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arxiv: 2604.07734 · v1 · submitted 2026-04-09 · 🌌 astro-ph.HE

Recognition: unknown

Resolving the 2024 Outburst of Magnetar 1E 1841-045 from its host Supernova Remnant with EP-FXT

Yu-Cong Fu , Lin Lin , Yu-Jia Zheng , Ming-Yu Ge , Han-Long Peng , Dong-Ming Li , Francesco Coti Zelati , Ersin G\"o\v{g}\"u\c{s}
show 6 more authors
Nanda Rea Bing Zhang Wei-Wei Zhu Ke-Jia Lee Teruaki Enoto Chryssa Kouveliotou
Authors on Pith no claims yet

Pith reviewed 2026-05-10 17:35 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords magnetar1E 1841-045X-ray outburstpulse profilephase-resolved spectroscopysupernova remnantblackbody emissionEinstein Probe
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The pith

High-resolution imaging of the 2024 magnetar outburst isolates its emission from the supernova remnant, revealing a 20% flux increase and blackbody temperature correlations with pulse intensity.

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

The paper analyzes X-ray data from the Einstein Probe on the magnetar 1E 1841-045 after its active episode began in August 2024. It reports a roughly 20% rise in the 0.5-10 keV flux relative to pre-outburst levels, modeled with a blackbody plus power-law spectrum. The pulse profile shows multiple peaks with shifts, and the dominant peak switches above 5.8 keV. Phase-resolved spectroscopy ties blackbody temperature directly to pulse intensity while noting spectral hardening at one phase. The instrument's spatial resolution is presented as the key to subtracting the surrounding supernova remnant and obtaining the magnetar's intrinsic pulsed signal.

Core claim

The magnetar 1E 1841-045 exhibited a new active episode starting on August 20, 2024, marked by X-ray bursts and enhanced persistent emission. Using data from the Einstein Probe, the pulse profile displays a multi-peaked structure, with notable phase shifts in the secondary peak. Energy-resolved pulse profile analysis indicates a transition in the dominant peak of the pulse profile above 5.8 keV. The 0.5-10 keV X-ray spectrum is well-modeled by a combined blackbody and power-law model, showing a ~20% flux increase following the outburst. Phase-resolved spectroscopy indicates a correlation between blackbody temperature and pulse profile intensity, along with spectral hardening at a specific脉冲相

What carries the argument

High spatial resolution of the Einstein Probe Follow-up X-ray Telescope combined with phase-resolved spectroscopy to separate the magnetar's pulsed emission from the host supernova remnant background.

If this is right

  • The magnetar's 0.5-10 keV persistent flux rose by about 20% after the outburst onset.
  • Pulse profiles evolve with energy, showing a dominant-peak transition above 5.8 keV and secondary-peak phase shifts.
  • Blackbody temperature correlates with pulse-profile intensity across phases.
  • Spectral hardening appears at one specific phase in the rotation cycle.
  • Subtracting the supernova remnant is required to recover the true intrinsic pulse properties.

Where Pith is reading between the lines

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

  • The same high-resolution separation method could be applied to other magnetars still inside their remnants to improve outburst statistics.
  • The temperature-intensity link points to outburst heating that varies across the neutron-star surface.
  • Continued monitoring with similar instruments may reveal whether 20% flux jumps are common during magnetar activation episodes.
  • The phase-specific hardening could connect to localized magnetic-field structures that future polarization measurements might test.

Load-bearing premise

The Einstein Probe's spatial resolution fully isolates the magnetar's pulsed X-ray emission from the supernova remnant without significant residual contamination that could change the reported 20% flux increase or the phase-resolved spectral correlations.

What would settle it

Independent observations with another high-resolution X-ray instrument that measure no 20% flux increase or different blackbody temperature versus intensity correlations after subtracting the remnant emission would contradict the central results.

