pith. machine review for the scientific record. sign in

arxiv: 2604.09987 · v1 · submitted 2026-04-11 · 🌌 astro-ph.HE

Recognition: unknown

To understand the radiative processes of pulsars and fast radio bursts with the FAST

Wei-Yang Wang , Shunshun Cao , Zhipeng Huang , Jiguang Lu , Yunpeng Men , Lingqi Meng , Jiarui Niu , Zhichen Pan
show 34 more authors
Pengfei Wang Dejiang Zhou Yi Feng Jinlin Han Jinchen Jiang Bin Liu Rui Luo Honguang Wang Shuangqiang Wang Tao Wang Zhengli Wang Heng Xu Jiangwei Xu Renxin Xu Yonghua Xu Yi Yan Zhen Yan Yukai Zhou Siyuan Chen Yinfeng Dai Mingyu Ge Zejun Jiang Kejia Lee Yujie Lian Kuo Liu Lei Qian Hao Tong Lin Wang Yujie Wang Zihao Xu Jumei Yao Dejiang Yin Li Zhang Weiwei Zhu
Authors on Pith no claims yet

Pith reviewed 2026-05-10 16:40 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords pulsarsfast radio burstsradiative processescoherent radio emissionobservational insightsradio astronomy dataemission mechanisms
0
0 comments X

The pith

Observations from a highly sensitive radio telescope are providing pivotal insights into the radiative processes of pulsars and fast radio bursts.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper reviews how advanced radio observations illuminate the mechanisms behind coherent radio emission from pulsars and fast radio bursts. It notes that fast radio bursts share traits with pulsar single pulses, opening a path to address a long-standing puzzle in emission physics. By examining these connections, the work positions the new data as a bridge between the two phenomena. This perspective highlights the value of continued high-sensitivity observations to refine understanding of the shared processes.

Core claim

The central claim is that observational breakthroughs from the telescope are providing pivotal insights to unravel the underlying physics of pulsars and fast radio bursts, especially by linking their single-pulse and burst behaviors to the mystery of coherent radio emission.

What carries the argument

The similarity between pulsar single-pulse behavior and fast radio burst events, which the review positions as the bridge for deciphering the radiative mechanisms.

If this is right

  • Unified models of coherent radio emission can incorporate the shared characteristics of pulsars and fast radio bursts.
  • The long-standing enigma of the emission mechanism may yield to resolution through these linked observations.
  • Further studies are positioned to build directly on the new perspective connecting the two classes of sources.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar high-sensitivity data could be applied to other radio transients to test for common emission traits.
  • The approach suggests multi-wavelength follow-up might reveal additional constraints on the physics.
  • If the connections hold, they could guide targeted searches for rare events that distinguish between competing emission models.

Load-bearing premise

The reviewed observations represent genuine breakthroughs capable of significantly advancing understanding of the radiative mechanisms rather than serving as incremental data points.

What would settle it

If modeling based on the reported observational features fails to produce consistent matches with theoretical predictions for coherent emission, or if subsequent data sets show no unifying patterns between pulsar pulses and bursts, the claim of pivotal insights would not hold.

Figures

Figures reproduced from arXiv: 2604.09987 by Bin Liu, Dejiang Yin, Dejiang Zhou, Hao Tong, Heng Xu, Honguang Wang, Jiangwei Xu, Jiarui Niu, Jiguang Lu, Jinchen Jiang, Jinlin Han, Jumei Yao, Kejia Lee, Kuo Liu, Lei Qian, Lingqi Meng, Lin Wang, Li Zhang, Mingyu Ge, Pengfei Wang, Renxin Xu, Rui Luo, Shuangqiang Wang, Shunshun Cao, Siyuan Chen, Tao Wang, Weiwei Zhu, Wei-Yang Wang, Yi Feng, Yinfeng Dai, Yi Yan, Yonghua Xu, Yujie Lian, Yujie Wang, Yukai Zhou, Yunpeng Men, Zejun Jiang, Zhengli Wang, Zhen Yan, Zhichen Pan, Zhipeng Huang, Zihao Xu.

