Pith. sign in

REVIEW 3 major objections 4 minor 1 cited by

The Frequency-dependent Modulation Features of PSR J1948+3540

T0 review · 3 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read This paper reports that in PSR J1948+3540 the dominant intensity-modulation component shifts from the first half to the second half of the central emission component as the observing frequency increases.

desk verdict A careful single-pulsar study reporting a plausible frequency-dependent modulation shift, but the key comparison is confounded with epoch and telescope and lacks error bars. read the letter →

arxiv 2505.03444 v1 pith:32AH4Z7Q submitted 2025-05-06 astro-ph.HE

Kaige Chang , Na Wang , Feifei Kou , Wenming Yan , Jianping Yuan , Shijun Dang , Jumei Yao , Vishal Gajjar
show 1 more author
Xia Zhou
This is my paper · ORCID
classification astro-ph.HE
keywords pulsars:individual(PSRJ1948+3540)intensitymodulationlongitude-resolvedfluctuationspectrumfrequencydependencecorecomponentphaselockingpolarizationsub-pulse
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports a previously unseen observational pattern in the pulsar PSR J1948+3540: the part of the pulse that carries the intensity modulation changes with observing frequency. At low frequencies the first half of the central component dominates the modulation, while at high frequencies the second half becomes dominant. The authors show that this shift is not caused by changes in component spectra or by linear polarization, both of which they analyze in detail. If the claim holds, it would be the first reported case of modulation dominance shifting with frequency in a pulsar, and it would challenge simple geometric explanations based on emission height alone.

What carries the argument

The central tool is the Longitude-Resolved Fluctuation Spectrum (LRFS), which measures modulation power as a function of pulse longitude and fluctuation frequency. The paper computes time-varying LRFS by sliding a 512-pulse window over each observation, showing that the modulation frequency changes with epoch. It then selects fixed modulation-frequency slices and plots the FFT amplitude and phase versus longitude, which locates the dominant component (MI versus MII) and tests whether components are phase-locked. A phase-resolved spectral-index fit using the ratio of component intensities across frequency channels supplies the spectral evidence that MI and MII have nearly identical spectral behavior.

What would settle it

A same-epoch multi-frequency observation of PSR J1948+3540 (for example, recording both roughly 750 MHz and 1250 MHz within the same day) that shows the same half of the core dominating modulation at both frequencies would falsify the frequency-dependence claim; it would instead indicate that epoch or telescope system, not frequency, sets the dominant modulation component.

Watch

Extended reading notes

Core claim

The paper shows that PSR J1948+3540, a 0.717-second radio pulsar with a core-single profile, displays broad low-frequency intensity modulation whose period changes with epoch. The new discovery is frequency-dependent dominance: in longitude-resolved fluctuation spectra, the modulation power is largest in the first half of the middle component (MI) at 400 and 750 MHz, but in the second half (MII) at 1250 MHz. The phase-resolved spectral index is essentially the same for MI and MII, and the degree of linear polarization is low and concentrated in MI, while the total-intensity peak lies in MII; the authors therefore conclude that the dominance shift is not a spectral or polarization artifact. They further find that the leading and trailing conal components are phase-locked to the middle component's modulation, with time delays of several to tens of rotation periods, and that these conal components have flatter spectra than the core.

Load-bearing premise

The claim assumes that the difference in dominant modulation component is caused by observing frequency, not by the fact that the low-frequency (GMRT, June 2024) and high-frequency (FAST, October 2020) data come from different epochs, and the paper itself shows the modulation period changes with epoch.

