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Timing irregularities of PSR J1705–1906

  • Y. L. Liu
  • J. P. Yuan
  • J. B. Wang
  • X. W. Liu
  • N. Wang
  • R. Yuen
Original Article
  • 74 Downloads

Abstract

Timing analysis of PSR J1705–1906 using data from Nanshan 25-m and Parkes 64-m radio telescopes, which span over fourteen years, shows that the pulsar exhibits significant proper motion, and rotation instability. We updated the astrometry parameters and the spin parameters of the pulsar. In order to minimize the effect of timing irregularities on measuring its position, we employ the Cholesky method to analyse the timing noise. We obtain the proper motion of \(-77(3)\) mas yr−1 in right ascension and \(-38(29)\) mas yr−1 in declination. The power spectrum of timing noise is analyzed for the first time, which gives the spectral exponent \(\alpha =-5.2\) for the power-law model indicating that the fluctuations in spin frequency and spin-down rate dominate the red noise. We detect two small glitches from this pulsar with fractional jump in spin frequency of \(\Delta \nu /\nu \sim 2.9 \times 10^{-10}\) around MJD 55199 and \(\Delta \nu /\nu \sim 2.7\times 10^{-10}\) around MJD 55953. Investigations of pulse profile at different time segments suggest no significant changes in the pulse profiles around the two glitches.

Keywords

Stars: neutron Pulsars: general Pulsars: individual(PSR J1705–1906) 

Notes

Acknowledgements

This work is supported by West light Foundation of CAS, Grant No. XBBS201421; Strategic Priority Research Programme of Chinese Academy of Sciences, Grant No. XDB23010200; and National Natural Science Foundation of China (NSFC No. U1531137, 11373011). The FAST Fellowship is supported by Special Funding for Advanced Users, budgeted and administrated by Center for Astronomical Mega-Science, Chinese Academy of Sciences (CAMS). JBW acknowledges support from NSFC, Grant 11403086, U1431107, 11573059). NW is supported by National Basic Research Program of China (2015CB857100), the National Program on Key Research and Development Project, Grant No. 2016YFA0400804. RY acknowledges supports from NSFC Project no. 11573059, and the West Light Foundation of the Chinese Academy of Sciences, project 2016-QNXZ-B-24.

This work is based on observations made with the Urumqi Nanshan 25 m Telescope, which is operated by XAO and the Key Laboratory of Radio Astronomy, Chinese Academy of Sciences. The Parkes radio telescope 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 Organization.

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Copyright information

© Springer Science+Business Media B.V., part of Springer Nature 2018

Authors and Affiliations

  • Y. L. Liu
    • 1
    • 2
  • J. P. Yuan
    • 2
    • 3
    • 4
  • J. B. Wang
    • 2
    • 4
  • X. W. Liu
    • 1
  • N. Wang
    • 2
    • 3
    • 4
  • R. Yuen
    • 2
    • 3
  1. 1.School of PhysicsChina West Normal UniversityNanchongChina
  2. 2.Xinjiang Astronomical ObservatoryCASUrumqiChina
  3. 3.Key Laboratory of Radio AstronomyChinese Academy of SciencesNanjingChina
  4. 4.Xinjiang Key Laboratory of Radio AstrophysicsUrumqiChina

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