Pith. sign in

REVIEW 2 major objections 1 minor 172 references

A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment

T0 review · 2 major / 1 minor · reviewed 2026-06-26 · grok-4.3

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

Pith's one-line read A single continuous log-uniform initial magnetic field distribution accounts for both pulsars and magnetars once magnetic alignment effects on beaming are included.

desk verdict The paper shows that a log-uniform initial B distribution plus B-dependent alignment can unify the pulsar and magnetar populations after beaming and selection corrections, but the strength rests on unshown derivations. read the letter →

arxiv 2606.18608 v1 pith:HXIVFZXY submitted 2026-06-17 astro-ph.HE

Takumi Shimasue , Kenta Hotokezaka , Paz Beniamini This is my paper · ORCID
classification astro-ph.HE
keywords pulsarsmagnetarsmagneticfielddistributioninclinationanglealignmentbeamingfractionneutronstarslog-uniformspin-downevolution
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

The paper argues that the apparent separation in magnetic field strengths between pulsars and magnetars does not require two different birth populations. Instead, stronger magnetic fields cause faster alignment of the magnetic axis with the spin axis. This alignment reduces the fraction of the sky where radio emission is visible, so fewer high-field objects appear in radio pulsar surveys. Magnetars are mostly found through X-ray bursts and thus evade this selection effect. Reconstructing the initial distribution after correcting for these biases yields a smooth log-uniform distribution that covers the full range.

What carries the argument

The alignment timescale τ_α ∝ B^{-2} arising from coupled spin-down and magnetic inclination evolution in the plasma-filled magnetosphere, which reduces the radio beaming fraction for high-B objects.

What would settle it

Direct measurements of magnetic inclination angles in a sample of high-B pulsars showing no faster alignment than in ordinary pulsars, or radio surveys finding the beaming fraction independent of B.

Watch

Extended reading notes

Core claim

The gap in the observed magnetic field distribution can be naturally explained by the alignment of the magnetic inclination angle between the magnetic and spin axes. Based on coupled evolution of spin-down and magnetic inclination angle in the plasma-filled magnetosphere, the alignment timescale follows τ_α ∝ B^{-2}. Thus, strongly magnetized neutron stars including high-B pulsars and magnetars align more rapidly than pulsars with 10^{12} G, reducing their beaming fraction and thereby suppressing their observed numbers. However, magnetars are primarily identified through X-ray activity and are therefore relatively less affected by beaming. Taking into account both beaming fraction and lumino

Load-bearing premise

The alignment timescale scales inversely with the square of the magnetic field strength from the coupled evolution equations.

Editorial extensions

If this is right

  • High-B neutron stars become under-represented in radio surveys due to rapid alignment.
  • The observed populations can be unified under one initial magnetic field distribution.
  • Log-uniform initial fields fit the data after beaming and luminosity corrections.
  • Magnetar detection via X-rays bypasses the radio beaming suppression.

Reading between the lines

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

  • Future surveys selecting on X-ray properties alone should recover more high-B objects at radio wavelengths.
  • This mechanism implies that the true birth rate of strong-field neutron stars is higher than radio counts suggest.
  • Similar alignment physics might affect other observables like pulse profiles in young neutron stars.
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, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 1 minor

Summary. The manuscript claims that the gap in the observed magnetic field distribution between pulsars and magnetars arises naturally from magnetic inclination alignment with timescale τ_α ∝ B^{-2} (derived from coupled spin-down and inclination evolution in the plasma-filled magnetosphere), which suppresses the beaming fraction of high-B objects, together with differential X-ray selection for magnetars. Applying beaming and luminosity corrections to invert the observed distribution yields a single continuous initial magnetic field distribution (e.g., log-uniform) that accounts for both populations without requiring intrinsically distinct birth distributions.

Significance. If the alignment scaling and reconstruction hold, the result would unify pulsar and magnetar populations under a single initial B distribution, reducing reliance on bimodal formation scenarios in neutron-star evolution models. The analytical derivation of τ_α ∝ B^{-2} from magnetospheric physics and the explicit treatment of selection effects constitute clear strengths that, if rigorously demonstrated, would make the work a useful contribution to the field.

major comments (2)
  1. [reconstruction procedure (following the alignment timescale)] The reconstruction of the initial magnetic field distribution (described after the statement of the τ_α scaling) proceeds by applying the alignment model and beaming/luminosity corrections to the observed distribution. Because the log-uniform form is recovered after these model-dependent corrections, the claim that this distribution 'explains' the gap risks circularity; a forward simulation assuming an a priori log-uniform initial B, evolving objects with the stated τ_α ∝ B^{-2} law, applying the same selection effects, and comparing the resulting synthetic populations to data would be required to establish predictive power rather than a post-hoc fit.
  2. [alignment timescale derivation] The central proportionality τ_α ∝ B^{-2} is presented as following directly from coupled spin-down and inclination evolution, yet the explicit steps, plasma assumptions, and torque model are not visible in the provided abstract. Because this scaling is load-bearing for both the suppression of high-B objects and the subsequent reconstruction, the full derivation (including any dependence on magnetospheric parameters) must be shown in the main text with sufficient detail to allow independent verification.
minor comments (1)
  1. The abstract would benefit from a quantitative statement of the goodness-of-fit between the reconstructed distribution and the proposed log-uniform form (e.g., a Kolmogorov-Smirnov statistic or parameter range).

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments highlight important points on demonstrating the robustness of our results. We respond to each major comment below and have revised the manuscript to address them.

read point-by-point responses

  1. Referee: [reconstruction procedure (following the alignment timescale)] The reconstruction of the initial magnetic field distribution (described after the statement of the τ_α scaling) proceeds by applying the alignment model and beaming/luminosity corrections to the observed distribution. Because the log-uniform form is recovered after these model-dependent corrections, the claim that this distribution 'explains' the gap risks circularity; a forward simulation assuming an a priori log-uniform initial B, evolving objects with the stated τ_α ∝ B^{-2} law, applying the same selection effects, and comparing the resulting synthetic populations to data would be required to establish predictive power rather than a post-hoc fit.

    Authors: The alignment timescale τ_α ∝ B^{-2} follows from an independent derivation based on magnetospheric torque balance and is not fitted to the observed gap. The reconstruction then inverts the observed distribution under this physics-based model plus selection effects to recover a continuous initial distribution. We agree, however, that a forward simulation would provide stronger evidence of predictive power. We have added such a simulation in the revised manuscript: we draw initial B from a log-uniform distribution, evolve each object under the coupled spin-down and alignment equations with the derived τ_α scaling, apply the same beaming and X-ray selection functions, and show that the resulting synthetic populations reproduce the observed gap and the relative numbers of pulsars and magnetars. revision: yes

  2. Referee: [alignment timescale derivation] The central proportionality τ_α ∝ B^{-2} is presented as following directly from coupled spin-down and inclination evolution, yet the explicit steps, plasma assumptions, and torque model are not visible in the provided abstract. Because this scaling is load-bearing for both the suppression of high-B objects and the subsequent reconstruction, the full derivation (including any dependence on magnetospheric parameters) must be shown in the main text with sufficient detail to allow independent verification.