Figure 1
Figure 1. Figure 1: The distributions of flux densities and luminosities of pulsars observed by FAST. In the left panel, the [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: GC pulsar discoveries from Paulo’s GC pulsar catalog (https://www3.mpifr [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Mean pulse profiles with diverse polarization. In the bottom panels, the black solid, red dashed and [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: the mean pulse profile of PSR B0950+08 over the number of about 36000 individual pulses [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Radio emission feature of PSR B1929+10 based on the conventional baseline subtraction. (a) The [PITH_FULL_IMAGE:figures/full_fig_p013_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Integrated polarization profiles of some millisecond pulsars. Panel (a) presents the position angle curve, [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FAST detection of a dwarf pulse in a series pulses of B2111+46. (a) A segment of pulse trains of PSR [PITH_FULL_IMAGE:figures/full_fig_p015_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Dwarf pulses of PSR B2111+46 as a distinct population from the partial nulling and normal pulses. [PITH_FULL_IMAGE:figures/full_fig_p016_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: A single pulse of B1919+21 from [73], with PA (𝜓), EA (𝜒) and total intensity 𝐼 plotted in two frequency subbands (1000–1125 MHz in green and 1375–1500 MHz in orange). In the 𝐼 panel, the intensity curves are normalized to the maximum values separately for two subbands. Black line—total intensity (𝐼); red dashed line—linear polarization intensity (𝐿 = √︀ 𝑄2 + 𝑈2); blue line—circular polarization intensity … view at source ↗
Figure 10
Figure 10. Figure 10: Three examples for the anomalous-filled mode, which combines the new leading component in the [PITH_FULL_IMAGE:figures/full_fig_p020_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Average polarization properties of mode A (red) and mode B (blue). Solid lines show the total [PITH_FULL_IMAGE:figures/full_fig_p021_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Longitude-resolved fluctuation spectra (LRFS) for 10 MSPs, with the average pulse profile overlaid [PITH_FULL_IMAGE:figures/full_fig_p021_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Distribution of polarization degree for 56 CPTA pulsars. The panels from left to right show the [PITH_FULL_IMAGE:figures/full_fig_p023_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Hard X-ray light curves and spectral evolution of the burst from SGR J1935+2154 associated with [PITH_FULL_IMAGE:figures/full_fig_p025_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Polarization profiles and dynamic spectra of one burst from GPM 1839-10. Top panel: PA of linear [PITH_FULL_IMAGE:figures/full_fig_p027_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: The 𝑃–𝑃˙ diagram of currently known pulsars. The horizontal axis shows the pulsar spin period, while the vertical axis represents the spin-period derivative. All pulsars are indicated by black dots. Pulsars in binary systems are highlighted by red circles, isolated neutron stars with X-ray emission by green pentagrams, RRATs by light-blue squares, pulsars with anomalous X-ray emission or soft 𝛾-ray emissi… view at source ↗
Figure 17
Figure 17. Figure 17: The timing residuals of PSR J1946+2052. The blue, orange, green, and red residuals correspond to [PITH_FULL_IMAGE:figures/full_fig_p032_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Mass-mass diagram for PSR J1946+2052. The regions consistent with the measured orbital decay [PITH_FULL_IMAGE:figures/full_fig_p033_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Basic parameters for 8 one-off FRBs discovered by FAST in the GPPS survey (solid star) [ [PITH_FULL_IMAGE:figures/full_fig_p034_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: The dynamic spectra of four bursts illuminating the difficulty to determine DMs. In the upper [PITH_FULL_IMAGE:figures/full_fig_p036_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Data distributions of emission peak frequency ( [PITH_FULL_IMAGE:figures/full_fig_p037_21.png] view at source ↗
Figure 22
Figure 22. Figure 22: Polarization degree statistics of repeating bursts observed by FAST. The X-axis represents the degree [PITH_FULL_IMAGE:figures/full_fig_p039_22.png] view at source ↗
Figure 23
Figure 23. Figure 23: Long time scale evolution of RM in repeating FRBs. [PITH_FULL_IMAGE:figures/full_fig_p040_23.png] view at source ↗
Figure 24
Figure 24. Figure 24: Polarization profiles and dynamic spectra from FRB 20180301A[ [PITH_FULL_IMAGE:figures/full_fig_p042_24.png] view at source ↗
Figure 25
Figure 25. Figure 25: Phenomenological models of pulsar radio emission beams. Left: the conal beam model [ [PITH_FULL_IMAGE:figures/full_fig_p043_25.png] view at source ↗
Figure 26
Figure 26. Figure 26: The radiation geometry (a), radiation frequency (b), emission beam (c) and resulted pulse profile [PITH_FULL_IMAGE:figures/full_fig_p044_26.png] view at source ↗
Figure 27
Figure 27. Figure 27: Schematic diagram of magnetospheric radiations. The blue solid lines denote low-frequency waves. [PITH_FULL_IMAGE:figures/full_fig_p048_27.png] view at source ↗
read the original abstract

