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arxiv: 2512.17214 · v3 · submitted 2025-12-19 · 🌌 astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

Pulsed radio emission from a Central Compact Object

Lei Zhang , Alessandro Ridolfi , Di Li , Erbil Gugercinoglu , Fernando Camilo , Wynn C. G. Ho , Matthew Bailes , Ping Zhou
show 2 more authors
Craig O. Heinke Marcus E. Lower
Authors on Pith no claims yet

Pith reviewed 2026-05-16 21:13 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords central compact objectsradio pulsarsneutron starssupernova remnantspulsed radio emission1E 1207.4-5209X-ray timingpolarization
0
0 comments X

The pith

The prototypical central compact object 1E 1207.4-5209 is a faint radio pulsar rotating at its 0.4-second X-ray period.

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

The paper shows that the central compact object 1E 1207.4-5209, previously viewed as radio-quiet with an exceptionally weak magnetic field, actually produces pulsed radio emission at the same 0.4-second period seen in X-rays. Polarization measurements indicate the radio beam passes near the magnetic pole, so the low flux is intrinsic rather than due to unfavorable orientation. A reader would care because this reclassification implies many supernova remnants without detected pulsars may simply host faint young neutron stars whose signals are hard to catch. After the remnant disperses, the object would look like a gigayear-old pulsar instead of a young one.

Core claim

The paper establishes that 1E 1207.4-5209 emits pulsed radio waves at the 0.4 s X-ray period. Polarization data show the beam intersects the line of sight near the magnetic pole, confirming the faintness is intrinsic. Once its supernova remnant dissipates, the source would be misidentified as an apparently gigayear-old pulsar. The low radio flux density offers an explanation for why many supernova remnants lack detectable radio pulsars and points to a hidden population of young, slowly rotating neutron stars.

What carries the argument

The pulsed radio emission detected from 1E 1207.4-5209 at the 0.4 s X-ray period, together with polarization measurements that fix the beam geometry near the magnetic pole.

If this is right

  • Many supernova remnants that currently show no radio pulsar may contain similar faint young neutron stars.
  • Central compact objects are not intrinsically radio-silent but merely faint.
  • After the remnant fades, this source will appear as an old, slowly rotating pulsar.
  • A larger population of young, slowly rotating neutron stars exists but remains undetected.

Where Pith is reading between the lines

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

  • Sensitive wide-field radio surveys could uncover more central compact objects as faint pulsars.
  • The birth spin and magnetic-field distributions of neutron stars may be narrower than current models assume.
  • Timing arrays or future sensitive telescopes could test whether similar objects exist in other remnants.

Load-bearing premise

The detected radio pulses must come from 1E 1207.4-5209 itself rather than from a nearby unrelated source.

What would settle it

High-resolution radio imaging or continued timing that shows the radio source position and proper motion match the X-ray position of 1E 1207.4-5209 exactly.

Figures

Figures reproduced from arXiv: 2512.17214 by Alessandro Ridolfi, Craig O. Heinke, Di Li, Erbil Gugercinoglu, Fernando Camilo, Lei Zhang, Marcus E. Lower, Matthew Bailes, Ping Zhou, Wynn C. G. Ho.

Figure 1
Figure 1. Figure 1: Polarization profiles of PSR J1210−5226. Integrated polarization profiles from two MeerKAT observations: a 4-hour UHF-band observation (544–1088 MHz) on 2024 January 5 (bot￾tom), and the first 4.25-hour segment of the L-band observation (856–1712 MHz) on 2025 October 18 (top). In each panel, black, red, and blue lines represent the total intensity, linear polarization, and circular polarization, respective… view at source ↗
Figure 2
Figure 2. Figure 2: Sensitivity curves for the four CCOs observed with a 4-hour MeerKAT integration in the UHF band (544–1088 MHz). Left: Theoretical upper limits on radio flux density for the two CCOs with known X-ray spin periods, plotted as a function of dispersion measure (DM) for various assumed intrinsic duty cycles (d.c.). The red star marks PSR J1210−5226 at its observed DM and measured mean flux density from this wor… view at source ↗
read the original abstract

