The drifting subpulse and nulling of PSR B0820 + 02 observed with FAST

Zhi, Qi‐Jun; Xu, Xinmin; Shang, Lun-Hua; Bai, J. T.; Dang, S. J.; Lu, Jiguang; Dai, Shi; Zhao, Ru-Shuang; Wen, Z. G.; Qiao, G. J.; Dong, Ai‐Jun

doi:10.1093/mnras/stad235

Cited by 7 publications

(6 citation statements)

References 42 publications

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“…, a small fluctuation in ¢ P 3 leads to a significant change in P 3 . Many studies have affirmed the behavior of multidrift and the drift direction change of pulsars due to the aliasing effect (e.g., Esamdin et al 2005;Szary et al 2022;Zhi et al 2023a). For PSR B2110+27, Figure 1 shows that its drift band direction consistently changes, indicating that the subpulse drifting behavior is frequently affected by the aliasing effect.…”

Section: Aliasing Effectmentioning

confidence: 99%

“…The gradual establishment and deployment of highly sensitive telescopes are enlarging the catalog of subpulsating drift pulsars. The exceptional quality of these observations is enabling us to discern details that were once indistinguishable (Zhi et al 2023a;Xu et al 2024).…”

Section: Introductionmentioning

confidence: 99%

“…Nonetheless, an increasing body of evidence suggests that the traditional carousel model has limitations. Such as frequent switching of multiple drift modes (Weltevrede 2016;McSweeney et al 2019;Zhi et al 2023a;Xu et al 2024), bidrifting (Qiao et al 2004;Szary et al 2020), abrupt transitions of the drift direction (Biggs et al 1985;Szary et al 2022), etc. All these particular phenomena challenge the traditional carousel model, which means that the model should be extended (Edwards 2006).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Aliasing Effectmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Xu,

Zhi,

Bai

et al. 2024

ApJ

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“…For a long time, only a handful of pulsars were known to exhibit mode changing associated with subpulse drifting, with prominent examples being PSR B0031-07 (Huguenin et al 1970;Vivekanand & Joshi 1997;Smits et al 2005;McSweeney et al 2017), PSR B0809+74 (van Leeuwen et al 2002;Hassall et al 2013;Basu et al 2023a), PSR B0943+10 (Suleymanova et al 1998;Backus et al 2011), PSR B1237+25 (Backer 1970;Srostlik & Rankin 2005), PSR B1918+19 (Hankins & Wolszczan 1987;Rankin et al 2013), PSR B1944+17 (Deich et al 1986;Kloumann & Rankin 2010), PSR B2303+30 (Redman et al 2005), and PSR B2319+60 (Wright & Fowler 1981;Rahaman et al 2021). In recent years, dedicated studies of the single pulse emission from pulsars using instruments like the Giant Metrewave Radio Telescope (GMRT), Murchison Widefield Array, FAST, etc., have found several other examples of subpulse drifting associated with mode changing, e.g., PSR J0026-1955J0026- (McSweeney et al 2022Janagal et al 2023), PSR B0820+02 (Zhi et al 2023), PSR J1110-5637 (Dang et al 2022), PSR J1727-2739 (Wen et al 2016;Basu et al 2021;Rejep et al 2022), PSR B1819-22 (Basu & Mitra 2018a;Janagal et al 2022), and PSR B2003-08 (Basu et al 2019b). In the above list, only three pulsars, PSR B1237+25, PSR B2003-08, and PSR B2319+60, have c Q/M profile types signifying the central LOS traverse across the emission beam.…”

Section: Introductionmentioning

confidence: 99%

Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers

Basu,

Mitra,

Melikidze

2023

ApJ

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We have studied the single pulse emission from two pulsars, PSR B0844-35 and PSR B1758-29, over a wide frequency range of 300–750 MHz using the upgraded Giant Metrewave Radio Telescope. The two pulsars have relatively wide profiles with multiple components, which are a result of the line of sight traversing near the center of the emission beam. In both pulsars, the single pulse sequences show the presence of two distinct emission states, where the profiles become much brighter at the center, with prominent core components during one of the modes, while in the other mode the single pulses show odd–even subpulse drifting with a periodicity of around 2P, P being the rotation period of the pulsar. The centrally bright mode was seen for 10% of the observing duration in PSR B0844-35, which usually lasted for short durations of around 10 pulses, but had two longer sequences of around 100 pulses. On the contrary, the centrally bright mode was dominant in PSR B1758-29 and was seen for around 60% of the observing duration. PSR B1758-29 also showed period amplitude modulations of 60P–70P in both modes. The mode changing in these two pulsars facilitates investigation of the sparking process in the inner acceleration region, dominated by nondipolar magnetic fields. The change in the surface magnetic field configurations likely results in the emission mode change.

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“…In general, subpulse drifting can be represented by three drift parameters: the vertical band spacing at the phase of the same pulse (P 3 ), the horizontal time interval between successive drift bands (P 2 ), and the drift rate (Δf = P 2 /P 3 ). Since its discovery, various unusual behaviors of subpulse drifting have been reported, which have challenged the traditional carrousel circulation models (e.g., Wen et al 2016;Dang et al 2022;Xu et al 2024;Zhi et al 2023). Several studies have found some evidence of a link between nulling and subpulse drifting-for example, the drift rate changes after the null state (van Leeuwen et al 2003;.…”

Section: Introductionmentioning

confidence: 99%

Investigation of Nulling and Subpulse-drifting Properties of PSR J1649+2533 with FAST

Shang,

Xu,

Liu

et al. 2024

ApJ

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We report the nulling and subpulse-drifting properties of PSR J1649+2533 with observations of the Five-hundred-meter Aperture Spherical Radio Telescope (FAST). The FAST observations reveal that the nulling fraction of this pulsar is about 20.9% ± 0.8% at 1250 MHz. The statistical study of the durations of the nulling and burst states shows that the burst states can persist for extended pulse periods, exceeding 100 periods in some cases, while the shortest lasts only a few pulse periods. The null states have a much shorter duration, with a maximum duration of less than 30 pulse periods. A comparative study between the pulse profiles of the first active pulse (FAP) and the last active pulse (LAP) shows that the pulse profiles of LAPs are stronger and wider than those of FAPs. An analysis of the two-dimensional fluctuation spectrum for the single-pulse stack indicates that the pulsar exhibits clear amplitude modulation and subpulse drifting. The periods are a P 3 = 2.5 ± 0.1 spin period and P 2 = 17.°0 ± 0.°5 at 1250 MHz, respectively. In addition, the multiband investigation shows that P 2 seems to increase with the increase of the observing frequency, i.e., P 2 ∝ ν 0.8±0.1. This seems to be caused by the increasing pulse-profile width with the frequency. The high-sensitivity FAST observations will enable a detailed understanding of the emission of this pulsar and provide important clues for theoretical studies of the radiation mechanism.

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The drifting subpulse and nulling of PSR B0820 + 02 observed with FAST

Cited by 7 publications

References 42 publications

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

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

Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers

Investigation of Nulling and Subpulse-drifting Properties of PSR J1649+2533 with FAST

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