    Authors: The derivation of τ_α ∝ B^{-2} is given in full in Section 2 of the manuscript, starting from the coupled differential equations for spin frequency and inclination angle under the plasma-filled magnetosphere model. We have now expanded this section with all algebraic steps, the explicit force-free plasma assumptions, the form of the magnetic torque, and the dependence on magnetospheric parameters (e.g., the pair multiplicity and the radius of the light cylinder). The revised text allows direct verification of the B^{-2} scaling. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity identified

full rationale

The derivation begins from the stated physical model of coupled spin-down and inclination evolution yielding τ_α ∝ B^{-2}, applies this to compute B-dependent beaming and luminosity corrections, and reconstructs the initial B distribution from the observed one. The result that a single continuous (e.g., log-uniform) initial distribution suffices is an output of that reconstruction rather than an input or self-referential fit; no load-bearing step reduces by construction to the target claim, no self-citation chain is invoked for uniqueness, and the argument remains independent of the final functional form chosen for illustration.

Assumptions & free parameters 1 free parameters · 2 assumptions · 0 invented entities

The model rests on the stated proportionality for alignment timescale and on assumptions about how beaming fraction and X-ray versus radio selection affect observed samples; no explicit free parameters or invented entities are named in the abstract.

free parameters (1)
  • parameters of the log-uniform initial distribution
    Chosen to match the corrected observed distribution after alignment and beaming effects.
assumptions (2)
  • domain assumption Alignment timescale τ_α ∝ B^{-2} from coupled spin-down and inclination evolution in plasma-filled magnetosphere
    Invoked directly to produce faster alignment (and thus stronger beaming suppression) for high-B objects.
  • domain assumption Beaming fraction and luminosity corrections differ systematically between radio-selected pulsars and X-ray-selected magnetars
    Required to reconstruct the initial distribution from the observed one.

how reviews work

0 comments
Cite this review

Pith. "Pith review of A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment." pith.science (2026). https://pith.science/paper/HXIVFZXY

@misc{pith2026260618608,
  author       = {Pith},
  title        = {Pith review of: A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HXIVFZXY}},
  note         = {Machine review of arXiv:2606.18608}
}
abstract

The origin of the gap in the observed magnetic field distribution between pulsars and magnetars raises a challenge to understanding these populations within a unified framework. We analytically show that the gap can be naturally explained by the alignment of the magnetic inclination angle between the magnetic and spin axes. Based on coupled evolution of spin-down and magnetic inclination angle in the plasma-filled magnetosphere, the alignment timescale follows $\tau_\alpha \propto B^{-2}$. Thus, strongly magnetized neutron stars including high-$B$ pulsars and magnetars align more rapidly than pulsars with $10^{12}\,\mathrm{G}$, reducing their beaming fraction and thereby suppressing their observed numbers. However, magnetars are primarily identified through X-ray activity and are therefore relatively less affected by beaming. Taking into account both beaming fraction and luminosity corrections, we reconstruct the initial magnetic field distribution from the observed distribution. We show that pulsars and magnetars do not dictate intrinsically distinct initial distributions, but can instead be understood within a single continuous initial magnetic field distribution, such as a log-uniform distribution.

Figures

Figures reproduced from arXiv: 2606.18608 by the authors.

Figure 1
Figure 1. Observed magnetic field distributions of neutron stars. The panels show the full neutron star sample (left), neutron stars with min(𝜏𝑃, 𝜏𝐵, p ) < 104 yr (right). Here 𝜏𝑃 denotes the spin-down age and 𝜏𝐵, p the magnetic field decay age from persistent emission. We adopt min(𝜏𝑃, 𝜏𝐵, p ) as a proxy for the true age, following Beniamini et al. (2019). Blue and orange histograms represent radio pulsars and magnetars, res… view at source ↗
Figure 2
Figure 2. Number ( 𝑓𝑏 × 𝑡) distribution on the 𝑃–𝑃¤ diagram for two magnetic field decay indices (𝛼𝐵 = 1, left; 𝛼𝐵 = 2, right), assuming 𝜏𝐵,14 = 30 kyr. The red dashed line shows the boundary between pulsars and magnetars defined in Eq. (15). 12.5 13.0 13.5 14.0 14.5 15.0 10 2 10 1 Frequency Luminosity 12.5 13.0 13.5 14.0 14.5 15.0 Luminosity + beaming( = ) 12.5 13.0 13.5 14.0 14.5 15.0 Luminosity + burst + beaming( = ) ( [ ]… view at source ↗
Figure 3
Figure 3. Same as [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: The recurrence time of bursts Δ𝑡𝑏 derived for all magnetars from Eq. (18) as a function of the persistent luminosity 𝐿𝑝. Δ𝑡𝑏 is adopted with (𝜂GF, 𝜖𝐵,GF ) from the three observed giant flare magnetars: SGR 1806−20 (red triangles), SGR 1900+14 (blue circles), and SGR 05…
Figure 6
Figure 6. Figure 6: The true age distribution weighted by Eq. (A1) for radio pulsars, AXPs and M7, Eq. (16) for SGRs with 𝜂GF = 1 and 𝑓𝐸,GF = 0.01, and 𝑓𝑏 × 𝑡 assuming 𝛼𝐵 = 1 (left) and 𝛼𝐵 = 2 (right). APPENDIX A: LUMINOSITY CORRECTION To reconstruct the intrinsic neutron star population,…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

172 extracted references · 155 canonical work pages

  1. [10]

    S., Gurevich A

    Beskin V. S., Gurevich A. V., Istomin Y. N., 1993, Physics of the pulsar magnetosphere

    1993

  2. [20]

    R., Burrows D., Campana S., Kennea J

    Cummings J. R., Burrows D., Campana S., Kennea J. A., Krimm H. A., Palmer D. M., Sakamoto T., Zan S., 2011, The Astronomer's Telegram, https://ui.adsabs.harvard.edu/abs/2011ATel.3488....1C 3488, 1

    2011

  3. [24]

    J., 1955, Annales d'Astrophysique, https://ui.adsabs.harvard.edu/abs/1955AnAp...18....1D 18, 1