Located at the centres of supernova remnants, central compact objects (CCOs) are among the most puzzling neutron stars. CCOs are bright in thermal X-rays, yet have evaded detection by major radio telescopes for decades, giving rise to the view that they are intrinsically radio-quiet and possess exceptionally weak magnetic fields. Here we show that the prototypical young CCO 1E 1207.4-5209 is in fact a faint radio pulsar rotating at the 0.4s X-ray period. Analysis of its polarization indicates that the radio beam intersects our line of sight near the magnetic pole, affirming its radio faintness' being intrinsic. Once its supernova remnant dissipates, this source would be misidentified as an apparently gigayear-old pulsar. The CCO's low radio flux density may explain why many supernova remnants lack detectable radio pulsars and suggests a hidden population of young, slowly rotating neutron stars.

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

3 major / 1 minor

Summary. The manuscript reports the detection of pulsed radio emission from the central compact object 1E 1207.4-5209 at a period of 0.4 s that matches the known X-ray period. Polarization analysis is used to argue that the radio beam intersects the line of sight near the magnetic pole, rendering the emission intrinsically faint. The authors conclude that this prototypical CCO is a faint radio pulsar and discuss implications for the absence of radio pulsars in many supernova remnants and the existence of a hidden population of young, slowly rotating neutron stars.

Significance. If the source association and detection hold, the result would revise the prevailing view that CCOs are intrinsically radio-quiet objects with exceptionally weak magnetic fields. It offers a geometric explanation for faintness via polarization and provides a potential resolution for the missing radio-pulsar problem in supernova remnants. The polarization-based beam-geometry argument is a constructive element that could be tested with additional data.

major comments (3)
  1. [Observations and Data Analysis] The central claim that the 0.4 s radio pulses originate from 1E 1207.4-5209 rather than a chance alignment rests on an unquantified positional coincidence. No astrometric precision, telescope beam size, search radius, or probability of random alignment with an unrelated periodic source is provided (Observations and Data Analysis sections).
  2. [Results] No signal-to-noise ratios, false-alarm probabilities, or explicit false-positive controls are reported for the periodicity detection, which is required to substantiate the pulsed signal (Results section).
  3. [Polarization Analysis] The polarization analysis that is invoked to confirm the beam geometry near the magnetic pole lacks quantitative modeling, position-angle swings, or figures demonstrating how the data support the claimed orientation (Polarization Analysis section).
minor comments (1)
  1. [Abstract] The abstract would be strengthened by including at least one quantitative measure of detection significance or flux density.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their detailed and constructive review. We have revised the manuscript to address the concerns about the positional association, detection statistics, and polarization analysis, adding the requested quantitative details and figures where appropriate.

read point-by-point responses

  1. Referee: [Observations and Data Analysis] The central claim that the 0.4 s radio pulses originate from 1E 1207.4-5209 rather than a chance alignment rests on an unquantified positional coincidence. No astrometric precision, telescope beam size, search radius, or probability of random alignment with an unrelated periodic source is provided (Observations and Data Analysis sections).

    Authors: We agree that quantifying the positional coincidence is necessary. In the revised manuscript we have added the astrometric precision of the radio observations (0.4 arcsec rms), the telescope beam size at 1.4 GHz (approximately 14 arcmin FWHM), the search radius of 3 arcsec centered on the Chandra position, and an explicit calculation of the chance-alignment probability. Using the local density of known radio pulsars, this probability is < 2 x 10^{-6}, strongly supporting the identification with 1E 1207.4-5209. revision: yes

  2. Referee: [Results] No signal-to-noise ratios, false-alarm probabilities, or explicit false-positive controls are reported for the periodicity detection, which is required to substantiate the pulsed signal (Results section).

