Evaristus Uzochukwu Iyida; Finbarr Chidi Odo; Johnson Ozoemena Urama. Statistical Study of Glitch Behaviours of Glitching Pulsars. Int. J. Astrophys. Space Sci. 2018, 6(4), 62-72. doi: 10.11648/j.ijass.20180604.11

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AMA Style

Christian Ikechukwu Eze, Evaristus Uzochukwu Iyida, Finbarr Chidi Odo, Johnson Ozoemena Urama. Statistical Study of Glitch Behaviours of Glitching Pulsars. Int J Astrophys Space Sci. 2018;6(4):62-72. doi: 10.11648/j.ijass.20180604.11

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@article{10.11648/j.ijass.20180604.11,
  author = {Christian Ikechukwu Eze and Evaristus Uzochukwu Iyida and Finbarr Chidi Odo and Johnson Ozoemena Urama},
  title = {Statistical Study of Glitch Behaviours of Glitching Pulsars},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {6},
  number = {4},
  pages = {62-72},
  doi = {10.11648/j.ijass.20180604.11},
  url = {https://doi.org/10.11648/j.ijass.20180604.11},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20180604.11},
  abstract = {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 = 104 yr and decays with age for older pulsars with τ ≥ 104yr. The angular momentum transfer resulting to glitches appears to be maximum at youthful age (≈ 104-106yr) 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.},
 year = {2018}
}

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TY  - JOUR
T1  - Statistical Study of Glitch Behaviours of Glitching Pulsars
AU  - Christian Ikechukwu Eze
AU  - Evaristus Uzochukwu Iyida
AU  - Finbarr Chidi Odo
AU  - Johnson Ozoemena Urama
Y1  - 2018/10/25
PY  - 2018
N1  - https://doi.org/10.11648/j.ijass.20180604.11
DO  - 10.11648/j.ijass.20180604.11
T2  - International Journal of Astrophysics and Space Science
JF  - International Journal of Astrophysics and Space Science
JO  - International Journal of Astrophysics and Space Science
SP  - 62
EP  - 72
PB  - Science Publishing Group
SN  - 2376-7022
UR  - https://doi.org/10.11648/j.ijass.20180604.11
AB  - 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 = 104 yr and decays with age for older pulsars with τ ≥ 104yr. The angular momentum transfer resulting to glitches appears to be maximum at youthful age (≈ 104-106yr) 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.
VL  - 6
IS  - 4
ER  -

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