The radiative mechanism of coherent radio emission has remained an enigma since the discovery of pulsars, even the emergence of fast radio bursts (FRBs), which exhibit similarities to the single-pulse behavior of pulsars and have opened a new view for deciphering the long-standing mystery. Besides tremendous efforts in modelling, advanced facilities matter for solving the problem. The authors review the observational breakthroughs from the Five-hundred-meter Aperture Spherical radio Telescope (FAST), which are providing pivotal insights to unravel the underlying physics of pulsars and FRBs. This study offers a novel perspective in the era when pulsars meet FRBs, and further investigations are encouraged to utilize the highly sensitive telescope, the FAST.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 3 minor

Summary. The manuscript is a review summarizing published observational results from the Five-hundred-meter Aperture Spherical radio Telescope (FAST) on pulsar single-pulse behavior, polarization, spectral features, and FRB properties. It claims these high-sensitivity data supply pivotal insights into the long-standing problem of coherent radio emission mechanisms shared by pulsars and FRBs, and it encourages additional FAST observations to advance the field.

Significance. If the cited FAST results are accurately and comprehensively summarized, the review could usefully collate recent high-sensitivity data in one place, underscoring observational synergies between pulsars and FRBs. This may help guide future modeling and observing strategies, though its impact is limited by the absence of new derivations, quantitative comparisons, or falsifiable predictions.

minor comments (3)
  1. [Abstract] Abstract: the statement that FAST observations are 'providing pivotal insights to unravel the underlying physics' is asserted without a concrete example in the abstract of how a specific FAST measurement (e.g., a polarization swing or spectral index) constrains a particular emission model; this should be illustrated briefly.
  2. [Title] The title is grammatically awkward; consider rephrasing to 'Understanding the Radiative Processes of Pulsars and Fast Radio Bursts with FAST Observations'.
  3. As a review, the manuscript should explicitly state its scope (e.g., which FAST pulsar and FRB papers are covered and which are omitted) to allow readers to assess completeness.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful review and recommendation for minor revision. The manuscript is a review synthesizing recent FAST observational results on pulsars and FRBs to highlight synergies in coherent radio emission. We respond to the points raised below.

read point-by-point responses

  1. Referee: The manuscript is a review summarizing published observational results from the Five-hundred-meter Aperture Spherical radio Telescope (FAST) on pulsar single-pulse behavior, polarization, spectral features, and FRB properties. It claims these high-sensitivity data supply pivotal insights into the long-standing problem of coherent radio emission mechanisms shared by pulsars and FRBs, and it encourages additional FAST observations to advance the field.

    Authors: We appreciate the referee's accurate summary of the manuscript's scope and intent. As a review, it focuses on collating and contextualizing published FAST results rather than presenting new data or models. We have revised the introduction and conclusion to more explicitly link the summarized observations to the shared emission physics between pulsars and FRBs, while maintaining the review format. revision: partial

  2. Referee: If the cited FAST results are accurately and comprehensively summarized, the review could usefully collate recent high-sensitivity data in one place, underscoring observational synergies between pulsars and FRBs. This may help guide future modeling and observing strategies, though its impact is limited by the absence of new derivations, quantitative comparisons, or falsifiable predictions.

