Subpulse Drifting of PSR J1110–5637

Dang, S. J.; Shang, Lun-Hua; Lei, Lin; Zhi, Qi‐Jun; Zhao, Ru-Shuang; Chenbin, Wu; You, Yi Zi; Dong, Ai‐Jun; Bai, J. T.; Xu, Xin; Zhang, Dandan; Yang, Hyunah; Quan-Wei, Lin

doi:10.1088/1674-4527/ac6aab

Cited by 4 publications

(2 citation statements)

References 57 publications

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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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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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“…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

Zhi

Shang

et al. 2023

Monthly Notices of the Royal Astronomical Society

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PSR B0820 + 02 is known to exhibit the subpulse drifting phenomenon, which carries vital information about the pulsar radiation process. In this work, we studied the subpulse drifting of PSR B0820 + 02 at a central frequency of 1250 MHz using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Thanks to the superior sensitivity of FAST, we found that PSR B0820 + 02 shows four distinct subpulse drifting modes (A, B, C, and D), the last three of which have not been reported before. The drifting periodicities of these four modes are found to be 4.3P1, 6.4P1, 8.2P1, and 10.3P1 (P1 is the pulse period), respectively. No null pulse is found in our FAST observation. By comparing the energy distribution of single pulses of all four modes, we found that mode A has the highest energy and mode D has the lowest energy. Finally, we interpreted the drift modes in terms of the carousel model, and showed that if B0820 + 02’s different drift modes are due to aliasing effects, the carousel rotation period of P4 lies in the range 29P1–33P1. The new subpulse drifting phenomena of PSR B0820 + 02 reported here provide a unique opportunity for understanding the mechanism and radiation geometry of pulsar radio radiation.

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Subpulse Drifting of PSR J1110–5637

Cited by 4 publications

References 57 publications

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

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

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

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