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Spin-down and emission variations for PSR J0742-2822

             

摘要

PSR J0742-2822 is known for its quasi-periodic changes in the observed pulse profile and spindown rate.In this paper,we analyzed 13 years of timing data obtained with the Nanshan 25-m radio telescope and the Parkes 64-m radio telescope.We found that the average values of the spin-down rate((v))of this pulsar changed in four different states.We investigated the correlation between v and W50,and ascertained that the correlation changed in different states.Moreover,not all the changes in states and correlation can be associated with glitch activities.We examined the long term evolution ofγ-ray flux(0.1-300 GeV)and the pulse profiles corresponding to the four different states using Fermi-LAT Pass8(P8 R3)data from 2008 August 5 to 2019 October 1.We did not detect a significant change inγ-ray flux or the pulse profile.Our results suggest that the connection between pulsar rotation and emission is more complex than previously reported for this pulsar.

著录项

  • 来源
    《天文和天体物理学研究》 |2021年第2期|142-148|共7页
  • 作者单位

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    University of Chinese Academy of Sciences 19A Yuquan Road Beijing 100049 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    CAS Key Laboratory of FAST National Astronomical Observatories Chinese Academy of Sciences Beijing 100101 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang 550001 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    University of Chinese Academy of Sciences 19A Yuquan Road Beijing 100049 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    School of Physics Huazhong University of Science and Technology Wuhan 430074 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    School of Electronic and Optical Engineering Nanjing University of Science and Technology Nanjing 210094 China;

    CAS Key Laboratory of FAST National Astronomical Observatories Chinese Academy of Sciences Beijing 100101 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing 100049 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing 210008 China;

    Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi 830011 China;

    University of Chinese Academy of Sciences 19A Yuquan Road Beijing 100049 China;

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