    Authors: We agree that the primary value lies in providing a consolidated summary of high-sensitivity FAST data. As this is a review article, new theoretical derivations fall outside its scope; however, we have added brief quantitative comparisons drawn from the cited literature (e.g., pulse energy distributions and polarization fractions) and expanded the discussion section to outline how the presented observations can inform falsifiable predictions for future modeling. These additions strengthen the manuscript's utility for guiding observing strategies without altering its review character. revision: partial

Circularity Check

0 steps flagged

No circularity: pure review with no derivations or predictions

full rationale

The manuscript is a literature review summarizing published FAST observations on pulsar single-pulse behavior, polarization, spectra, and FRB properties. It contains no equations, models, derivations, or new predictions. All central claims rest on citations to external observational results rather than any internal logic, fitted parameters, or self-referential steps that reduce to the paper's own inputs. No load-bearing self-citations or ansatzes are present; the text functions as a perspective piece collating existing data.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No free parameters, axioms, or invented entities are introduced because the paper is a review of observational results rather than a theoretical derivation.

pith-pipeline@v0.9.0 · 5564 in / 967 out tokens · 33670 ms · 2026-05-10T16:40:56.181703+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

221 extracted references · 221 canonical work pages · 2 internal anchors

  1. [1]

    Manchester R N, Taylor J H, 1977PulsarsSan Francisco : W. H. Freeman

    work page

  2. [2]

    Peng B, 2021The FAST ProjectShanghai Science & Technology Education Press: Shanghai

    work page

  3. [3]

    Jiang P, Yue Y L, Gan H Q,et al.2019Science China Physics, Mechanics, and Astronomy62, 959502

    work page

  4. [4]

    Jiang P, Tang N Y, Hou L G,et al.2020Research in Astronomy and Astrophysics20, 064

    work page

  5. [5]

    Ruderman M A, Sutherland P G, 1975The Astrophysical Journal196, 51

    work page

  6. [6]

    Arons J, Scharlemenn E T, 1979The Astrophysical Journal231, 854

    work page

  7. [7]

    Spitkovsky A, 2006The Astrophysical Journal Letters648, L51

    work page

  8. [8]

    Philippov A, Timokhin A, Spitkovsky A, 2020Physical Review Letters124, 24

    work page

  9. [9]

    Ben´ aˇ cek, J, Jessner, A, Pohl, M,et al.2025arXiv e-prints2503.17249

    work page arXiv

  10. [10]

    Chernoglazov, A., Philippov, A., Timokhin, A., 2024ApJ974, 2

    work page

  11. [11]

    Bransgrove, A., Beloborodov, A., Levin, Y., 2023ApJ958, 1

    work page

  12. [12]

    Li D, Wang P, Qian L,et al.2018IEEE Microwave Magazine19, 112-119

    work page

  13. [13]

    Cordes J M, Freire P C C, Lorimer D R,et al.2006,ApJ637, 446

    work page 2006

  14. [14]

    Manchester R N, Lyne A G, Camilo F,et al.2001,MNRAS328, 17

    work page 2001

  15. [15]

    L., Zhou D

    Han J. L., Zhou D. J., Wang C.,et al.2025,Research in Astronomy and Astrophysics25, 014001

    work page 2025

  16. [16]

    L., Wang C., Wang P

    Han J. L., Wang C., Wang P. F.,et al.2021,Research in Astron. Astrophys. (RAA)21, 107

    work page 2021

  17. [17]

    J., Han J

    Zhou D. J., Han J. L., Xu J.,et al.2023,Research in Astron. Astrophys. (RAA)23, 104001

    work page 2023

  18. [18]

    F., Han J

    Wang P. F., Han J. L., Yang Z. L.,et al.2025,Research in Astron. Astrophys. (RAA)25, 014003

    work page 2025

  19. [19]

    Tedila H M, Yuen R, Wang N,et al.2022The Astrophysical Journal929, 171

    work page

  20. [20]

    Cai Y Q, Dang S J, Tedila H M,et al.2025Monthly Notices of the Royal Astronomical Society544, 299–308

    work page

  21. [21]

    Blackmon V A, McLaughlin M A, Zhao D,et al.2025arXiv e-prints, arXiv:2510.22910

    work page internal anchor Pith review Pith/arXiv arXiv

  22. [22]