Figures

Figures reproduced from arXiv: 2604.07734 by Bing Zhang, Chryssa Kouveliotou, Dong-Ming Li, Ersin G\"o\v{g}\"u\c{s}, Francesco Coti Zelati, Han-Long Peng, Ke-Jia Lee, Lin Lin, Ming-Yu Ge, Nanda Rea, Teruaki Enoto, Wei-Wei Zhu, Yu-Cong Fu, Yu-Jia Zheng.

Figure 1
Figure 1. Figure 1: Observation timelines for different instruments. The dark vertical bars in each panel indicate the observation epochs. The arrows mark the time of the short bursts reported in the references. In panel (e), the purple arrows correspond to bursts detected by Swift/BAT, while the black and green arrows represent the bursts detected by Fermi/GBM and SVOM/GRM, respectively. The dashed and dotted vertical lines … view at source ↗
Figure 2
Figure 2. Figure 2: Logarithmic scale images of 1E 1841–045 captured by FXT-A (left) and FXT-B (right) of Obs. ID 06800000059 (MJD 60552.62). The blue rectangular areas indicate the FXT fields of view in PW mode. A black circle with a 30-arcsecond radius displays the central source. A white annulus with a 40-arcsecond inner radius and a 100-arcsecond outer radius displays the surrounding SNR. The color bar shows the counts pe… view at source ↗
Figure 3
Figure 3. Figure 3: The average pulse profiles of 1E 1841–045 during two epochs observed by FXT in the 0.5–10 keV band. Epoch I represents the pulse profile before the outburst, correspond￾ing to Obs. ID 11908432129 on MJD 60505.57. Epoch II rep￾resents the average pulse profile after the outburst, spanning from MJD 60544.74 to MJD 60582.45. The phase of epoch I is aligned to epoch II using circular cross-correlation. The sol… view at source ↗
Figure 4
Figure 4. Figure 4: The colors representing the values of the pulse profile are normalized by the Pulse/Average count rate, the red represents pulse-on phase, and the blue repre￾sents pulse-off phase. The phase and shape of peak II 0.0 0.5 1.0 1.5 2.0 Phase 0.6 0.8 1.0 1.2 1.4 Norm (Count/Average) Epoch I Epoch II [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The evolution of the pulse profiles over energy for FXT(0.5–10 keV). The values of the pulse profiles are nor￾malized by the Pulse/Average count rate, generated from the combined data spanning from MJD 60544.74 to MJD 60582.45 (Epoch II in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The evolution of the pulsed fraction (PF) of 1E 1841–045. (a): The evolution of PF over time, with the red dashed line representing the average value. (b): The evolu￾tion of PF over energy. The horizontal error bars denote the energy bin widths, with each point plotted at the bin cen￾troid. The red solid line shows the weighted linear fit, with the red shaded area representing the 1σ statistical uncertain￾… view at source ↗
Figure 7
Figure 7. Figure 7: Spectra and residuals from Obs. ID 06800000059. The spectra from FXT-A and FXT-B are extracted separately and fitted jointly. (a): The total model (black solid line) is shown alongside its individual components: a blackbody (red dashed line) and a power-law (blue dashed line). (b): The total model (black solid line) is shown alongside its individual components: a cooler blackbody (red dashed line) and a ho… view at source ↗
Figure 8
Figure 8. Figure 8: Temporal evolution of spectral parameters: blackbody temperature, emission radius, power-law photon index, unabsorbed total flux, and the fractional contribution of the blackbody flux to the total flux. The source radius in kilometers is calculated from the distance of 8.5 kpc (Tian & Leahy 2008). The dashed horizontal line indicates the mean value across all parameters. The dashed vertical line indi￾cates… view at source ↗
Figure 9
Figure 9. Figure 9: Fitting results of the phase-resolved spectral analysis of the BB+PL model. Solid lines represent the pulse profiles as shown in [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Fitting results of the phase-resolved spectral analysis of the BB+BB model. The blue dashed horizontal line indicates the constant fit result for the hotter BB temperature (1.93 ± 0.08 keV), with the gray shaded region representing the 1σ uncertainty. The blue vertical band highlights the phase interval corresponding to peak III. The source radius in kilometers is calculated from the distance of 8.5 kpc (… view at source ↗
read the original abstract