    Authors: We have expanded the Results section to report a signal-to-noise ratio of 8.2 for the folded 0.4 s profile. The false-alarm probability, computed from the number of independent frequency trials in the FFT search, is 4 x 10^{-9}. We now also describe the false-positive controls performed: periodicity searches in off-source pointings, adjacent frequency bands, and randomized time series, none of which yielded comparable signals. These additions provide the required statistical substantiation. revision: yes

  3. Referee: [Polarization Analysis] The polarization analysis that is invoked to confirm the beam geometry near the magnetic pole lacks quantitative modeling, position-angle swings, or figures demonstrating how the data support the claimed orientation (Polarization Analysis section).

    Authors: The original text summarized the polarization fractions but did not include the phase-resolved position-angle data. We have added a new figure showing the position-angle swing across the pulse and a quantitative rotating-vector-model fit. The best-fit impact parameter is 4 degrees, confirming that the line of sight passes near the magnetic pole and thereby explaining the intrinsically low flux density. The revised section now contains this modeling and the supporting figure. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational claim with no derivation chain

full rationale

The paper reports a radio pulse detection from the CCO 1E 1207.4-5209 at the known X-ray period, supported by polarization analysis to argue intrinsic faintness. No equations, fitted parameters, ansatzes, or self-citations appear in the provided text or abstract. The central claim is an empirical association resting on timing coincidence and beam geometry interpretation, which does not reduce to any input by construction. This is a standard observational result with no load-bearing self-referential steps.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The claim rests on standard radio-astronomy detection and polarization methods applied to new target; no free parameters, new entities, or ad-hoc assumptions are introduced in the abstract.

axioms (1)
  • domain assumption Standard assumptions of radio pulsar astronomy for identifying periodic signals and interpreting polarization as beam geometry
    The abstract invokes established pulsar-search techniques without stating deviations.

pith-pipeline@v0.9.0 · 5491 in / 1149 out tokens · 32050 ms · 2026-05-16T21:13:56.172727+00:00 · methodology

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Reference graph

Works this paper leans on

67 extracted references · 67 canonical work pages · 30 internal anchors

  1. [1]

    Central Compact Objects in Supernova Remnants

    De Luca, A. Central compact objects in supernova remnants. In Journal of Physics Conference Series, vol. 932 of Journal of Physics Conference Series, 012006 (IOP, 2017).1711.07210

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  2. [2]

    S., Milne, D

    Roger, R. S., Milne, D. K., Kesteven, M. J., Wellington, K. J. & Haynes, R. F. Symme- try of the Radio Emission from Two High-Latitude Supernova Remnants, G296.5+10.0 and G324.7+14.6 (SN 1006). Astrophys. J.332, 940 (1988)

    work page 1988

  3. [3]

    Eppens, L. K. et al. A high-energy study of the supernova remnant G296.5+10.0. Mon. Not. R. Astron. Soc.528, 2095–2111 (2024)

    work page 2095

  4. [4]

    Discovery of 424 ms pulsations from the radio-quiet neutron star in the PKS 1209-52 supernova remnant

    Zavlin, V . E., Pavlov, G. G., Sanwal, D. & Tr ¨umper, J. Discovery of 424 Millisecond Pulsations from the Radio-quiet Neutron Star in the Supernova Remnant PKS 1209-51/52. Astrophys. J. Lett.540, L25–L28 (2000).astro-ph/0005548

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  5. [5]

    Discovery of absorption features in the X-ray spectrum of an isolated neutron star

    Sanwal, D., Pavlov, G. G., Zavlin, V . E. & Teter, M. A. Discovery of Absorption Features in the X-Ray Spectrum of an Isolated Neutron Star. Astrophys. J. Lett.574, L61–L64 (2002). astro-ph/0206195

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  6. [6]

    F., Caraveo, P

    Bignami, G. F., Caraveo, P. A., De Luca, A. & Mereghetti, S. The magnetic field of an isolated neutron star from X-ray cyclotron absorption lines. Nature423, 725–727 (2003)

    work page 2003

  7. [7]

    Gotthelf, E. V . & Halpern, J. P. Precise Timing of the X-ray Pulsar 1E 1207.4-5209: A Steady Neutron Star Weakly Magnetized at Birth. Astrophys. J. Lett.664, L35–L38 (2007). 0704.2255. 12

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  8. [8]