    DeCesar M E, Ransom S M, Kaplan D L,et al.2015,ApJ807, 2

    work page 2015

  23. [23]

    Chen X, V´ azquez-Aceves V, Chen S,et al.2025,Physical Review Research7, 3

    work page 2025

  24. [24]

    Hessels J W T, Ransom S M, Stairs I H, Freire P C C, Kaspi V M, Camilo F,et al.2006,Science311, 5769

    work page 2006

  25. [25]

    Hessels J. W. T., Ransom S. M., Stairs I. H.,et al.2007,ApJ670, 1, 363. 52

    work page 2007

  26. [26]

    W.,et al.2020,ApJ892, 1, 43

    Wang L., Peng B., Stappers B. W.,et al.2020,ApJ892, 1, 43

    work page 2020

  27. [27]

    Lian Y., Pan Z., Zhang H.,et al.2025,ApJS279, 2, 51

    work page 2025

  28. [28]

    M., Lorimer D

    Pan Z., Ransom S. M., Lorimer D. R.,et al.2020,ApJ892, 1, L6

    work page 2020

  29. [29]

    C., Zhu W

    Miao C. C., Zhu W. W., Li D.,et al.2023,MNRAS518, 2, 1672

    work page 2023

  30. [30]

    Wang L.,et al.in prep. ,

    work page

  31. [31]

    M.,et al.2021,ApJ921, 2, 120

    Yan Z., Pan Z.-C., Ransom S. M.,et al.2021,ApJ921, 2, 120

    work page 2021

  32. [32]

    Li B., Liu K., Wang L.,et al.2025,ApJ991, 1, 44

    work page 2025

  33. [33]

    G., Jiang P.,et al.2023,Nature620, 7976, 961

    Pan Z., Lu J. G., Jiang P.,et al.2023,Nature620, 7976, 961

    work page 2023

  34. [34]

    Li B, Zhang L-Y, Yao J, Yin D, Eatough R P, Li M, Li Y,et al.2024,ApJ972, 1

    work page 2024

  35. [35]

    Wu Y., Pan Z., Qian L.,et al.2024,The Astrophysical Journal Letters974, 2, L23

    work page 2024

  36. [36]

    Kremer K, Ye C S, Heinke C O,et al.2024,ApJ977, 2, L42

    work page 2024

  37. [37]

    Pan Z, Hobbs G, Li D,et al.2016,MNRAS459, 1, L26

    work page 2016

  38. [38]

    Dai Y, Pan Z, Qian L,et al.2025,Research in Astronomy and Astrophysics25, 7, 071001

    work page 2025

  39. [39]

    Qian L & Pan Z-C 2021,Research in Astronomy and Astrophysics21, 8, 185

    work page 2021

  40. [40]

    Pan Z, Ma X-Y, Qian L,et al.2021,Research in Astronomy and Astrophysics21, 6, 143

    work page 2021

  41. [41]

    Yin D, Zhang L-Y, Qian L,et al.2024,ApJ969, 1, L7

    work page 2024

  42. [42]

    Wang Z, Lu J, 2022MNRAS517, 2, 5560

    work page

  43. [43]

    Wang Z, Lu J, Wang W,et al.2025,A&A700, A255

    work page 2025

  44. [44]

    Wang P F, Han J L, Xu J,et al.2023Research in Astronomy and Astrophysics23, 10

    work page

  45. [45]

    Wang P F, Wang C , Han J L, 2014MNRAS441, 3, 1943

    work page 1943

  46. [46]

    Wang P F, Han J L, 2016MNRAS462, 4, 4416

    work page

  47. [47]

    Wang P F, Wang C, Han J L, 2012MNRAS423, 3, 2464

    work page

  48. [48]

    Karastergiou A, Johnston S, Posselt B,et al.2024,MNRAS532, 3, 3558

    work page 2024

  49. [49]

    Johnston S & Karastergiou A 2019,MNRAS485, 1, 640

    work page 2019

  50. [50]

    Komesaroff M M 1970,Nature225, 5233, 612

    work page 1970

  51. [51]

    Manchester R N & Han J L 2004,ApJ609, 1, 354

    work page 2004

  52. [52]