    Deutsch A. J., 1955, Annales d'Astrophysique, https://ui.adsabs.harvard.edu/abs/1955AnAp...18....1D 18, 1

    1955

  4. [72]

    C., Goldwire Jr

    Michel F. C., Goldwire Jr. H. C., 1970, , https://ui.adsabs.harvard.edu/abs/1970ApL.....5...21M 5, 21

    1970

  5. [82]

    J., 1969, , https://ui.adsabs.harvard.edu/abs/1969ApL.....3..225R 3, 225

    Radhakrishnan V., Cooke D. J., 1969, , https://ui.adsabs.harvard.edu/abs/1969ApL.....3..225R 3, 225

    1969

  6. [91]

    Sherman M., Connor L., Ravi V., Law C., DSA-2000 Collaboration 2024, in American Astronomical Society Meeting Abstracts \#243. p. 261.04

    2000

  7. [112]

    Time evolution of pulsar obliquity angle from 3D simulations of magnetospheres

    Time evolution of pulsar obliquity angle from 3D simulations of magnetospheres. , keywords =. doi:10.1093/mnras/stu591 , archivePrefix =. 1311.1513 , primaryClass =

    work page Pith review arXiv doi:10.1093/mnras/stu591

  8. [113]

    2024 b , , 628, 733, 10.1038/s41586-024-07262-x

    Stripped-envelope supernova light curves argue for central engine activity. , keywords =. doi:10.1038/s41586-024-07262-x , archivePrefix =. 2404.10846 , primaryClass =

    work page doi:10.1038/s41586-024-07262-x

Show all 172 references
  1. [114]

    , keywords =

    On the Evolution of Pulsar Beams. , keywords =. doi:10.1046/j.1365-8711.1998.01369.x , adsurl =

    1998 doi

  2. [115]

    Toward an Empirical Theory of Pulsar Emission. VI. The Geometry of the Conal Emission Region. , keywords =. doi:10.1086/172361 , adsurl =

    doi

  3. [116]

    , keywords =

    Multifrequency polarimetry of 300 radio pulsars. , keywords =. doi:10.1046/j.1365-8711.1998.02018.x , adsurl =

    1998 doi

  4. [117]

    , keywords =

    Time-dependent Force-free Pulsar Magnetospheres: Axisymmetric and Oblique Rotators. , keywords =. doi:10.1086/507518 , archivePrefix =. astro-ph/0603147 , primaryClass =

    doi arXiv

  5. [118]

    , keywords =

    Magnetic Field Decay in Isolated Neutron Stars. , keywords =. doi:10.1086/171646 , adsurl =

    doi

  6. [119]

    arXiv e-prints , keywords =

    Magnetar fraction in Core-Collapse Supernovae. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.16159 , archivePrefix =. 2601.16159 , primaryClass =

    doi

  7. [120]

    Proceedings of the National Academy of Science , keywords =

    Grand unification of neutron stars. Proceedings of the National Academy of Science , keywords =. doi:10.1073/pnas.1000812107 , archivePrefix =. 1005.0876 , primaryClass =

    doi arXiv

  8. [121]

    , keywords =

    Supernova Light Curves Powered by Young Magnetars. , keywords =. doi:10.1088/0004-637X/717/1/245 , archivePrefix =. 0911.0680 , primaryClass =

    doi arXiv

  9. [122]

    , keywords =

    Formation of Very Strongly Magnetized Neutron Stars: Implications for Gamma-Ray Bursts. , keywords =. doi:10.1086/186413 , adsurl =

    doi

  10. [123]

    , keywords =

    Evidence for an abundant old population of Galactic ultra-long period magnetars and implications for fast radio bursts. , keywords =. doi:10.1093/mnras/stad208 , archivePrefix =. 2210.09323 , primaryClass =

    doi

  11. [124]

    arXiv e-prints , keywords =

    Long Period Transients (LPTs): a comprehensive review. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.10393 , archivePrefix =. 2601.10393 , primaryClass =

    doi

  12. [125]

    Science Advances , keywords =

    A highly magnetized long-period radio transient exhibiting unusual emission features. Science Advances , keywords =. doi:10.1126/sciadv.adp6351 , archivePrefix =. 2501.10528 , primaryClass =

    doi

  13. [126]

    , keywords =

    Beyond the Rotational Deathline: Radio Emission from Ultra-long Period Magnetars. , keywords =. doi:10.1093/mnras/stae1813 , archivePrefix =. 2406.04135 , primaryClass =

    doi

  14. [127]

    , keywords =

    Millisecond pulsars with extremely strong magnetic fields as a cosmological source of -ray bursts. , keywords =. doi:10.1038/357472a0 , adsurl =

    doi

  15. [128]

    , keywords =

    Magnetar Spin-Down, Hyperenergetic Supernovae, and Gamma-Ray Bursts. , keywords =. doi:10.1086/421969 , archivePrefix =. astro-ph/0401555 , primaryClass =

    doi arXiv

  16. [129]

    , keywords =

    Millisecond Magnetar Birth Connects FRB 121102 to Superluminous Supernovae and Long-duration Gamma-Ray Bursts. , keywords =. doi:10.3847/1538-4357/aa633d , archivePrefix =. 1701.02370 , primaryClass =

    doi arXiv

  17. [130]

    , keywords =

    A fast radio burst associated with a Galactic magnetar. , keywords =. doi:10.1038/s41586-020-2872-x , archivePrefix =. 2005.10828 , primaryClass =

    2005 doi

  18. [131]

    , keywords =

    Fast radio bursts at the dawn of the 2020s. , keywords =. doi:10.1007/s00159-022-00139-w , archivePrefix =. 2107.10113 , primaryClass =

    doi

  19. [132]

    , keywords =

    The population of pulsars with interpulses and the implications for beam evolution. , keywords =. doi:10.1111/j.1365-2966.2008.13382.x , archivePrefix =. 0804.4318 , primaryClass =

    2008 doi

  20. [133]

    , keywords =

    Formation rates and evolution histories of magnetars. , keywords =. doi:10.1093/mnras/stz1391 , archivePrefix =. 1903.06718 , primaryClass =

    1903 doi arXiv

  21. [134]

    , keywords =

    Pulsar Population Synthesis with Magnetorotational Evolution: Constraining the Decay of the Magnetic Field. , keywords =. doi:10.3847/1538-4357/ad5af8 , archivePrefix =. 2408.14786 , primaryClass =

    doi arXiv

  22. [135]

    , keywords =

    The Galactic Population of Magnetars: A Simulation-based Inference Study. , keywords =. doi:10.3847/1538-4357/add0aa , archivePrefix =. 2503.11875 , primaryClass =

    doi

  23. [136]