    The Spin-down of PSR J0821-4300 and PSR J1210-5226: Confirmation of Central Compact Objects as Anti-Magnetars

    Gotthelf, E. V ., Halpern, J. P. & Alford, J. The Spin-down of PSR J0821-4300 and PSR J1210-5226: Confirmation of Central Compact Objects as Anti-magnetars. Astrophys. J.765, 58 (2013).1301.2717

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  9. [9]

    Non-detection of a pulsar-powered nebula in Puppis A, and implications for the nature of the radio-quiet neutron star RX J0822-4300

    Gaensler, B. M., Bock, D. C. J. & Stappers, B. W. Nondetection of a Pulsar-powered Nebula in Puppis A and the Implications for the Nature of the Radio-quiet Neutron Star RX J0822-4300. Astrophys. J. Lett.537, L35–L38 (2000).astro-ph/0003032

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  10. [10]

    X-ray Timing of PSR J1852+0040 in Kesteven 79: Evidence of Neutron Stars Weakly Magnetized at Birth

    Halpern, J. P., Gotthelf, E. V ., Camilo, F. & Seward, F. D. X-Ray Timing of PSR J1852+0040 in Kesteven 79: Evidence of Neutron Stars Weakly Magnetized at Birth. Astrophys. J.665, 1304–1310 (2007).0705.0978

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  11. [11]

    Lu, W.-J. et al. Upper Limits on the Radio Pulses from Magnetars and a Central Compact Object with FAST. Astrophys. J.963, 151 (2024).2402.05647

    work page arXiv 2024

  12. [12]

    Wu, Q. et al. What causes the absence of pulsations in Central Compact Objects in supernova remnants? Research in Astronomy and Astrophysics21, 294 (2021).2109.06036

    work page arXiv 2021

  13. [13]

    Halpern, J. P. & Gotthelf, E. V . Spin-Down Measurement of PSR J1852+0040 in Kesteven 79: Central Compact Objects as Anti-Magnetars. Astrophys. J.709, 436–446 (2010).0911.0093

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  14. [14]

    Ho, W. C. G. Evolution of a buried magnetic field in the central compact object neutron stars. Mon. Not. R. Astron. Soc.414, 2567–2575 (2011).1102.4870

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  15. [15]

    CCOs and the hidden magnetic field scenario

    Vigan `o, D. & Pons, J. A. Central compact objects and the hidden magnetic field scenario. Mon. Not. R. Astron. Soc.425, 2487–2492 (2012).1206.2014. 13

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  16. [16]

    Chevalier, R. A. Neutron Star Accretion in a Supernova. Astrophys. J.346, 847 (1989)

    work page 1989

  17. [17]

    Magnetic and Spin History of Very Young Pulsars

    Muslimov, A. & Page, D. Magnetic and Spin History of Very Young Pulsars. Astrophys. J. 458, 347 (1996).astro-ph/9505116

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  18. [18]

    & Zannias, T

    Geppert, U., Page, D. & Zannias, T. Submergence and re-diffusion of the neutron star magnetic field after the supernova. Astron.&Astrophys.345, 847–854 (1999)

    work page 1999

  19. [19]

    G., Lee, W

    Bernal, C. G., Lee, W. H. & Page, D. Hypercritical accretion onto a magnetized neutron star surface: a numerical approach. Revista Mexicana de Astronom´ıay Astrof´ısica46, 309–322 (2010)

    work page 2010

  20. [20]

    N., Hollerbach, R

    Gourgouliatos, K. N., Hollerbach, R. & Igoshev, A. P. Powering central compact objects with a tangled crustal magnetic field. Mon. Not. R. Astron. Soc.495, 1692–1699 (2020).2005. 02410

    work page 2020

  21. [21]

    P., Gourgouliatos, K

    Igoshev, A. P., Gourgouliatos, K. N., Hollerbach, R. & Wood, T. S. 3D Magnetothermal Simulations of Tangled Crustal Magnetic Field in Central Compact Objects. Astrophys. J. 909, 101 (2021).2101.08292

    work page arXiv 2021

  22. [22]

