Abstract
We present analysis of the timing noise in PSR J1733−3716, which combines data from Parkes 64-m radio telescope and nearly 15 years of timing data obtained from the Nanshan 25-m radio telescope. The variations in the spin frequency and frequency derivative are determined. The fluctuation in the spin frequency is obvious with an amplitude of \(1.94(7)\times 10^{-9}\text{ Hz}\). Variations of the integrated profile at 1369 MHz are detected with the changes occur in the relative peak intensity from the right profile component. From analysis of the single pulse data at 1382 MHz, we detect weak emission states that account for 63% of the whole data, and its duration distribution can be fitted with a power law. The pulsar also exhibits strong emission states, during which the emission shows multiple modes. This includes the normal mode, left mode and the right mode, with the time scales spanning between one and seventeen pulse periods. Such short term variability in pulses contributes to the variation of the integrated profile. Examination of the correlations between the spin parameters and the integrated profiles shows likelihood of a random distribution, which reveals that there is probably no obvious relationship between spin-down rate variations and changes of emission in this pulsar.
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Acknowledgements
This work was supported by the National Key R&D Program of China (No. 2017YFA0402602), the National Natural Science Foundation of China (11563008, 11873080, 11573059), JY acknowledges supports from Center for Astronomical Mega-Science, Chinese Academy of Sciences. RY is supported by the West Light Foundation of the Chinese Academy of Sciences, project 2016-QNXZ-B-24. We are grateful to Feifei Kou for valuable suggestions, and Zhigang Wen for helpful discussion. The Parkes radio telescope is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO.
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Hu, Y., Li, L., Yuan, J.P. et al. Timing and emission variation of PSR J1733−3716. Astrophys Space Sci 365, 143 (2020). https://doi.org/10.1007/s10509-020-03849-8
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DOI: https://doi.org/10.1007/s10509-020-03849-8