Neutron star glitches; spanning a period of 42 years of pulsar timing were studied. These glitches are from Radio, X-ray, Anomalous X-ray and Milliseconds Pulsars. Radio Pulsars dominates the glitch events, contributing 87% of the glitches. Pulsars of characteristic age bracket 103 to 105 yrs dominated the glitch events, at a rate of 5.2 glitches per year per pulsar. Pulsar of the above age bracket exhibits large size glitches compared to others. A large frequency spin-up (△v) is generally associated with large frequency derivative jump (△v ̇). The distribution of the glitch magnitude (△v/v) is bimodal reaffirming dual glitch mechanism, but that of spin-up (△v) is tending towards multi-modal. Moreover, glitches in Vela pulsar and PSR J0537-6910 showed strong elasticity of the objects, suggesting that the interiors of these objects are in thermal equilibrium. Glitches from PSR J1740-3015 and PSR J1341-6220 appeared to occur in groups, suggesting that their interior fluid is switching between two phases. We discussed the glitch activity of young pulsars in terms of vortex creep model.
| Published in | International Journal of Astrophysics and Space Science (Volume 2, Issue 2) |
| DOI | 10.11648/j.ijass.20140202.11 |
| Page(s) | 16-21 |
| 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), 2014. Published by Science Publishing Group |
Star, Neutron, Pulsar, Glitch, General
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APA Style
Eya, Innocent Okwudili, Urama, Johnson O. (2014). Statistical Study of Neutron Star Glitches. International Journal of Astrophysics and Space Science, 2(2), 16-21. https://doi.org/10.11648/j.ijass.20140202.11
ACS Style
Eya; Innocent Okwudili; Urama; Johnson O. Statistical Study of Neutron Star Glitches. Int. J. Astrophys. Space Sci. 2014, 2(2), 16-21. doi: 10.11648/j.ijass.20140202.11
AMA Style
Eya, Innocent Okwudili, Urama, Johnson O. Statistical Study of Neutron Star Glitches. Int J Astrophys Space Sci. 2014;2(2):16-21. doi: 10.11648/j.ijass.20140202.11
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Download@article{10.11648/j.ijass.20140202.11,
author = {Eya and Innocent Okwudili and Urama and Johnson O.},
title = {Statistical Study of Neutron Star Glitches},
journal = {International Journal of Astrophysics and Space Science},
volume = {2},
number = {2},
pages = {16-21},
doi = {10.11648/j.ijass.20140202.11},
url = {https://doi.org/10.11648/j.ijass.20140202.11},
eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20140202.11},
abstract = {Neutron star glitches; spanning a period of 42 years of pulsar timing were studied. These glitches are from Radio, X-ray, Anomalous X-ray and Milliseconds Pulsars. Radio Pulsars dominates the glitch events, contributing 87% of the glitches. Pulsars of characteristic age bracket 103 to 105 yrs dominated the glitch events, at a rate of 5.2 glitches per year per pulsar. Pulsar of the above age bracket exhibits large size glitches compared to others. A large frequency spin-up (△v) is generally associated with large frequency derivative jump (△v ̇). The distribution of the glitch magnitude (△v/v) is bimodal reaffirming dual glitch mechanism, but that of spin-up (△v) is tending towards multi-modal. Moreover, glitches in Vela pulsar and PSR J0537-6910 showed strong elasticity of the objects, suggesting that the interiors of these objects are in thermal equilibrium. Glitches from PSR J1740-3015 and PSR J1341-6220 appeared to occur in groups, suggesting that their interior fluid is switching between two phases. We discussed the glitch activity of young pulsars in terms of vortex creep model.},
year = {2014}
}
TY - JOUR T1 - Statistical Study of Neutron Star Glitches AU - Eya AU - Innocent Okwudili AU - Urama AU - Johnson O. Y1 - 2014/05/20 PY - 2014 N1 - https://doi.org/10.11648/j.ijass.20140202.11 DO - 10.11648/j.ijass.20140202.11 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 - 16 EP - 21 PB - Science Publishing Group SN - 2376-7022 UR - https://doi.org/10.11648/j.ijass.20140202.11 AB - Neutron star glitches; spanning a period of 42 years of pulsar timing were studied. These glitches are from Radio, X-ray, Anomalous X-ray and Milliseconds Pulsars. Radio Pulsars dominates the glitch events, contributing 87% of the glitches. Pulsars of characteristic age bracket 103 to 105 yrs dominated the glitch events, at a rate of 5.2 glitches per year per pulsar. Pulsar of the above age bracket exhibits large size glitches compared to others. A large frequency spin-up (△v) is generally associated with large frequency derivative jump (△v ̇). The distribution of the glitch magnitude (△v/v) is bimodal reaffirming dual glitch mechanism, but that of spin-up (△v) is tending towards multi-modal. Moreover, glitches in Vela pulsar and PSR J0537-6910 showed strong elasticity of the objects, suggesting that the interiors of these objects are in thermal equilibrium. Glitches from PSR J1740-3015 and PSR J1341-6220 appeared to occur in groups, suggesting that their interior fluid is switching between two phases. We discussed the glitch activity of young pulsars in terms of vortex creep model. VL - 2 IS - 2 ER -
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