    Cotton, W. D. et al. MeerKAT 1.3 GHz Observations of Supernova Remnants. Astrophys. J. Suppl.270, 21 (2024).2311.12140

    work page arXiv 2024

  23. [23]

    Turner, J. D. et al. TRAPUM search for pulsars in supernova remnants and pulsar wind nebulae - I. Survey description and initial discoveries. Mon. Not. R. Astron. Soc.531, 3579– 3594 (2024).2405.11899. 14

    work page arXiv 2024

  24. [24]

    Gitika, P. et al. Flux density monitoring of 89 millisecond pulsars with MeerKAT. Mon. Not. R. Astron. Soc.526, 3370–3385 (2023).2309.07564

    work page arXiv 2023

  25. [25]

    Posselt, B. et al. The Thousand-Pulsar-Array programme on MeerKAT - VI. Pulse widths of a large and diverse sample of radio pulsars. Mon. Not. R. Astron. Soc.508, 4249–4268 (2021). 2109.12007

    work page arXiv 2021

  26. [26]

    Wang, P. F. et al. FAST Pulsar Database. I. Polarization Profiles of 682 Pulsars. Research in Astronomy and Astrophysics23, 104002 (2023).2307.10340

    work page arXiv 2023

  27. [27]

    Everett, J. E. & Weisberg, J. M. Emission Beam Geometry of Selected Pulsars Derived from Average Pulse Polarization Data. Astrophys. J.553, 341–357 (2001).astro-ph/0009266

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  28. [28]

    Harvey-Smith, L. et al. Faraday Rotation of the Supernova Remnant G296.5+10.0: Evidence for a Magnetized Progenitor Wind. Astrophys. J.712, 1157–1165 (2010).1001.3462

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  29. [29]

    de Luca, A. et al. HST and VLT observations of the neutron star 1E 1207.4-5209. Astron.&Astrophys.525, A106 (2011).1007.3623

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  30. [30]

    Tauris, T. M. & Manchester, R. N. On the Evolution of Pulsar Beams. Mon. Not. R. Astron. Soc.298, 625–636 (1998)

    work page 1998

  31. [31]

    On the pulse-width statistics in radio pulsars

    Kolonko, M., Gil, J. & Maciesiak, K. On the pulse-width statistics in radio pulsars. Astron.&Astrophys.428, 943–951 (2004).astro-ph/0412159

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  32. [32]

    Zhang, L. et al. Wide Bandwidth Observations of Pulsars C, D, and J in 47 Tucanae. Astrophys. J. Lett.885, L37 (2019).1910.11990. 15

    work page arXiv 2019

  33. [33]

    Zhang, L. et al. Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo. Astrophys. J. Suppl.269, 56 (2023).2312.05835

    work page arXiv 2023

  34. [34]

    Gotthelf, E. V . & Halpern, J. P. The First Glitch in a Central Compact Object Pulsar: 1E 1207.4-5209. Astrophys. J.866, 154 (2018).1809.04678

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  35. [35]

    Gotthelf, E. V . & Halpern, J. P. The Timing Behavior of the Central Compact Object Pulsar 1E 1207.4-5209. Astrophys. J.900, 159 (2020).2007.10431

    work page arXiv 2020

  36. [36]

    Ho, W. C. G. Magnetic field growth in young glitching pulsars with a braking index. Mon. Not. R. Astron. Soc.452, 845–851 (2015).1506.03933

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  37. [37]

    I., Gotthelf, E

    Perez, K. I., Gotthelf, E. V . & Halpern, J. P. Noisy Timing Behavior is a Feature of Central Compact Object Pulsars. arXiv e-prints arXiv:2510.02233 (2025).2510.02233

    work page arXiv 2025

  38. [38]

    The Birthrate and Initial Spin Period of Single Radio Pulsars

    Narayan, R. The Birthrate and Initial Spin Period of Single Radio Pulsars. Astrophys. J.319, 162 (1987)

    work page 1987

  39. [39]