    M., Manchester R

    Yan W. M., Manchester R. N., van Straten W.,et al.2011,MNRAS414, 3, 2087. 53

    work page 2011

  53. [53]

    N.,et al.2015,MNRAS449, 3, 3223

    Dai S., Hobbs G., Manchester R. N.,et al.2015,MNRAS449, 3, 3223

    work page 2015

  54. [54]

    A., McLaughlin M

    Gentile P. A., McLaughlin M. A., Demorest P. B.,et al.2018,ApJ862, 1, 47

    work page 2018

  55. [55]

    T.,et al.2022,PASA39, e027

    Spiewak R., Bailes M., Miles M. T.,et al.2022,PASA39, e027

    work page 2022

  56. [56]

    M., McLaughlin M

    Wahl H. M., McLaughlin M. A., Gentile P. A.,et al.2022,ApJ926, 2, 168

    work page 2022

  57. [57]

    Xu J., Jiang J., Xu H.,et al.2025,A&A695, A173

    work page 2025

  58. [58]

    Johnston S., Kramer M., Karastergiou A.,et al.2023,MNRAS520, 4, 4801

    work page 2023

  59. [59]

    & Karastergiou A

    Johnston S. & Karastergiou A. 2017,MNRAS467, 3, 3493

    work page 2017

  60. [60]

    Wang P. F. & Han J. L. 2025,ApJ985, 1, 57

    work page 2025

  61. [61]

    Chen X, Yan Y, Han J L,et al.2023Nature Astronomy7, 1235-1244

    work page

  62. [62]

    Tedila H M, Li D, Wang P,et al.2025ApJS277, 39

    work page

  63. [63]

    Rusul A, Wen Z G, Yuan J P,et al.2025arXiv e-printsarXiv:2507.04816

    work page arXiv

  64. [64]

    Yan Y, Han, J L, Zhou D J,et al.2024ApJ965, 25

    work page

  65. [65]

    Radhakrishnan V, Cooke D J, 1969Astrophysical Letters3, 255

    work page

  66. [66]

    Everett J E, Weisberg J M, 2001The Astrophysical Journal553, 341

    work page

  67. [67]

    Sun S N, Wang N, Yan W M, Wang S Q, 2025The Astrophysical Journal983, 2

    work page

  68. [68]

    Cao S S, Jiang J C, Dyks J,et al.2024The Astrophysical Journal973, 1

    work page

  69. [69]

    Dang S J, Yuan J P, Shang L H,et al.2024Monthly Notices of the Royal Astronomical Society528, 2

    work page

  70. [70]

    Beskin V S, Philippov A A, 2012Monthly Notices of the Royal Astronomical Society425, 2

    work page

  71. [71]

    Johnston S, Mitra D, Keith M J,et al.2024Monthly Notices of the Royal Astronomical Society530, 4

    work page

  72. [72]

    Cao S S, Jiang J C, Dyks J,et al.2025The Astrophysical Journal983, 1

    work page

  73. [73]

    Petrova S A, Lyubarskii Y E, 2000Astronomy and Astrophysics355, 1168

    work page

  74. [74]

    Wang C, Lai D, Han J L, 2010Monthly Notices of the Royal Astronomical Society403, 569

    work page

  75. [75]

    Cao S S, Guo Y J, Jiang J C,et al.2025arXiv e-prints2512.19056

    work page internal anchor Pith review arXiv

  76. [76]

    Lyubarskii Y E, Petrova S A, 1998Astrophysics and Space Science262, 4

    work page

  77. [77]

    Rankin J M, Rodriguez C, Wright G A E,et al., 2006,MNRAS370, 673–680

    work page 2006

  78. [78]

    Wahl H M, Orfeo D J, Rankin J M, Weisberg J M,et al., 2016,MNRAS461, 3740–3746

    work page 2016

  79. [79]

    Wang L, Yu Y-Z, Kou F, Liu K, Wang X, Peng B,et al., 2022,RAA22, 045001

    work page 2022

  80. [80]

    Han J, Han J L, Peng L-X, Tang D-Y, Wang J,et al., 2016,MNRAS456, 3413–3421. 54

    work page 2016

Showing first 80 references.