Editorial extensions

If this is right

  • The dominance switch between MI and MII is a new type of frequency-dependent pulsar modulation, distinct from the disappearance of drifting sub-pulse modes seen in PSR B0031−07.
  • Because MI and MII have nearly the same spectral index, the switch cannot be a trivial consequence of component spectra, so it constrains models of core emission geometry.
  • The leading and trailing components are phase-locked to the core modulation with stable time delays, implying a single modulation driver acting across the profile.
  • The modulation frequency is time-dependent at every band, so the frequency-dependence of dominance is independent of the drift of the modulation period.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If later simultaneous multi-frequency observations confirm the shift, the most economical explanation would be that the modulating region is viewed at different effective altitudes at different frequencies, so the line of sight cuts the modulation pattern in different halves of the core.
  • The phase-locked leading/trailing alternation resembles the shifted-pulse phenomenon; comparing PSR J1948+3540 with shifted-pulse pulsars at overlapping frequencies could test whether the same contraction-expansion mechanism operates.
  • A direct test: reprocess the archived 1.4 GHz Arecibo data and 92 cm Westerbork data used in earlier studies with the same LRFS slicing; if the dominance there also follows frequency, the claim gains independent support without new observations.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper analyzes GMRT 400/750 MHz and FAST 1250 MHz observations of PSR J1948+3540, combining single-pulse stacks, longitude-resolved fluctuation spectra (LRFS), phase-resolved spectral indices, and polarization/RVM fitting. The central claim is that the dominant modulation component of the middle profile component shifts from the first half (MI) at low frequency to the second half (MII) at high frequency, and that this shift is not caused by spectral intensity changes or linear polarization. The paper also reports time-dependent modulation periods, phase-locking among components, flatter spectra for the leading/trailing conal components, and a complex PA swing. The discussion argues that this frequency-dependent modulation is a previously unreported phenomenon that challenges current emission models.

Significance. If the central claim were robust, it would be a genuinely novel observational result: a frequency-dependent switch of the dominant sub-profile modulation component has, to my knowledge, not been reported for a non-drifting pulsar, and it would constrain emission-height and magnetospheric models. The paper also contains useful by-products: phase-resolved spectra showing the conal components have flatter spectra, phase-locking measurements among components, and an RVM fit using highly polarized samples. The analysis is purely observational, and the consistency checks against earlier published LRFS are appropriate. However, the headline frequency-dependence claim is currently not securely established because the evidence rests on qualitative power comparisons without statistical uncertainties and because frequency is confounded with epoch and telescope in the data.

major comments (3)
  1. [Section 3.1 and Figure 4] The claim that MI dominates at 750 MHz and MII at 1250 MHz rests on a visual comparison of the longitude-resolved average LRFS power in Figure 4. No error bars, confidence intervals, or significance tests are provided for the MI-versus-MII power difference. Because the modulation features are broad and the low-frequency power in individual pulse blocks is noisy, the apparent reversal could be within the noise. Please report the ratio of MI to MII LRFS power (or the phase-resolved amplitudes at the identified modulation frequencies) with uncertainties, for example from bootstrap resampling of pulse blocks, and state the significance of the difference.
  2. [Table 1 and Section 3.1] Frequency is confounded with epoch and telescope. The 750 MHz data were taken with GMRT on MJD 60469, the 400 MHz data with GMRT on MJD 60463, while the 1250 MHz data were taken with FAST on MJD 59127, about 3.7 years earlier. The paper itself shows that the modulation state is strongly time-dependent: Table 1 lists peak modulation frequencies of 0.0058(2), 0.012(2), 0.018(3), 0.021(3), and 0.023(5) cpp across the three bands, and Figures 3 and 4 show the LRFS evolving among pulse blocks within a single observation. Therefore the observed MI-versus-MII dominance pattern could equally reflect a change in modulation mode between epochs, a telescope-dependent systematic, or a mode change, rather than a genuine frequency effect. The cited support from Weltevrede et al. (2006, 2007) and Mitra & Rankin (2017) is also based on non-contemporaneous, single-frequency observations and cannot break this degeneracy. To support the frequency-dependence claim, the authors need either contemporaneous multi-frequency observations covering several epochs, or a demonstration that the MI/MII dominance pattern is stable across independent pulse blocks within each band and is reproduced when the same pulsar is observed at a given frequency on different epochs.
  3. [Section 3.1 (400 MHz data)] The 400 MHz data are explicitly described as scattering-limited, and the authors state that no component separation was attempted at this frequency. Consequently, the statement that 'the modulation is also dominated by the leading half of the pulse' at 400 MHz is not the same MI/MII comparison made at 750 and 1250 MHz. The abstract and conclusions nevertheless include 400 MHz as low-frequency evidence for MI dominance. Please either restrict the frequency-dependence claim to the 750 MHz versus 1250 MHz comparison, or present a scattering-corrected decomposition for the 400 MHz profile.
minor comments (4)
  1. [Section 1 heading and Section 2] There are typographical errors: 'INDRUCTION' in the Section 1 heading and 'respetively' in Section 2; these should be corrected.
  2. [Section 3.1] In the text, the modulation frequency is given as '0.023 ± 0.05 cpp', which appears to be a typo for 0.023 ± 0.005 cpp, consistent with Table 1's 0.023(5). Please check and correct all such notational inconsistencies.
  3. [Figure 7 caption] The caption of Figure 7 says '0.058 cpp' in the left panel description; this should be '0.0058 cpp' to match the text and Table 1.
  4. [Table 1] The header 'P3 Phase delay' appears to combine two different quantities: the modulation period P3 and the phase delays between components. Please split the table into separate columns for P3 and for each pair-wise phase delay, with units clearly stated, so that rows are not ambiguous.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central claim is a directly measured property of the longitude-resolved fluctuation spectra, not the output of a derivation from fitted inputs.