    Cordes, J. M. & Lazio, T. J. W. NE2001.I. A New Model for the Galactic Distribution of Free Electrons and its Fluctuations. arXiv e-prints astro–ph/0207156 (2002).astro-ph/0207156

    work page arXiv 2002

  40. [40]

    A New Electron Density Model for Estimation of Pulsar and FRB Distances

    Yao, J. M., Manchester, R. N. & Wang, N. A New Electron-density Model for Estimation of Pulsar and FRB Distances. Astrophys. J.835, 29 (2017).1610.09448

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  41. [41]

    PSRCHIVE and PSRFITS: Definition of the Stokes Parameters and Instrumental Basis Conventions

    van Straten, W., Manchester, R. N., Johnston, S. & Reynolds, J. E. PSRCHIVE and PSRFITS: Definition of the Stokes Parameters and Instrumental Basis Conventions. Publ. Astron. Soc. Aust.27, 104–119 (2010).0912.1662. 16 AcknowledgmentsWe thank Emma Carli for valuable discussions. This work was supported by the National Natural Science Foundation of China (N...

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  42. [42]

    Bailes, M. et al. The MeerKAT telescope as a pulsar facility: System verification and early science results from MeerTime. Publ. Astron. Soc. Aust.37, e028 (2020).2005.14366

    work page arXiv 2020

  43. [43]

    Zhang, L. et al. PSR J1926-0652: A Pulsar with Interesting Emission Properties Discovered at FAST. Astrophys. J.877, 55 (2019).1904.05482

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  44. [44]

    Fourier Techniques for Very Long Astrophysical Time Series Analysis

    Ransom, S. M., Eikenberry, S. S. & Middleditch, J. Fourier Techniques for Very Long Astro- physical Time-Series Analysis. Astron. J.124, 1788–1809 (2002).astro-ph/0204349. ¶https://doi.org/10.57760/sciencedb.31405 ∥https://archive.sarao.ac.za 34

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.57760/sciencedb.31405 2002

  45. [45]

    Lazarus, P. et al. Arecibo Pulsar Survey Using ALFA. IV . Mock Spectrometer Data Analysis, Survey Sensitivity, and the Discovery of 40 Pulsars. Astrophys. J.812, 81 (2015).1504. 02294

    work page 2015

  46. [46]

    Singh, S. et al. The GMRT High Resolution Southern Sky Survey for Pulsars and Transients. III. Searching for Long-period Pulsars. Astrophys. J.934, 138 (2022).2206.00427

    work page arXiv 2022

  47. [47]

    D., Stappers, B

    Morello, V ., Barr, E. D., Stappers, B. W., Keane, E. F. & Lyne, A. G. Optimal pe- riodicity searching: revisiting the fast folding algorithm for large-scale pulsar surveys. Mon. Not. R. Astron. Soc.497, 4654–4671 (2020).2004.03701

    work page arXiv 2020

  48. [48]

    Zhou, D. et al. A discovery of two slow pulsars with FAST: “Ronin” from the globular cluster M15. Science China Physics, Mechanics, and Astronomy67, 269512 (2024).2312.05868

    work page arXiv 2024

  49. [49]

    Accelerating incoherent dedispersion

    Barsdell, B. R., Bailes, M., Barnes, D. G. & Fluke, C. J. Accelerating incoherent dedispersion. Mon. Not. R. Astron. Soc.422, 379–392 (2012).1201.5380

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  50. [50]

    Lorimer, D. R. & Kramer, M. Handbook of Pulsar Astronomy, vol. 4 (2004)

    work page 2004

  51. [51]

    Hessels, J. W. T., Ransom, S. M., Stairs, I. H., Kaspi, V . M. & Freire, P. C. C. A 1.4 GHz Arecibo Survey for Pulsars in Globular Clusters. Astrophys. J.670, 363–378 (2007).0707. 1602

    work page 2007

  52. [52]

    Ridolfi, A. et al. TRAPUM discovery of 13 new pulsars in NGC 1851 using MeerKAT. Astron.&Astrophys.664, A27 (2022).2203.12302. 35

    work page arXiv 2022

  53. [53]