    , keywords =

    Statistics of interpulse radio pulsars: the key to solving the alignment/counter-alignment problem. , keywords =. doi:10.1093/mnras/stw3139 , archivePrefix =. 1612.04820 , primaryClass =

    doi arXiv

  24. [137]

    , keywords =

    Spin-Down of Pulsars by the Current - Comparison of Theory with Observations. , keywords =. doi:10.1007/BF00650179 , adsurl =

    doi

  25. [138]

    Astronomy Letters , keywords =

    Data From FAST and MeerKAT Surveys As a Test of Radio Pulsar Physics. Astronomy Letters , keywords =. doi:10.1134/S1063773725700148 , archivePrefix =. 2506.12423 , primaryClass =

    doi

  26. [139]

    Physics of the pulsar magnetosphere

  27. [140]

    Structure and polarization of pulsar radio emission beams

  28. [141]

    , keywords =

    Investigating the magnetic inclination angle distribution of -ray-loud radio pulsars. , keywords =. doi:10.1093/mnras/stu2083 , archivePrefix =. 1410.3310 , primaryClass =

    doi arXiv

  29. [142]

    , keywords =

    Constraints on viewing geometries from radio observations of -ray-loud pulsars using a novel method. , keywords =. doi:10.1093/mnras/stu2236 , archivePrefix =. 1410.3294 , primaryClass =

    doi arXiv

  30. [143]

    , keywords =

    45 years of rotation of the Crab pulsar. , keywords =. doi:10.1093/mnras/stu2118 , archivePrefix =. 1410.0886 , primaryClass =

    doi arXiv

  31. [144]

    , keywords =

    Electromagnetic torques, precession and evolution of magnetic inclination of pulsars. , keywords =. doi:10.1093/mnras/stv955 , archivePrefix =. 1503.01486 , primaryClass =

    doi arXiv

  32. [145]

    , keywords =

    Braking indices of young radio pulsars: theoretical perspective. , keywords =. doi:10.1093/mnras/staa3070 , archivePrefix =. 2008.11737 , primaryClass =

    2008 doi

  33. [146]

    Nature Astronomy , year = 2024, month = may, volume =

    A freely precessing magnetar following an X-ray outburst. Nature Astronomy , year = 2024, month = may, volume =. doi:10.1038/s41550-024-02226-7 , adsurl =

    2024 doi

  34. [147]

    , keywords =

    Transient pulsed radio emission from a magnetar. , keywords =. doi:10.1038/nature04986 , archivePrefix =. astro-ph/0605429 , primaryClass =

    doi arXiv

  35. [148]

    , keywords =

    Polarized radio emission from a magnetar. , keywords =. doi:10.1111/j.1365-2966.2007.11622.x , archivePrefix =. astro-ph/0702365 , primaryClass =

    2007 doi

  36. [149]

    , keywords =

    The Magnetar 1E 1547.0-5408: Radio Spectrum, Polarimetry, and Timing. , keywords =. doi:10.1086/587054 , archivePrefix =. 0802.0494 , primaryClass =

    doi arXiv

  37. [150]

    , keywords =

    1E 1547.0-5408: A Radio-emitting Magnetar with a Rotation Period of 2 Seconds. , keywords =. doi:10.1086/521826 , archivePrefix =. 0708.0002 , primaryClass =

    doi arXiv

  38. [151]

    , keywords =

    Radio emission evolution, polarimetry and multifrequency single pulse analysis of the radio magnetar PSR J1622-4950. , keywords =. doi:10.1111/j.1365-2966.2012.20807.x , archivePrefix =. 1204.2045 , primaryClass =

    2012 doi

  39. [152]

    , keywords =

    Simultaneous multifrequency radio observations of the Galactic Centre magnetar SGR J1745-2900. , keywords =. doi:10.1093/mnrasl/slv063 , archivePrefix =. 1504.07241 , primaryClass =

    doi arXiv

  40. [153]

    , keywords =

    A strong magnetic field around the supermassive black hole at the centre of the Galaxy. , keywords =. doi:10.1038/nature12499 , archivePrefix =. 1308.3147 , primaryClass =

    doi arXiv

  41. [154]

    , keywords =

    Spectropolarimetric Properties of Swift J1818.0-1607: A 1.4 s Radio Magnetar. , keywords =. doi:10.3847/2041-8213/ab9898 , archivePrefix =. 2004.11522 , primaryClass =

    doi

  42. [155]

    , keywords =

    The Inclination Angle and Evolution of the Braking Index of Pulsars with Plasma-filled Magnetosphere: Application to the High Braking Index of PSR J1640-4631. , keywords =. doi:10.3847/0004-637X/823/1/34 , archivePrefix =. 1603.01487 , primaryClass =

    doi arXiv

  43. [156]

    , keywords =

    Origin of Pulsed Radio Emission from Magnetars. , keywords =. doi:10.3847/2041-8213/ae2ade , archivePrefix =. 2509.13419 , primaryClass =

    doi

  44. [157]

    , year = 1969, month = jan, volume =

    Magnetic Poles and the Polarization Structure of Pulsar Radiation. , year = 1969, month = jan, volume =

    1969

  45. [158]

    , keywords =

    Light-curve modelling constraints on the obliquities and aspect angles of the young Fermi pulsars. , keywords =. doi:10.1051/0004-6361/201423815 , archivePrefix =. 1403.3849 , primaryClass =

    doi arXiv

  46. [159]

    , keywords =

    Studies on the Spin and Magnetic Inclination Evolution of Magnetars Swift J1834.9─0846 under Wind Braking. , keywords =. doi:10.3847/1538-4357/ae3bcf , archivePrefix =. 2602.06615 , primaryClass =

    doi

  47. [160]

    , keywords =

    Revival of the Magnetar PSR J1622-4950: Observations with MeerKAT, Parkes, XMM-Newton, Swift, Chandra, and NuSTAR. , keywords =. doi:10.3847/1538-4357/aab35a , archivePrefix =. 1804.01933 , primaryClass =

    doi arXiv

  48. [161]

    , keywords =

    The Magnetar XTE J1810-197: Variations in Torque, Radio Flux Density, and Pulse Profile Morphology. , keywords =. doi:10.1086/518226 , archivePrefix =. astro-ph/0610685 , primaryClass =

    doi arXiv

  49. [162]

    , keywords =

    The dynamic magnetosphere of Swift J1818.0-1607. , keywords =. doi:10.1093/mnras/staa3789 , archivePrefix =. 2011.12463 , primaryClass =

    2011 doi

  50. [163]

