The Single-pulse Observation of PSR B2111+46 with the Five-hundred-meter Aperture Spherical Radio Telescope

Zhi, Q. J.; Bai, J. T.; Shang, L. H.; Xu, X.; Dang, S. J.; Li, D.; Zhang, L.; Wang, P.; Xie, X. Y.; Zhao, R. S.; Dong, A. J.; Qiao, G. J.

doi:10.3847/1538-4357/ace362

Cited by 3 publications

(2 citation statements)

References 58 publications

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“…For example, PSR J1926−0652 (Zhang et al 2019) displays complex subpulse drifting across multiple profile components, with irregular P 3 and different drift bands, indicating intricate magnetospheric activities. PSR J1631 + 1252 (Wen et al 2022) and the nulling pulsar PSR B2111 + 46 (Zhi et al 2023) both demonstrate modulated drifting subpulses in their leading components, revealing the local emission properties. In addition, with the switching in the subpulse drift rate and curved drift bands, PSR J1857 + 0057 (Yan et al 2023) highlights the temporal variation in pulsar emission.…”

Section: Comparison With Other Radio Pulsarsmentioning

confidence: 97%

Investigation of Profile Shifting and Subpulse Movement in PSR J0344-0901 with FAST

Tedila,

Yuen,

Wang

et al. 2024

ApJ

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We report two phenomena detected in PSR J0344−0901 from two observations conducted at frequencies centered at 1.25 GHz using the Five-hundred-meter Aperture Spherical Radio Telescope. The first phenomenon manifests as the pulse emission shifting to later longitudinal phases and then gradually returning to its original location. The event lasts for about 216 pulse periods, with an average shift of about 0.°7 measured at the peak of the integrated profile. Changes in the polarization position angle (PPA) are detected around the trailing edge of the profile, together with an increase in the profile width. The second phenomenon is characterized by the apparent movement of subpulses, which results in different subpulse track patterns across the profile window. For the first time in this pulsar, we identify four emission modes, each with unique subpulse movement, and determine the pattern periods for three of them. Pulse nulling was not detected. Modeling of the changes in the PPA using the rotating vector model gives an inclination angle of 75.°12 ± 3.°80 and an impact parameter of −3.°17 ± 5.°32 for this pulsar. We speculate that the subpulse movement may be related to the shifting of the pulse emission.

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Section: Comparison With Other Radio Pulsarsmentioning

confidence: 97%

Investigation of Profile Shifting and Subpulse Movement in PSR J0344-0901 with FAST

Tedila,

Yuen,

Wang

et al. 2024

ApJ

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show abstract

“…As the number of discovered pulsars continues to rise since their first discovery (Hewish et al 1968), advancements in high-sensitivity telescopes have opened avenues for expanding pulsar populations (e.g., Dai et al 2020;Han et al 2021;Zhi et al 2024) and uncovering fascinating phenomena (e.g., Zhi et al 2023b;Chen et al 2023;Zhang et al 2023). This progress has also provided opportunities for in-depth investigations into single pulse features.…”

Section: Introductionmentioning

confidence: 99%

Investigating the Unique Drift Behavior of PSR B2110+27 with FAST

Xu,

Zhi,

Bai

et al. 2024

ApJ

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Careful scrutiny of the single pulse emissions from PSR B2110+27 has been conducted through highly sensitive observations using the Five-hundred-meter Aperture Spherical radio Telescope (FAST) at a central frequency of 1250 MHz. Our investigation revealed significant subpulse drift behavior and nulling in this pulsar. Moreover, we observed that the nulling events tend to be of short duration, with an estimated overall nulling fraction of approximately 27% ± 3%. It is noteworthy that the drift direction of the subpulses exhibits abrupt changes, occasionally transitioning into a steady state or displaying a low drift rate. Analysis using longitude resolved fluctuation spectra indicates the presence of two distinct repetition periods for the pulsar: P 3 = (10.8 ± 2.5)P and P 3 = (31.6 ± 4.2)P, where P denotes the pulsar period. Our investigation revealed that the subpulse separation remains consistent across different drift patterns, with P 2 = 2.°3 ± 0.°2. A more comprehensive analysis indicates that the unique drift behavior observed can be explained by a carousel model of the dipole field. Minor changes in P 2 and drift rate caused significant variations in the apparent P 3 and abrupt shifts in the drift direction, while the true repetition period (assuming first-order aliasing) changed by only ∼10%. We observe a drift band memory and apparent phase memory across the null state in this pulsar, as well as variations in the drift rate and drift direction across the null state, though we have not detected significant periodicity of the nulling itself. This suggests that these phenomena may arise from random null pulses intersecting with the frequently aliased drift bands.

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Studying the nulling, subpulse drifting, and moding in PSR J1921+1948 with the FAST

Shang,

Bai,

et al. 2024

Monthly Notices of the Royal Astronomical Society

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We reported the observations of nulling, subpulse drifting, and moding of radio radiation in pulsar (PSR) B1918+19 at 1250 MHz with the Five-hundred-meter Aperture Spherical radio Telescope. The nulling fraction is 2.6 ± 0.1 per cent and no periodicity of nulling can be seen. We confirmed the existence of three different drift modes (A, B, C) and a disordered mode (N) at 1250 MHz. Unlike the other three modes where the second component of the average pulse profile dominates, the first component of the average pulse profile in mode C is brighter than the other components, the second component shifts forward and the fourth component shifts backward. The bidrifting phenomenon is observed in PSR B1918+19, the drifting of the first and second components is positive, and the drift direction of the fourth component is negative. The drifting rate of the drift bands composed of the first and second components has an obvious evolutionary trend. Mode B has a short duration and no clear trend can be seen. But for mode A, the drift rate of each drift band starts relatively fast, then slows down to a steady state, and finally increases slowly until it enters either null or mode N. Further analysis shows that the emergence and significant variation in the drifting period of multidrifting subpulse emission modes for PSR B1918+19 may be due to the aliasing effect. The interesting subpulse emission phenomenon of PSR B1918+19 at different frequencies provides a unique opportunity to understand the switching mechanism of the multidrift mode of the pulsars.

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The Single-pulse Observation of PSR B2111+46 with the Five-hundred-meter Aperture Spherical Radio Telescope

Cited by 3 publications

References 58 publications

Investigation of Profile Shifting and Subpulse Movement in PSR J0344-0901 with FAST

Investigation of Profile Shifting and Subpulse Movement in PSR J0344-0901 with FAST

Investigating the Unique Drift Behavior of PSR B2110+27 with FAST

Studying the nulling, subpulse drifting, and moding in PSR J1921+1948 with the FAST

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