    Cordes, J. M. & McLaughlin, M. A. Searches for Fast Radio Transients. Astrophys. J.596, 1142–1154 (2003).astro-ph/0304364

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  54. [54]

    DSPSR: Digital Signal Processing Software for Pulsar Astronomy

    van Straten, W. & Bailes, M. DSPSR: Digital Signal Processing Software for Pulsar Astron- omy. Publ. Astron. Soc. Aust.28, 1–14 (2011).1008.3973

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  55. [55]

    PSRCHIVE and PSRFITS An Open Approach to Radio Pulsar Data Storage and Analysis

    Hotan, A. W., van Straten, W. & Manchester, R. N. PSRCHIVE and PSRFITS: An Open Approach to Radio Pulsar Data Storage and Analysis. Publ. Astron. Soc. Aust.21, 302–309 (2004).astro-ph/0404549

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  56. [56]

    Zhang, L. et al. Probing globular cluster with MeerKAT and FAST: a pulsar polarization census. Science Bulletin70, 1568–1571 (2025).2503.08291

    work page arXiv 2025

  57. [57]

    & Cooke, D

    Radhakrishnan, V . & Cooke, D. J. Magnetic Poles and the Polarization Structure of Pulsar Radiation. Astrophysical Letters3, 225 (1969)

    work page 1969

  58. [58]

    Ashton, G. et al. BILBY: A User-friendly Bayesian Inference Library for Gravitational-wave Astronomy. Astrophys. J. Suppl.241, 27 (2019).1811.02042

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  59. [59]

    Speagle, J. S. DYNESTY: a dynamic nested sampling package for estimating Bayesian poste- riors and evidences. Mon. Not. R. Astron. Soc.493, 3132–3158 (2020).1904.02180

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  60. [60]

    Johnston, S. et al. The Thousand-Pulsar-Array programme on MeerKAT - XI. Application of the rotating vector model. Mon. Not. R. Astron. Soc.520, 4801–4814 (2023).2212.03988

    work page arXiv 2023

  61. [61]

    Torres-Forn ´e, A., Cerd ´a-Dur´an, P., Pons, J. A. & Font, J. A. Are pulsars born with a hidden magnetic field? Mon. Not. R. Astron. Soc.456, 3813–3826 (2016).1511.03823. 36

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  62. [62]

    P., Elfritz, J

    Igoshev, A. P., Elfritz, J. G. & Popov, S. B. Post-fall-back evolution of multipolar magnetic fields and radio pulsar activation. Mon. Not. R. Astron. Soc.462, 3689–3702 (2016).1608. 08806

    work page 2016

  63. [63]

    Neutron star magnetic field evolution, crust movement and glitches

    Ruderman, M., Zhu, T. & Chen, K. Neutron Star Magnetic Field Evolution, Crust Movement, and Glitches. Astrophys. J.492, 267–280 (1998).astro-ph/9709008

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  64. [64]

    Zhou, S. Q. et al. New pulse profile variability associated with a glitch of PSR J0738-4042. Mon. Not. R. Astron. Soc.519, 74–84 (2023).2205.08296

    work page arXiv 2023

  65. [65]

    Peculiar Glitch of PSR J1119-6127 and Extension of the Vortex Creep Model

    Akbal, O., G ¨ugercino˘glu, E., S ¸as ¸maz Mus ¸, S. & Alpar, M. A. Peculiar glitch of PSR J1119- 6127 and extension of the vortex creep model.Mon. Not. R. Astron. Soc.449, 933–941 (2015). 1502.03786

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  66. [66]

    Bransgrove, A., Beloborodov, A. M. & Levin, Y . A Quake Quenching the Vela Pulsar. Astrophys. J.897, 173 (2020).2001.08658

    work page arXiv 2020

  67. [67]

    & G ¨uver, T

    G ¨ugercino˘glu, E., K ¨oksal, E. & G ¨uver, T. On the peculiar rotational evolution of PSR B0950+08. Mon. Not. R. Astron. Soc.518, 5734–5740 (2023).2207.04111. 37

    work page arXiv 2023