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The 2016 glitch in the Vela pulsar

  • Y. H. Xu
  • J. P. YuanEmail author
  • K. J. Lee
  • L. F. Hao
  • N. Wang
  • M. Wang
  • M. Yu
  • Z. X. Li
  • Y. L. Yue
  • Z. Y. Liu
  • R. Yuen
  • Z. G. Wen
  • S. J. Dang
  • J. M. Bai
  • W. Chen
  • Y. X. Huang
  • W. M. Yan
Original Article
  • 29 Downloads

Abstract

We report the detection of a glitch event in the Vela pulsar, which occurred on 12 December 2016, based on the timing data obtained from observations between January 2016 and February 2018 at frequency centered at 2256 MHz using the Kunming 40-m radio telescope. The timing solutions for the pre- and post-glitch are presented. By fitting the glitch model to the timing data, we found that the post-glitch recovery exhibits two terms with exponential decay with the time scales of 1 d and 6 d, respectively. The glitch parameters are determined with \(\Delta \nu _{\mathrm{g}}/\nu =1.431(2)\times 10^{-6}\) and \(\Delta \dot{\nu }_{\mathrm{g}}/\dot{\nu }=73.354\times 10^{-3}\). The value of the coupling parameter is calculated to be ∼0.08, implying that the core superfluid is probably not involved in this event. For the glitches with two or more terms with exponential decay in the Vela pulsar, we show that the exponential decays usually exhibit longer time scales with higher degree of glitch recovery. The post-glitch behavior in the slow-down rate \(|\dot{\nu }|\) is dominated by a linear decrease process. From detection of the variations in the slopes of the spin-down rates after the exponential recoveries of the 2013 and 2016 glitches, we conclude that no persistent shift was involved in the 2016 glitches.

Keywords

Pulsars: individual (PSR B0833-45, J0835-4510) Stars: neutron Radio: stars 

Notes

Acknowledgements

This work was supported by Strategic Priority Research Programme of Chinese Academy of Sciences (XDB23010200), the National Natural Science Foundation of China (U1531243, U1631237, 11573059, 11873080), the National Key R&D Program of China (No. 2017YFA0402602), and Open Fund of Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing. The Kunming 40-m Telescope is jointly operated and administrated by Yunnan Astronomical Observatory and Center for Astronomical Mega-Science, Chinese Academy of Sciences. The Parkes Test-Bed Facility is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by the Commonwealth Scientific and Industrial Research Organisation (CSIRO).

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  • Y. H. Xu
    • 1
    • 4
    • 5
    • 6
  • J. P. Yuan
    • 2
    • 7
    • 9
    Email author
  • K. J. Lee
    • 3
  • L. F. Hao
    • 1
    • 5
  • N. Wang
    • 2
  • M. Wang
    • 1
    • 5
  • M. Yu
    • 8
  • Z. X. Li
    • 1
    • 5
    • 6
  • Y. L. Yue
    • 8
  • Z. Y. Liu
    • 2
  • R. Yuen
    • 10
    • 2
  • Z. G. Wen
    • 2
  • S. J. Dang
    • 2
  • J. M. Bai
    • 1
    • 5
  • W. Chen
    • 1
    • 5
    • 6
  • Y. X. Huang
    • 1
    • 5
  • W. M. Yan
    • 2
  1. 1.Yunnan ObservatoriesChinese Academy of SciencesKunmingChina
  2. 2.Xinjiang Astronomical ObservatoryChinese Academy of SciencesUrumqiChina
  3. 3.Kavli Institute for Astronomy and AstrophysicsPeking UniversityBeijingChina
  4. 4.Guizhou Provincial Key Laboratory for Radio Astronomy and Data ProcessingGuiyangChina
  5. 5.Key Laboratory for Structure and Evolution of Celestial ObjectsChinese Academy of SciencesKunmingChina
  6. 6.University of Chinese Academy of SciencesBeijingChina
  7. 7.Center for Astronomical Mega-ScienceChinese Academy of SciencesBeijingP.R. China
  8. 8.National Astronomical ObservatoriesChinese Academy of SciencesBeijingChina
  9. 9.Key Laboratory of Radio AstronomyChinese Academy of ScienceNanjingChina
  10. 10.Key Laboratory of Radio AstronomyChinese Academy of ScienceUrumqiChina

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