full rationale

The paper reports an observational measurement: the MI/MII LRFS amplitude ordering reverses between 750 MHz and 1250 MHz (Section 3.1, Figure 4), and this is presented as a phenomenological finding rather than as the result of a model fit. No parameter is fitted to the MI-versus-MII difference and then renamed a prediction; the comparison is made directly from the fluctuation spectra. The supporting citations (Weltevrede et al. 2006, 2007; Mitra & Rankin 2017) are external observations at other epochs and telescopes, cited for consistency, and are not used as inputs that force the present conclusion. The phase-locking and spectral-index analyses in Sections 3.2 and 3.3 are auxiliary and do not presuppose the frequency-dependence claim. The paper's own Table 1 shows that the modulation frequency is time-dependent, which raises a legitimate epoch-versus-frequency confound because the low- and high-frequency data were taken years apart with different telescopes; however, that is a correctness or interpretation risk, not an instance of circular reasoning under the enumerated patterns. The discussion cites prior work by the same group (e.g., Sun et al. 2022; Yan et al. 2019) only for comparison with shifted-pulse and mode-changing pulsars, not as load-bearing support for the central claim. Accordingly, there is no derivation chain that reduces to its own inputs, and no circularity is identified.

Assumptions & free parameters 0 free parameters · 5 assumptions · 0 invented entities

The central claim is a measurement, not a derivation, so no free parameters are fitted as inputs. The key assumptions are the descriptive MI/MII longitude split, the combination of non-contemporaneous telescope data, the interpretation of LRFS features as intrinsic modulation, and the neglect of scattering effects at the higher bands. Fitted spectral-index offsets and RVM geometry parameters are reported results, not inputs to the central claim.

assumptions (5)
  • ad hoc to paper The MI/MII split of the middle component, defined from the total intensity profile 'purely for descriptive convenience', identifies stable emission regions across frequency and epoch.
    Section 3, Figure 1. If the physical emission regions shift relative to this longitude division with frequency, the reported dominance change could be an artifact of the definition.
  • domain assumption Combining data from different telescopes and epochs (GMRT in June 2024 and FAST in October 2020) is valid for inferring a frequency dependence of the dominant modulation component.
    Section 3.1 and Table 1. The paper shows the modulation frequency is time-dependent, so epoch confounding is a real risk.
  • domain assumption The broad low-frequency features in the LRFS are intrinsic amplitude modulation and not artifacts of red noise, unflagged RFI, or interstellar scattering.
    Section 3.1, Figures 3 and 4. RFI was flagged, but no noise simulations or off-pulse significance tests are shown.
  • domain assumption Scattering effects at 400 MHz and any residual at 750 MHz do not affect the conclusions drawn from the 750 and 1250 MHz comparison.
    Section 3 states: 'although scattering broadening at 400 MHz does not affect the conclusions of the article.'
  • domain assumption The phase-resolved spectral analysis is valid under the assumption I = K nu^chi and with relative, uncalibrated flux ratios.
    Section 3.3. This supports the claim that the modulation shift is not caused by intensity changes.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The Frequency-dependent Modulation Features of PSR J1948+3540." pith.science (2026). https://pith.science/paper/32AH4Z7Q