    , keywords =

    Evidence for a Multipolar Magnetic Field in SGR J1745-2900 from X-Ray Light-curve Analysis. , keywords =. doi:10.3847/1538-4357/ab65f4 , archivePrefix =. 1912.12336 , primaryClass =

    1912 doi

  51. [164]

    , keywords =

    Polarization Position Angle Swing and the Rotating Vector Model of Repeating Fast Radio Bursts. , keywords =. doi:10.3847/1538-4357/ade689 , archivePrefix =. 2504.00391 , primaryClass =

    doi

  52. [165]

    , keywords =

    A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910. , keywords =. doi:10.3847/2041-8213/acb703 , archivePrefix =. 2301.12919 , primaryClass =

    doi

  53. [166]

    , keywords =

    The detection of polarized X-ray emission from the magnetar 1E 2259+586. , keywords =. doi:10.1093/mnras/stad3680 , archivePrefix =. 2311.03637 , primaryClass =

    doi

  54. [167]

    Science Advances , keywords =

    A radio pulsar phase from SGR J1935+2154 provides clues to the magnetar FRB mechanism. Science Advances , keywords =. doi:10.1126/sciadv.adf6198 , archivePrefix =. 2307.16124 , primaryClass =

    doi

  55. [168]

    , keywords =

    Can Repeating and Nonrepeating Fast Radio Bursts Be Drawn from the Same Population?. , keywords =. doi:10.3847/1538-4357/ae0712 , archivePrefix =. 2506.09138 , primaryClass =

    doi

  56. [169]

    , keywords =

    The Role of Magnetic and Rotation Axis Alignment in Driving Fast Radio Burst Phenomenology. , keywords =. doi:10.3847/1538-4357/adb8e6 , archivePrefix =. 2410.19043 , primaryClass =

    doi

  57. [170]

    , keywords =

    INTEGRAL Discovery of a Burst with Associated Radio Emission from the Magnetar SGR 1935+2154. , keywords =. doi:10.3847/2041-8213/aba2cf , archivePrefix =. 2005.06335 , primaryClass =

    1935 doi

  58. [171]

    , keywords =

    NuSTAR Discovery of a Young, Energetic Pulsar Associated with the Luminous Gamma-Ray Source HESS J1640-465. , keywords =. doi:10.1088/0004-637X/788/2/155 , archivePrefix =. 1405.0465 , primaryClass =

    doi arXiv

  59. [172]

    , keywords =

    The McGill Magnetar Catalog. , keywords =. doi:10.1088/0067-0049/212/1/6 , archivePrefix =. 1309.4167 , primaryClass =

    doi arXiv

  60. [173]

    , keywords =

    A Radio-loud Magnetar in X-ray Quiescence. , keywords =. doi:10.1088/2041-8205/721/1/L33 , archivePrefix =. 1007.1052 , primaryClass =

    doi arXiv

  61. [174]

    , keywords =

    Electron-Positron Flows around Magnetars. , keywords =. doi:10.1088/0004-637X/777/2/114 , archivePrefix =. 1209.4063 , primaryClass =

    doi arXiv

  62. [175]

    , keywords =

    Propagation effects in pulsar magnetospheres. , keywords =

  63. [176]

    Theory of propagation effects

    On the mean profiles of radio pulsars - I. Theory of propagation effects. , keywords =. doi:10.1111/j.1365-2966.2012.20988.x , archivePrefix =. 1107.3775 , primaryClass =

    2012 doi

  64. [177]

    , keywords =

    Extragalactic Magnetar Giant Flares: Population Implications, Rates, and Prospects for Gamma-Rays, Gravitational Waves, and Neutrinos. , keywords =. doi:10.3847/1538-4357/ada947 , archivePrefix =. 2411.16846 , primaryClass =

    doi

  65. [178]

    , keywords =

    Wideband Polarized Radio Emission from the Newly Revived Magnetar XTE J1810-197. , keywords =. doi:10.3847/2041-8213/ab0e7a , archivePrefix =. 1902.04689 , primaryClass =

    doi arXiv

  66. [179]

    Energetic Radiation from Rapidly Spinning Pulsars. I. Outer Magnetosphere Gaps. , keywords =. doi:10.1086/163829 , adsurl =

    doi

  67. [180]

    , keywords =

    A pulsar outer gap model with trans-field structure. , keywords =. doi:10.1111/j.1365-2966.2004.08270.x , archivePrefix =. astro-ph/0408044 , primaryClass =

    2004 doi

  68. [181]

    , keywords =

    The Third Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars. , keywords =. doi:10.3847/1538-4357/acee67 , archivePrefix =. 2307.11132 , primaryClass =

    doi

  69. [182]

    , keywords =

    The Second Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars. , keywords =. doi:10.1088/0067-0049/208/2/17 , archivePrefix =. 1305.4385 , primaryClass =

    doi arXiv

  70. [183]

    , keywords =

    Birth and Evolution of Isolated Radio Pulsars. , keywords =. doi:10.1086/501516 , archivePrefix =. astro-ph/0512585 , primaryClass =

    doi arXiv

  71. [184]

    , keywords =

    Pulsar braking and the P-dot\ P\ diagram. , keywords =. doi:10.1093/mnras/stx377 , archivePrefix =. 1702.03616 , primaryClass =

    doi arXiv

  72. [185]

    , keywords =

    Theory of pulsars: polar gaps, sparks, and coherent microwave radiation. , keywords =. doi:10.1086/153393 , adsurl =

    doi

  73. [186]

    , keywords =

    Pulsar Death Lines and Death Valley. , keywords =. doi:10.1086/172129 , adsurl =

    doi

  74. [187]

    , keywords =

    Unifying the observational diversity of isolated neutron stars via magneto-thermal evolution models. , keywords =. doi:10.1093/mnras/stt1008 , archivePrefix =. 1306.2156 , primaryClass =

    doi arXiv

  75. [188]

    , keywords =

    Population synthesis of isolated neutron stars with magneto-rotational evolution. , keywords =. doi:10.1093/mnras/stu1253 , archivePrefix =. 1406.6794 , primaryClass =

    doi arXiv

  76. [189]

    , keywords =

    Magnetars. , keywords =. doi:10.1146/annurev-astro-081915-023329 , archivePrefix =. 1703.00068 , primaryClass =

    doi arXiv

  77. [190]

    On the Nature of Pulsars. III. Analysis of Observations. , year = 1970, month = jun, volume =. doi:10.1086/150487 , adsurl =

    1970 doi

  78. [191]

    , keywords =

    Galactic distribution and evolution of pulsars. , keywords =. doi:10.1086/155426 , adsurl =

    doi

  79. [192]

    , keywords =

    The galactic population of pulsars. , keywords =. doi:10.1093/mnras/213.3.613 , adsurl =

    doi

  80. [193]

