International Journal of Astrophysics and Space Science

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Statistical Study of Neutron Star Glitches

Received: 11 April 2014    Accepted: 04 May 2014    Published: 20 May 2014
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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.

DOI 10.11648/j.ijass.20140202.11
Published in International Journal of Astrophysics and Space Science (Volume 2, Issue 2, April 2014)
Page(s) 16-21
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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), 2024. Published by Science Publishing Group

Keywords

Star, Neutron, Pulsar, Glitch, General

References
[1] Maran, S.P. 1992, The Astronomy and Astrophysics Encyclopedia, Van Nostrand Reinhold, New York
[2] Gold, T., Rotating Neutron Stars as the Origin of the Pulsating Radio Sources. Nature, 1968, 218, 416
[3] McKenna, J. Lyne, A. G. PSR1737 - 30 and period discontinuities in young pulsars. Nature, 1990, 343, 349
[4] Baym, G., Pethick, C., Pines, D., Ruderman, M., Spin up in neutron stars: The future of the Vela pulsar. Nature,1969, 224, 872
[5] Wang, N., Manches-ter, R.N., Pace, R.T., Glitches in southern pulsars. MINRAS, 2000, 317, 843
[6] Espinoza, C.M., Lyne, A.G., Stappers, B.W, Kramer, M., A study of 315 glitches in the rotation of 102 pulsars 2011, MNRAS, 414, 1679.
[7] Ruderman, M., Neutron Star quakes and pulsar periods. 1969, Nature 223, 597
[8] Ruderman, M., Neutron Star crustal plate tectonics. I - Magnetic dipole evolution in millisecond pulsars and low-mass X-ray binaries. ApJ, 1991, 366, 261
[9] Ruderman, M., Zhu T., Chen K., Neutron Star Magnetic Field Evolution, Crust Move-ment, and Glitches. ApJ, 1998, 492, 267
[10] Anderson, P.W., Itoh, N., Pulsar glitches and res-tlessness as a hard superfluidity phenomenon. Nature, 1975, 256, 25
[11] Ruderman, M., Crust-breaking by neutron superfluids and the VELA pulsar glitches. ApJ, 1976, 203, 213
[12] Alpar, M. A., Anderson, P.W., Pines, D., Shaham, J., Giant glitches and pinned vorticity in the VELA and other pulsars. ApJ, 1981, 249, l29
[13] Urama, J. O., Okeke, P. N. Vela-size glitch rates in youthful pulsars. MNRAS, 1999, 310, 313
[14] Lyne, A. G., Hobbs, G., Kramar, M., Strirs I., Stappers, B., Switched Magnetospheric Regulation of Pulsar Spin-Down. Science, 2010, 329, 408
[15] Dib, R., Kaspi, V.M., Grviil, F.P., Glitches in Anomalous X-ray Pulsars. , ApJ, 2008 673, 1044
[16] Link, B., K., Epstein, R., I., Thermally Driven Neutron Star Glitches. ApJ, 1996, 457, 844
[17] Alpar, M. A., Chau, H. F., Cheng, K. S., Pines, D., Postglitch Relaxation of the Crab Pulsar after Its First Four Major Glitches: The Combined Effects of Crust Cracking, Formation of Vortex Depletion Region and Vortex Creep. 1996, ApJ, 459, 706
[18] Comella, J. M., Craft H. D., Lovelace, R. V. E., Sutton, J. M., Tyler G. L., Crab Nebula Pulsar NP 0532. Nature, 1969, 221, 453
[19] Aschenbach, B., Egger R., Trumper J., Discovery of explosion fragments outside the Vela supernova remnant shock-wave boundary. Nature, 1995, 373, 587
[20] Marshall, F. E., Gotthelf, E. V., Zhang W., Middleditch, J., Wang Q. D., Discovery of an Ultrafast X-Ray Pulsar in the Supernova Remnant N157B. ApJ, 1998, 499, L179
[21] Link, B., Epstein, R.I., Lattimer, J.M. Pulsar Constraints on Neutron Star Structure and Equation of State. Phys. Rev Lett., 1999, 83, 3362
[22] Middleditch, J., Marshall, F. E.,Wang, Q. D., Gotthelf, E. V., Zhang W., Predicting the Starquakes in PSR J0537-6910. 2006, ApJ, 652, 153.
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    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

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    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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    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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  • @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://download.sciencepg.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}
    }
    

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  • 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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