@misc{pith2026250503444,
  author       = {Pith},
  title        = {Pith review of: The Frequency-dependent Modulation Features of PSR J1948+3540},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/32AH4Z7Q}},
  note         = {Machine review of arXiv:2505.03444}
}
read the original abstract

Using observations from GMRT and FAST, we conducted multi-wavelength studies on PSR J1948+3540 and analyzed its intensity modulation characteristics in detail. We found that the intensity modulation of this pulsar exhibits broad low-frequency modulation features. The modulation frequency/period is time-dependent, but the dominant modulation component varies with the observing frequency. Specifically, at low frequencies, the modulation is dominated by the first half of the middle component, while at high frequencies, it is dominated by the second half of the middle component. Spectral analysis revealed that the intensities of the leading and trailing components vary with the observing frequency, but the middle component does not change significantly. Besides, the polarization analyses reveal that the peak of the radiation intensity is located in the latter half of the middle component, whereas the linear polarization is dominant in the former half. However, due to the low degree of linear polarization, the change of the dominant modulation component with the observed frequency is not caused by the variation in linear polarization. The phenomenon of the dominant modulation component varying with observing frequency has not been reported before and remains difficult to understand within the current theoretical framework.

Figures

Figures reproduced from arXiv: 2505.03444 by the authors.

Figure 1
Figure 1. The normalized pulse profile for PSR J1948+3540 at center frequencies of 400 MHz, 750 MHz and 1250 MHz. The longitude of the pulse peak is set to be zero. The top panel of the right column shows the the position angles of the linearly polarized emission. The black, red, and blue lines of the bottom panel are the total intensity, linear polarized intensity, and circular polarized intensity, respectively. We distingui… view at source ↗
Figure 2
Figure 2. The single-pulse stacks of PSR J1948+3540 at center frequencies of 400 MHz (upper left), 750 MHz (upper middle) and 1250 MHz (upper right). The left panels of top columns show the energy variations for the on-pulse range (blue solid line) and the off pulse range (black solid line). The bottom panels of top columns show the integrated pulse profiles which are normalized to the peak intensity. The two columns below di… view at source ↗
Figure 3
Figure 3. The time varying LRFSs of PSR J1948+3540 at 400 MHz (left), 750 MHz (middle) and 1250 MHz (right). The side panels of each column show the temporal variation of the LRFS. The bottom panels are the average LRFS, which are in units of P/P3. tions. The time delays make it difficult to distinguish emission modes. 3.3. The Spectrum The pulsar exhibits significant frequency-dependent features: the intensities of the leadi… view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: The fluctuation spectra analyses for different pulse blocks at center frequencies of 400 MHz (upper left),750 MHz (upper right) and 1250 MHz (below). The upper rows are the results of the first 512 pulses at 400 MHz, 750 MHz. The lower rows represents the pulse range f…
Figure 5
Figure 5. Figure 5: Phase variations of the LRFSs of the FAST data for different modulation frequencies of 0.018 cpp (left) and 0.023 cpp (middle) and 0.012 cpp (right). The panels from top to bottom show the peak amplitudes, the corresponding phase variations and the normalized integrate…
Figure 6
Figure 6. Figure 6: Phase Variations of the LRFSs of the GMRT data for different modulation frequencies, with left for 0.012 cpp , middle for 0.021 cpp and right for 0.018 cpp. The panels from top to bottom show the peak amplitudes, the corresponding phase variations and the normalized in…
Figure 7
Figure 7. Figure 7: Phase Variations of the LRFSs of the GMRT data for different modulation frequencies, with left for 0.058 cpp, middle for 0.017 cpp and right for 0.012 cpp. The panels from top to bottom show the peak amplitudes, the corresponding phase variations and the normalized int…
Figure 8
Figure 8. Figure 8: The normalized pulse profile at different fre￾quencies (upper panel) and longitude-resolved spectral in￾dexes (lower panel). The red points with error bars of the same color are the longitude-resolved spectral indexes cal￾culated for the total intensity at frequencies …
Figure 9
Figure 9. Figure 9: The smoothed difference evolution of the total intensity, linear polarization intensity and circular with fre￾quency from 1050 MHz to 1450 MHz. The colors correspond￾ing to different intensities are displayed in the color-bar on the right. The white line in the middle …
Figure 11
Figure 11. Figure 11: The integrated pulse profile (top panel) and PA distribution (bottom panel). In the top panel, the black and red dashed lines represent total intensity and linear po￾larization intensity (L) of highly polarized single pulse time samples (L/I >= 90%). In the bottom pan…