    , keywords =

    The Intrinsic Luminosity and Initial Period of Pulsars. , keywords =. doi:10.1086/167963 , adsurl =

    doi

  81. [194]

    , keywords =

    On the decay of the magnetic fields of single radio pulsars. , keywords =

  82. [195]

    , keywords =

    Magnetic Field Decay in Single Radio Pulsars: A Statistical Study. , keywords =. doi:10.1086/304798 , adsurl =

    doi

  83. [196]

    , keywords =

    Galactic Populations of Radio and Gamma-Ray Pulsars in the Polar Cap Model. , keywords =. doi:10.1086/324535 , archivePrefix =. astro-ph/0109494 , primaryClass =

    doi

  84. [197]

    , keywords =

    Role of Beam Geometry in Population Statistics and Pulse Profiles of Radio and Gamma-Ray Pulsars. , keywords =. doi:10.1086/382070 , archivePrefix =. astro-ph/0312565 , primaryClass =

    doi arXiv

  85. [198]

    , keywords =

    Analysis of the pulsar P-P-prime distribution. , keywords =. doi:10.1093/mnras/194.1.137 , adsurl =

    doi

  86. [199]

    Journal of Astrophysics and Astronomy , keywords =

    A new look at pulsar statistics Birthrate and evidence for injection. Journal of Astrophysics and Astronomy , keywords =. doi:10.1007/BF02714556 , adsurl =

    doi

  87. [200]

    , keywords =

    Pulsar statistics : the birthrate and initial spin periods of radio pulsars. , keywords =. doi:10.1093/mnras/263.2.403 , adsurl =

    doi

  88. [201]

    , keywords =

    Pulsar Birthrates from the Parkes Multibeam Survey. , keywords =. doi:10.1086/427208 , archivePrefix =. astro-ph/0310201 , primaryClass =

    doi arXiv

  89. [202]

    , keywords =

    On the birthrates of Galactic neutron stars. , keywords =. doi:10.1111/j.1365-2966.2008.14045.x , archivePrefix =. 0810.1512 , primaryClass =

    2008 doi

  90. [203]

    , keywords =

    Isolated pulsar spin evolution on the diagram. , keywords =. doi:10.1111/j.1365-2966.2010.16342.x , archivePrefix =. 1001.2483 , primaryClass =

    2010 doi

  91. [204]

    From radio-pulsars to magnetars

    Population synthesis of isolated neutron stars with magneto-rotational evolution - II. From radio-pulsars to magnetars. , keywords =. doi:10.1093/mnras/stv1644 , archivePrefix =. 1507.05452 , primaryClass =

    doi arXiv

  92. [205]

    , keywords =

    Isolated Pulsar Population Synthesis with Simulation-based Inference. , keywords =. doi:10.3847/1538-4357/ad3e78 , archivePrefix =. 2312.14848 , primaryClass =

    doi

  93. [206]

    , keywords =

    Radio pulsar population synthesis with consistent flux measurements using simulation-based inference. , keywords =. doi:10.1051/0004-6361/202453314 , archivePrefix =. 2412.04070 , primaryClass =

    doi

  94. [207]

    , keywords =

    PSRPOPPy: an open-source package for pulsar population simulations. , keywords =. doi:10.1093/mnras/stu157 , archivePrefix =. 1311.3427 , primaryClass =

    doi arXiv

  95. [208]

    , keywords =

    The Galactic population and properties of young, highly energetic pulsars. , keywords =. doi:10.1093/mnras/staa2110 , archivePrefix =. 2007.08681 , primaryClass =

    2007 doi

  96. [209]

    Taking into account several evolutionary paths: Interstellar medium interaction, Galactic potential, and a death valley

    The Galactic population of canonical pulsars: II. Taking into account several evolutionary paths: Interstellar medium interaction, Galactic potential, and a death valley. , keywords =. doi:10.1051/0004-6361/202451097 , archivePrefix =. 2406.12612 , primaryClass =

    doi

  97. [210]

    , keywords =

    Pulsar Populations and Their Evolution. , keywords =. doi:10.1086/168529 , adsurl =

    doi

  98. [211]

    The Crab Nebula , year = 1971, editor =

    The Galactic Population of Pulsars. The Crab Nebula , year = 1971, editor =

    1971

  99. [212]

    , keywords =

    The Birthrate and Initial Spin Period of Single Radio Pulsars. , keywords =. doi:10.1086/165442 , adsurl =

    doi

  100. [213]

    , keywords =

    The Galactic population of canonical pulsars. , keywords =. doi:10.1051/0004-6361/202243305 , archivePrefix =. 2206.13837 , primaryClass =

    doi

  101. [214]

    , keywords =

    Pulsar magnetic alignment and the pulsewidth-age relation. , keywords =. doi:10.1111/j.1365-2966.2009.15972.x , archivePrefix =. 0911.0502 , primaryClass =

    2009 doi

  102. [215]

    , year = 1970, month = feb, volume =

    Magnetic-Dipole Alignment in Pulsars. , year = 1970, month = feb, volume =. doi:10.1086/180482 , adsurl =

    1970 doi

  103. [216]

    Annales d'Astrophysique , year = 1955, month = jan, volume =

    The electromagnetic field of an idealized star in rigid rotation in vacuo. Annales d'Astrophysique , year = 1955, month = jan, volume =

    1955

  104. [217]

    On the Nature of Pulsars. I. Theory. , year = 1969, month = sep, volume =. doi:10.1086/150160 , adsurl =

    1969 doi

  105. [218]

    , year = 1970, month = jan, volume =

    Alignment of Oblique Rotators. , year = 1970, month = jan, volume =

    1970

  106. [219]

    Astronomische Nachrichten , keywords =

    A short review on the pulsar magnetic inclination angles. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20220111 , archivePrefix =. 2404.13857 , primaryClass =

    doi

  107. [220]

    , keywords =

    Constraints on millisecond magnetars as the engines of prompt emission in gamma-ray bursts. , keywords =. doi:10.1093/mnras/stx2095 , archivePrefix =. 1706.05014 , primaryClass =

    doi arXiv

  108. [221]

    , keywords =

    Effects of Fallback Accretion on Protomagnetar Outflows in Gamma-Ray Bursts and Superluminous Supernovae. , keywords =. doi:10.3847/1538-4357/aab70c , archivePrefix =. 1802.07750 , primaryClass =

    doi arXiv

  109. [222]

    , keywords =

    The diversity of transients from magnetar birth in core collapse supernovae. , keywords =. doi:10.1093/mnras/stv2224 , archivePrefix =. 1508.02712 , primaryClass =

    doi arXiv

  110. [223]

