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Start Over Author "Xu, R X" Journal monthly notices of the royal astronomical society
30 results on '"Xu, R X"'

2. The FAST Galactic Plane Pulsar Snapshot Survey – III. Timing results of 30 newly discovered pulsars

Author

Su, W Q, primary, Han, J L, additional, Wang, P F, additional, Yuan, J P, additional, Wang, Chen, additional, Zhou, D J, additional, Wang, Tao, additional, Yan, Yi, additional, Jing, W C, additional, Yang, Z L, additional, Cai, N N, additional, Chen, Xue, additional, Xu, Jun, additional, Xie, Lang, additional, Wang, H G, additional, Xu, R X, additional, and You, X P, additional

Published
2023
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6. Exploring the single-pulse behaviours of PSR J0628+0909 with FAST.

Author

Hsu, J A, Jiang, J C, Xu, H, Lee, K J, and Xu, R X

Subjects
FARADAY effect, PULSARS, RADIO telescopes
Abstract

More than 100 rotating radio transients (RRATs) have been discovered since 2006. However, it is unclear whether RRATs radiate in nulling states. PSR J0628+0909 has been classified as an RRAT. In this paper, we study the single pulses and integrated pulse profile of PSR J0628+0909 to check whether we can detect pulsed radio emission in the nulling states. We also aim to study the polarization of the RRAT and its relationship to the general pulsar population. We used the Five-hundred-meter Aperture Spherical radio Telescope (FAST) to observe PSR J0628+0909 in the frequency range from 1.0 to 1.5 GHz. We searched for strong single pulses and looked for pulsed emission in the RRAT nulling states. Polarization profiles, the single-pulse energy distribution, and waiting-time statistics were measured. The Faraday rotation measure and dispersion measure values are updated with the current observation. The single-pulse polarization behaviours show great diversity, similar to the case of pulsars. Based on the integrated pulse profile and single-pulse energy statistics, we argue that continuous pulsar-like emission exists in addition to the transient-like burst emission for PSR J0628+0909. We find that the pulse waiting time is not correlated with the pulse energy and conclude that the strong transient emission of RRAT is not generated by the energy store–release mechanism. [ABSTRACT FROM AUTHOR]

Published
2023
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10. An in-depth investigation of 11 pulsars discovered by FAST

Author

Cameron, A D, primary, Li, D, primary, Hobbs, G, primary, Zhang, L, primary, Miao, C C, primary, Wang, J B, primary, Yuan, M, primary, Wang, S, primary, Jacobs Corban, G, primary, Cruces, M, primary, Dai, S, primary, Feng, Y, primary, Han, J, primary, Kaczmarek, J F, primary, Niu, J R, primary, Pan, Z C, primary, Qian, L, primary, Tao, Z Z, primary, Wang, P, primary, Wang, S Q, primary, Xu, H, primary, Xu, R X, primary, Yue, Y L, primary, Zhang, S B, primary, Zhi, Q J, primary, Zhu, W W, primary, Champion, D J, primary, Kramer, M, primary, Zhou, S Q, primary, Qiu, K P, primary, and Zhu, M, primary

Published
2020
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11. Piggyback search for fast radio bursts using Nanshan 26 m and Kunming 40 m radio telescopes – I. Observing and data analysis systems, discovery of a mysterious peryton

Author

Men, Y P, primary, Luo, R, additional, Chen, M Z, additional, Hao, L F, additional, Lee, K J, additional, Li, J, additional, Li, Z X, additional, Liu, Z Y, additional, Pei, X, additional, Wen, Z G, additional, Wu, J J, additional, Xu, Y H, additional, Xu, R X, additional, Yuan, J P, additional, and Zhang, C F, additional

Published
2019
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13. A study of multifrequency polarization pulse profiles of millisecond pulsars

Author

Dai, S., primary, Hobbs, G., additional, Manchester, R. N., additional, Kerr, M., additional, Shannon, R. M., additional, van Straten, W., additional, Mata, A., additional, Bailes, M., additional, Bhat, N. D. R., additional, Burke-Spolaor, S., additional, Coles, W. A., additional, Johnston, S., additional, Keith, M. J., additional, Levin, Y., additional, Osłowski, S., additional, Reardon, D., additional, Ravi, V., additional, Sarkissian, J. M., additional, Tiburzi, C., additional, Toomey, L., additional, Wang, H. G., additional, Wang, J.-B., additional, Wen, L., additional, Xu, R. X., additional, Yan, W. M., additional, and Zhu, X.-J., additional