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. OpenAlex reports about 2 citations worldwide. Full citation record

  1. FAST Pulsar Database III. Snapshots of nulling, mode-changing and subpulse modulation of 374 pulsars

    astro-ph.HE 2026-07 accept novelty 7.0 of 10

    Sensitive FAST L-band single-pulse sequences detect nulling, mode-changing or subpulse modulation in 374 pulsars, with hundreds of first reports and statistical links to older, longer-period, lower-Ė objects.

Reference graph

Works this paper leans on

42 extracted references · 7 canonical work pages · cited by 1 Pith paper

  1. [1]

    Backer, D. C. 1970, Nature, 227, 692, doi: 10.1038/227692a0

    doi:10.1038/227692a0 1970

  2. [2]

    I., & Mitra, D

    Basu, R., Melikidze, G. I., & Mitra, D. 2022a, ApJ, 936, 35, doi: 10.3847/1538-4357/ac8479

    doi:10.3847/1538-4357/ac8479

  3. [3]

    2018, MNRAS, 476, 1345, doi: 10.1093/mnras/sty297 —

    Basu, R., & Mitra, D. 2018, MNRAS, 476, 1345, doi: 10.1093/mnras/sty297 —. 2019, MNRAS, 487, 4536, doi: 10.1093/mnras/stz1590

    doi:10.1093/mnras/sty297 2018

  4. [4]

    Basu, R., Mitra, D., & Melikidze, G. I. 2017, ApJ, 846, 109, doi: 10.3847/1538-4357/aa862d —. 2020a, MNRAS, 496, 465, doi: 10.1093/mnras/staa1574 —. 2020b, ApJ, 889, 133, doi: 10.3847/1538-4357/ab63c9 —. 2021, ApJ, 917, 48, doi: 10.3847/1538-4357/ac0828 —. 2022b, ApJ, 927, 208, doi: 10.3847/1538-4357/ac5039 —. 2023, ApJ, 959, 92, doi: 10.3847/1538-4357/ad083d

    doi:10.3847/1538-4357/aa862d 2017

  5. [5]

    I., et al

    Basu, R., Mitra, D., Melikidze, G. I., et al. 2016, ApJ, 833, 29, doi: 10.3847/1538-4357/833/1/29

    doi:10.3847/1538-4357/833/1/29 2016

  6. [6]

    2024, ApJ, 966, 241, doi: 10.3847/1538-4357/ad395f

    Cai, Y., Dang, S., Yuen, R., et al. 2024, ApJ, 966, 241, doi: 10.3847/1538-4357/ad395f

    work page doi:10.3847/1538-4357/ad395f 2024

  7. [7]