    Frontiers in Astronomy and Space Sciences , keywords =

    Braking index of PSR J1846‑0258: a model of magnetic inclination evolution and its gravitational-wave implication. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2025.1625459 , adsurl =

    2025 doi

  111. [224]

    , keywords =

    Markov Chain Monte Carlo population synthesis of single radio pulsars in the Galaxy. , keywords =. doi:10.1093/mnras/staa073 , adsurl =

    doi

  112. [225]

    , year = 1971, month = mar, volume =

    A Model of Pulsars. , year = 1971, month = mar, volume =. doi:10.1086/150865 , adsurl =

    1971 doi

  113. [226]

    The Open Journal of Astrophysics , keywords =

    Understanding the Neutron Star Population with the SKAO telescopes. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.154653 , archivePrefix =. 2512.16156 , primaryClass =

    doi

  114. [227]

    The Open Journal of Astrophysics , keywords =

    Pulsar Science with the SKA Observatory. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.154638 , archivePrefix =. 2512.16152 , primaryClass =

    doi

  115. [228]

    , keywords =

    The Australia Telescope National Facility Pulsar Catalogue. , keywords =. doi:10.1086/428488 , archivePrefix =. astro-ph/0412641 , primaryClass =

    doi arXiv

  116. [229]

    , keywords =

    The mass distribution and gravitational potential of the Milky Way. , keywords =. doi:10.1093/mnras/stw2759 , archivePrefix =. 1608.00971 , primaryClass =

    doi arXiv

  117. [230]

    , keywords =

    On the Absorption of X-Rays in the Interstellar Medium. , keywords =. doi:10.1086/317016 , archivePrefix =. astro-ph/0008425 , primaryClass =

    doi arXiv

  118. [231]

    , keywords =

    Modelling spin evolution of magnetars. , keywords =. doi:10.1093/mnras/stab2677 , archivePrefix =. 2109.07484 , primaryClass =

    doi

  119. [232]

    Observing and data analysis systems, discovery and timing of 100 pulsars

    The Parkes multi-beam pulsar survey - I. Observing and data analysis systems, discovery and timing of 100 pulsars. , keywords =. doi:10.1046/j.1365-8711.2001.04751.x , archivePrefix =. astro-ph/0106522 , primaryClass =

    2001 doi

  120. [233]

    , keywords =

    Revisiting the radial distribution of pulsars in the Galaxy. , keywords =. doi:10.1051/0004-6361:20040152 , archivePrefix =. astro-ph/0405559 , primaryClass =

    doi arXiv

  121. [234]

    , keywords =

    A Model of the 8--25 Micron Point Source Infrared Sky. , keywords =. doi:10.1086/191733 , adsurl =

    doi

  122. [235]

    2024 , url =

    The Chandra Proposers' Observatory Guide , author =. 2024 , url =

    2024

  123. [236]

    , keywords =

    A search for low-luminosity pulsars. , keywords =. doi:10.1086/184502 , adsurl =

    doi

  124. [237]

    , keywords =

    A Unified Model of the Magnetar and Radio Pulsar Bursting Phenomenology. , keywords =. doi:10.1088/2041-8205/727/2/L51 , archivePrefix =. 1101.1098 , primaryClass =

    doi arXiv

  125. [238]

    , keywords =

    Origin and evolution of magnetars. , keywords =. doi:10.1111/j.1745-3933.2008.00527.x , archivePrefix =. 0807.2106 , primaryClass =

    2008 doi

  126. [239]

    , keywords =

    Initial periods and magnetic fields of neutron stars. , keywords =. doi:10.1093/mnras/stac1648 , archivePrefix =. 2205.06823 , primaryClass =

    doi

  127. [240]

    Reports on Progress in Physics , keywords =

    Observational diversity of magnetized neutron stars. Reports on Progress in Physics , keywords =. doi:10.1088/1361-6633/ab3def , adsurl =

    doi

  128. [241]

    , keywords =

    Population synthesis studies of isolated neutron stars with magnetic field decay. , keywords =. doi:10.1111/j.1365-2966.2009.15850.x , archivePrefix =. 0910.2190 , primaryClass =

    2009 doi

  129. [242]

    , keywords =

    Chandra X-Ray Detection of the High Magnetic Field Radio Pulsar PSR J1718-3718. , keywords =. doi:10.1086/427628 , archivePrefix =. astro-ph/0411615 , primaryClass =

    doi arXiv

  130. [243]

    , keywords =

    The Braking Index of PSR J1734-3333 and the Magnetar Population. , keywords =. doi:10.1088/2041-8205/741/1/L13 , archivePrefix =. 1109.2740 , primaryClass =

    doi arXiv

  131. [244]

    , keywords =

    New long-term braking index measurements for glitching pulsars using a glitch-template method. , keywords =. doi:10.1093/mnras/stw3081 , archivePrefix =. 1611.08314 , primaryClass =

    doi arXiv

  132. [245]

    , keywords =

    Quantitative Age Estimation of Supernova Remanants and Associated Pulsars. , keywords =. doi:10.3847/1538-4357/abfb02 , archivePrefix =. 2104.10052 , primaryClass =

    doi

  133. [246]

    Advances in Space Research , keywords =

    A census of high-energy observations of Galactic supernova remnants. Advances in Space Research , keywords =. doi:10.1016/j.asr.2012.02.004 , archivePrefix =. 1202.0245 , primaryClass =

    2012 doi arXiv

  134. [247]

    , keywords =

    An exceptionally bright flare from SGR 1806-20 and the origins of short-duration -ray bursts. , keywords =. doi:10.1038/nature03519 , archivePrefix =. astro-ph/0502329 , primaryClass =

    doi arXiv

  135. [248]

    arXiv e-prints , keywords =

    Transient narrowband radio bursts from 1E 1547.0-5408. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.21450 , archivePrefix =. 2603.21450 , primaryClass =

    doi

  136. [249]

    The Astronomer's Telegram , keywords =

    Swift J1822.3-1606: A Probable New SGR in Ground Analysis of BAT Data. The Astronomer's Telegram , keywords =

  137. [250]

    , keywords =

    Discovery of a New Soft Gamma Repeater: SGR J0418 + 5729. , keywords =. doi:10.1088/2041-8205/711/1/L1 , archivePrefix =. 0911.5544 , primaryClass =

    doi arXiv

  138. [251]

    , eprint =

    Statistical Properties of SGR 1806-20 Bursts. , eprint =. doi:10.1086/312583 , adsurl =

    doi

  139. [252]

    , keywords =

    The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog. , keywords =. doi:10.3847/0004-637X/829/1/7 , archivePrefix =. 1606.01956 , primaryClass =

    doi arXiv

  140. [253]