Published
2015
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16. Detection of 107 glitches in 36 southern pulsars

Author

Yu, M., primary, Manchester, R. N., additional, Hobbs, G., additional, Johnston, S., additional, Kaspi, V. M., additional, Keith, M., additional, Lyne, A. G., additional, Qiao, G. J., additional, Ravi, V., additional, Sarkissian, J. M., additional, Shannon, R., additional, and Xu, R. X., additional

Published
2012
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29. Detection of 107 glitches in 36 southern pulsars.

Author

Yu, M., Manchester, R. N., Hobbs, G., Johnston, S., Kaspi, V. M., Keith, M., Lyne, A. G., Qiao, G. J., Ravi, V., Sarkissian, J. M., Shannon, R., and Xu, R. X.

Subjects
PULSAR detection, RADIO telescopes, RADIO frequency, LINEAR systems, PLANETARY magnetospheres, PREDICTION models, NEUTRONS
Abstract

Timing observations from the Parkes 64-m radio telescope for 165 pulsars between 1990 and 2011 have been searched for period glitches. Data spans for each pulsar ranged between 5.3 and 20.8 yr. From the total of 1911 yr of pulsar rotational history, 107 glitches were identified in 36 pulsars. Out of these glitches, 61 have previously been reported whereas 46 are new discoveries. Glitch parameters, both for the previously known and the new glitch detections, were measured by fitting the timing residual data. Observed relative glitch sizes Δνg/ν range between 10−10 and 10−5, where ν = 1/P is the pulse frequency. We confirm that the distribution of Δνg/ν is bimodal with peaks at approximately 10−9 and 10−6. Glitches are mostly observed in pulsars with characteristic ages between 103 and 105 yr, with large glitches mostly occurring in the younger pulsars. Exponential post-glitch recoveries were observed for 27 large glitches in 18 pulsars. The fraction Q of the glitch that recovers exponentially also has a bimodal distribution. Large glitches generally have low Q, typically just a few per cent, but large Q values are observed in both large and small glitches. Observed time constants for exponential recoveries ranged between 10 and 300 d with some tendency for longer time-scales in older pulsars. Shorter time-scale recoveries may exist but were not revealed by our data which typically have observation intervals of 2–4 weeks. For most of the 36 pulsars with observed glitches, there is a persistent linear increase in $\dot{\nu }$ (i.e. decrease in the slow-down rate $|\dot{\nu }|$) in the interglitch interval. Where an exponential recovery is also observed, the effects of this are superimposed on the linear increase in $\dot{\nu }$. In some but not all cases, the slope of the linear recovery changes at the time of a glitch. The $\ddot{\nu }$ values characterizing the linear changes in $\dot{\nu }$ are almost always positive and, after subtracting the magnetospheric component of the braking, are approximately proportional to the ratio of $|\dot{\nu }|$ and the interglitch interval, as predicted by vortex-creep models. [ABSTRACT FROM AUTHOR]

Published
2013
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30. 1E 1207.4−5209: a low-mass bare strange star?

Author

Xu, R. X.

Subjects
*STARS, *COSMIC magnetic fields, *ASTROPHYSICS, *DISKS (Astrophysics), *WHITE dwarf stars, *TELESCOPES, *FERROMAGNETISM
Abstract

Both rotation- and accretion-powered low-mass bare strange stars are studied, with particular regard to their astrophysical appearance. It is suggested that low-mass bare strange stars, with weaker ferromagnetic fields than that of normal pulsars, could result from the accretion-induced collapse of white dwarfs. According to its peculiar timing behaviour, we propose that the radio-quiet object, 1E 1207.4−5209, could be a low-mass bare strange star with a polar surface magnetic field ofand a radius of a few kilometres. The low-mass bare strange star idea is helpful in distinguishing neutron and strange stars, and is testable by imaging pulsar-like stars with the future Constellation-X telescope. [ABSTRACT FROM AUTHOR]

Published
2005
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