    2007, ChJA&A, 7, 789, doi: 10.1088/1009-9271/7/6/06

    Chen, J.-L., Wang, H.-G., Chen, W.-H., Zhang, H., & Liu, Y. 2007, ChJA&A, 7, 789, doi: 10.1088/1009-9271/7/6/06

    work page doi:10.1088/1009-9271/7/6/06 2007

  8. [8]

    Cordes, J. M. 1978, ApJ, 222, 1006, doi: 10.1086/156218

    doi:10.1086/156218 1978

Show all 42 references
  1. [9]

    G., & Large, M

    Davies, J. G., & Large, M. I. 1970, MNRAS, 149, 301, doi: 10.1093/mnras/149.4.301

    1970 doi

  2. [10]

    D., & Craft, H

    Drake, F. D., & Craft, H. D. 1968, Nature, 220, 231, doi: 10.1038/220231a0

    1968 doi

  3. [11]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, Publications of the Astronomical Society of the Pacific, 125, 306, doi: 10.1086/670067

    2013 doi

  4. [12]

    L., & Rankin, J

    Herfindal, J. L., & Rankin, J. M. 2007, MNRAS, 380, 430, doi: 10.1111/j.1365-2966.2007.12089.x —. 2009, MNRAS, 393, 1391, doi: 10.1111/j.1365-2966.2008.14119.x

    2007

  5. [13]

    2004, MNRAS, 353, 1311, doi: 10.1111/j.1365-2966.2004.08157.x

    Jordan, C. 2004, MNRAS, 353, 1311, doi: 10.1111/j.1365-2966.2004.08157.x

    2004

  6. [14]

    B., Edwards, R

    Hobbs, G. B., Edwards, R. T., & Manchester, R. N. 2006, MNRAS, 369, 655, doi: 10.1111/j.1365-2966.2006.10302.x

    2006

  7. [15]

    W., van Straten, W., & Manchester, R

    Hotan, A. W., van Straten, W., & Manchester, R. N. 2004, PASA, 21, 302, doi: 10.1071/AS04022 14

    2004 doi

  8. [16]

    R., Taylor, J

    Huguenin, G. R., Taylor, J. H., & Troland, T. H. 1970, ApJ, 162, 727, doi: 10.1086/150704

    1970 doi

  9. [17]

    F., et al

    Jankowski, F., van Straten, W., Keane, E. F., et al. 2018, MNRAS, 473, 4436, doi: 10.1093/mnras/stx2476

    2018 doi

  10. [18]

    2019, Science China

    Jiang, P., Yue, Y., Gan, H., et al. 2019, Science China

    2019

  11. [19]

    Physics, Mechanics, and Astronomy, 62, 959502, doi: 10.1007/s11433-018-9376-1

    doi

  12. [20]

    2020, Research in Astronomy and Astrophysics, 20, 064, doi: 10.1088/1674-4527/20/5/64

    Jiang, P., Tang, N.-Y., Hou, L.-G., et al. 2020, Research in Astronomy and Astrophysics, 20, 064, doi: 10.1088/1674-4527/20/5/64

    2020 doi

  13. [21]

    2019, MNRAS, 490, 4565, doi: 10.1093/mnras/stz2865

    Johnston, S., & Kramer, M. 2019, MNRAS, 490, 4565, doi: 10.1093/mnras/stz2865

    2019 doi

  14. [22]

    2024, MNRAS, 530, 4839, doi: 10.1093/mnras/stae1175

    Karastergiou, A. 2024, MNRAS, 530, 4839, doi: 10.1093/mnras/stae1175

    2024 doi

  15. [23]

    Komesaroff, M. M. 1970, Nature, 225, 612, doi: 10.1038/225612a0

    1970 doi

  16. [24]

    Seiradakis, J. H. 1994, A&AS, 107, 515

    1994

  17. [25]

    2012, MNRAS, 427, 180, doi: 10.1111/j.1365-2966.2012.21985.x

    Latham, C., Mitra, D., & Rankin, J. 2012, MNRAS, 427, 180, doi: 10.1111/j.1365-2966.2012.21985.x