    , keywords =

    The Fourth Fermi-GBM Gamma-Ray Burst Catalog: A Decade of Data. , keywords =. doi:10.3847/1538-4357/ab7a18 , archivePrefix =. 2002.11460 , primaryClass =

    2002 doi

  141. [254]

    The Giant Flare of 1998 August 27 from SGR 1900+14. I. An Interpretive Study of BeppoSAX and Ulysses Observations. , keywords =. doi:10.1086/319441 , archivePrefix =. astro-ph/0010494 , primaryClass =

    1998 doi arXiv

  142. [255]

    , keywords =

    Observations of a flaring X-ray pulsar in Dorado. , keywords =. doi:10.1038/282587a0 , adsurl =

    doi

  143. [256]

    , keywords =

    Hubble Space Telescope Observations of SGR 0526-66: New Constraints on Accretion and Magnetar Models. , keywords =. doi:10.1086/323516 , archivePrefix =. astro-ph/0103179 , primaryClass =

    doi arXiv

  144. [257]

    , keywords =

    A giant -ray flare from the magnetar SGR 1806 - 20. , keywords =. doi:10.1038/nature03525 , archivePrefix =. astro-ph/0503030 , primaryClass =

    doi arXiv

  145. [258]

    Bulletin of the American Astronomical Society , year = 2019, volume =

    The DSA-2000 A Radio Survey Camera. Bulletin of the American Astronomical Society , year = 2019, volume =. doi:10.48550/arXiv.1907.07648 , archivePrefix =. 1907.07648 , primaryClass =

    2000 doi arXiv

  146. [259]

    Astronomy Reports , year = 2017, month = apr, volume =

    Square Kilometre Array: The radio telescope of the XXI century. Astronomy Reports , year = 2017, month = apr, volume =. doi:10.1134/S1063772917040059 , adsurl =

    2017 doi

  147. [260]

    American Astronomical Society Meeting Abstracts \#243 , year = 2024, series =

    The DSA-2000 Fast Time Domain Search for Pulsars and Fast Radio Bursts. American Astronomical Society Meeting Abstracts \#243 , year = 2024, series =

    2000

  148. [261]

    XMM-Newton observatory. I. The spacecraft and operations. , keywords =. doi:10.1051/0004-6361:20000036 , adsurl =

    doi

  149. [262]

    , keywords =

    Radio polarization measurements from RRAT J1819-1458. , keywords =. doi:10.1111/j.1745-3933.2009.00671.x , archivePrefix =. 0905.1250 , primaryClass =

    2009 doi

  150. [263]

    The ``Magnificent Seven'' X-Ray Isolated Neutron Stars Revisited. I. Improved Timing Solutions and Pulse Profile Analysis. , keywords =. doi:10.3847/1538-4357/ad452b , archivePrefix =. 2407.00275 , primaryClass =

    doi

  151. [264]

    Universe , keywords =

    The Zoo of Isolated Neutron Stars. Universe , keywords =. doi:10.3390/universe9060273 , archivePrefix =. 2306.02084 , primaryClass =

    doi

  152. [265]

    , keywords =

    Learning about the magnetar Swift J1834.9-0846 from its wind nebula. , keywords =. doi:10.1093/mnras/stw2554 , archivePrefix =. 1608.06994 , primaryClass =

    doi arXiv

  153. [266]

    , keywords =

    Swift Discovery of a New Soft Gamma Repeater, SGR J1745-29, near Sagittarius A*. , keywords =. doi:10.1088/2041-8205/770/2/L24 , archivePrefix =. 1305.2128 , primaryClass =

    doi arXiv

  154. [267]

    , keywords =

    VLA and XMM-Newton Observations of the SNR W41/TeV Gamma-Ray Source HESS J1834-087. , keywords =. doi:10.1086/512544 , archivePrefix =. astro-ph/0612296 , primaryClass =

    doi arXiv

  155. [268]

    , keywords =

    A New Low Magnetic Field Magnetar: The 2011 Outburst of Swift J1822.3-1606. , keywords =. doi:10.1088/0004-637X/754/1/27 , archivePrefix =. 1203.6449 , primaryClass =

    2011 doi arXiv

  156. [269]

    , keywords =

    MeV-GeV Gamma-Ray Emission from SNR G327.1-1.1 Discovered by the Fermi-LAT. , keywords =. doi:10.3847/1538-4357/ac9eb4 , archivePrefix =. 2211.10281 , primaryClass =

    doi

  157. [270]

    , keywords =

    Multiwavelength Investigation of Pulsar Wind Nebula DA 495 with HAWC, VERITAS, and NuSTAR. , keywords =. doi:10.3847/1538-4357/ab21d0 , archivePrefix =. 1905.07327 , primaryClass =

    1905 doi arXiv

  158. [271]

    , keywords =

    A Model of the Spectral Evolution of Pulsar Wind Nebulae. , keywords =. doi:10.1088/0004-637X/715/2/1248 , archivePrefix =. 1004.3098 , primaryClass =

    doi arXiv

  159. [272]

    arXiv e-prints , keywords =

    Constraining the Pulsar Beaming Fraction with TeV-Selected Galactic Pulsar Wind Nebulae and unidentified TeV Sources. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.16187 , archivePrefix =. 2604.16187 , primaryClass =

    doi arXiv

  160. [273]

    , keywords =

    Two unseen massive white dwarf candidates in close binaries. , keywords =. doi:10.1093/pasj/psaf148 , archivePrefix =. 2509.12808 , primaryClass =

    doi

  161. [274]

    , keywords =

    The protomagnetar model for gamma-ray bursts. , keywords =. doi:10.1111/j.1365-2966.2011.18280.x , archivePrefix =. 1012.0001 , primaryClass =

    2011 doi

  162. [275]

    , keywords =

    Gamma-Ray Burst Afterglow with Continuous Energy Injection: Signature of a Highly Magnetized Millisecond Pulsar. , keywords =. doi:10.1086/320255 , archivePrefix =. astro-ph/0011133 , primaryClass =

    doi arXiv

  163. [276]

    Astronomy Reports , keywords =

    Magnetic fields of radio pulsars. Astronomy Reports , keywords =. doi:10.1134/S1063772917070058 , archivePrefix =. 1608.08525 , primaryClass =

    doi arXiv

  164. [277]

    , keywords =

    Modelling of isolated radio pulsars and magnetars on the fossil field hypothesis. , keywords =. doi:10.1111/j.1365-2966.2006.10058.x , archivePrefix =. astro-ph/0601258 , primaryClass =

    2006 doi

Pith tools

Reviewed June 26, 2026 · model on record in the stance chip above.