    2012

  18. [26]

    G., & Manchester, R

    Lyne, A. G., & Manchester, R. N. 1988, MNRAS, 234, 477, doi: 10.1093/mnras/234.3.477

    1988 doi

  19. [27]

    M., & Malov, I

    Malofeev, V. M., & Malov, I. F. 1980, Soviet Ast., 24, 54

    1980

  20. [28]

    N., Hobbs, G

    Manchester, R. N., Hobbs, G. B., Teoh, A., & Hobbs, M. 2005, AJ, 129, 1993, doi: 10.1086/428488

    2005 doi

  21. [29]

    2000, A&AS, 147, 195, doi: 10.1051/aas:2000298

    Maron, O., Kijak, J., Kramer, M., & Wielebinski, R. 2000, A&AS, 147, 195, doi: 10.1051/aas:2000298

    2000 doi

  22. [30]

    A., & Ord, S

    Deshpande, A. A., & Ord, S. M. 2017, ApJ, 836, 224, doi: 10.3847/1538-4357/aa5c35

    2017 doi

  23. [31]

    I., & Basu, R

    Mitra, D., Melikidze, G. I., & Basu, R. 2023, MNRAS, 521, L34, doi: 10.1093/mnrasl/slad022

    2023 doi

  24. [32]

    2017, MNRAS, 468, 4601, doi: 10.1093/mnras/stx814

    Mitra, D., & Rankin, J. 2017, MNRAS, 468, 4601, doi: 10.1093/mnras/stx814

    2017 doi

  25. [33]

    M., Perera, B

    Rajwade, K. M., Perera, B. B. P., Stappers, B. W., et al. 2021, MNRAS, 506, 5836, doi: 10.1093/mnras/stab1942

    2021 doi

  26. [34]

    Rankin, J. M. 1983a, ApJ, 274, 333, doi: 10.1086/161450 —. 1983b, ApJ, 274, 359, doi: 10.1086/161451 —. 1993a, ApJS, 85, 145, doi: 10.1086/191758 —. 1993b, ApJ, 405, 285, doi: 10.1086/172361

    doi

  27. [35]

    M., Rodriguez, C., & Wright, G

    Rankin, J. M., Rodriguez, C., & Wright, G. A. E. 2006, Monthly Notices of the Royal Astronomical Society, 370, 673

    2006

  28. [36]

    A., & Sutherland, P

    Ruderman, M. A., & Sutherland, P. G. 1975, ApJ, 196, 51, doi: 10.1086/153393

    1975 doi

  29. [37]

    M., Mitra, D., & Kuijpers, J

    Smits, J. M., Mitra, D., & Kuijpers, J. 2005, A&A, 440, 683, doi: 10.1051/0004-6361:20041626

    2005 doi

  30. [38]

    M., Mitra, D., Stappers, B

    Smits, J. M., Mitra, D., Stappers, B. W., et al. 2007, A&A, 465, 575, doi: 10.1051/0004-6361:20066292

    2007 doi

  31. [39]

    N., Yan, W

    Sun, S. N., Yan, W. M., Wang, N., et al. 2022, ApJ, 934, 57, doi: 10.3847/1538-4357/ac7c15 van Straten, W., & Bailes, M. 2011, PASA, 28, 1, doi: 10.1071/AS10021

    2022 doi

  32. [40]

    T., & Stappers, B

    Weltevrede, P., Edwards, R. T., & Stappers, B. W. 2006, A&A, 445, 243, doi: 10.1051/0004-6361:20053088

    2006 doi

  33. [41]

    W., & Edwards, R

    Weltevrede, P., Stappers, B. W., & Edwards, R. T. 2007, A&A, 469, 607, doi: 10.1051/0004-6361:20066855

    2007 doi

  34. [42]

    M., Manchester, R

    Yan, W. M., Manchester, R. N., Wang, N., et al. 2019, MNRAS, 485, 3241, doi: 10.1093/mnras/stz650

    2019 doi

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.