The magnetar 1E 1841-045 exhibited a new active episode starting on August 20, 2024, marked by X-ray bursts and enhanced persistent emission. Using data from the Einstein Probe (EP), we report on the timing and spectral results following the onset of this outburst. The pulse profile displays a multi-peaked structure, with notable phase shifts in the secondary peak. Energy-resolved pulse profile analysis indicates a transition in the dominant peak of the pulse profile above 5.8 keV. The 0.5-10 keV X-ray spectrum is well-modeled by a combined blackbody and power-law (BB+PL) model, showing a $\sim 20\%$ flux increase following the outburst. Phase-resolved spectroscopy indicates a correlation between BB temperature and pulse profile intensity, along with spectral hardening at a specific pulse phase. The high spatial resolution of EP enables effective separation of the supernova remnant emission, which is crucial for measuring the intrinsic pulse emission of the source. These findings underscore the intricate relationship between magnetar outbursts, pulse profile evolution, and spectral characteristics.

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

2 major / 2 minor

Summary. The paper reports on the 2024 outburst of magnetar 1E 1841-045 observed with the Einstein Probe (EP), focusing on timing and spectral properties. It describes a multi-peaked pulse profile with phase shifts in the secondary peak, an energy-dependent transition where the dominant peak changes above 5.8 keV, and a ~20% increase in 0.5-10 keV flux. The spectrum is modeled with a blackbody plus power-law (BB+PL) component. Phase-resolved spectroscopy shows a correlation between blackbody temperature and pulse intensity, plus spectral hardening at one phase. The high spatial resolution of EP is credited with separating the magnetar's emission from its host supernova remnant.

Significance. If the results are robust, the work adds useful observational constraints on magnetar outburst evolution, including how pulse profiles and spectra change together. The phase-resolved temperature-intensity correlation could inform emission geometry models, and the EP resolution demonstration is relevant for future X-ray studies of sources embedded in SNRs. The observational nature means impact depends on reproducibility and statistical rigor.

major comments (2)
  1. Abstract: The ~20% flux increase and the BB temperature-pulse intensity correlation are presented without error bars, reduced chi-squared values, degrees of freedom, or details on background subtraction and data exclusion. These omissions directly affect assessment of whether the reported changes and correlations are statistically significant.
  2. Spectral and timing results sections: The claim that EP's spatial resolution fully isolates the pulsed emission from SNR contamination (central to the flux increase and phase-resolved findings) lacks quantitative limits on residual contamination or tests of background subtraction accuracy, leaving open the possibility that the 20% flux change and correlations are affected by incomplete separation.
minor comments (2)
  1. Abstract: The description of 'notable phase shifts in the secondary peak' would benefit from specifying the approximate phase offset or direction to make the timing results more immediately interpretable.
  2. Overall: Standard X-ray analysis details such as the exact energy bands used for pulse profiles, phase binning choices, and any cross-calibration with other instruments are not mentioned in the provided text and should be added for reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful review and constructive comments on our manuscript. We address each major comment below and have revised the manuscript accordingly to improve statistical transparency and quantitative support for our claims regarding source separation.

read point-by-point responses

  1. Referee: Abstract: The ~20% flux increase and the BB temperature-pulse intensity correlation are presented without error bars, reduced chi-squared values, degrees of freedom, or details on background subtraction and data exclusion. These omissions directly affect assessment of whether the reported changes and correlations are statistically significant.

    Authors: We agree that the abstract summary omits key statistical details due to length constraints. In the revised manuscript we will add approximate uncertainties to the reported ~20% flux increase and note the statistical significance of the BB temperature-pulse intensity correlation. The full details—including reduced chi-squared values, degrees of freedom, background subtraction procedures, and data exclusion criteria—are already present in the spectral fitting and phase-resolved spectroscopy sections; we will ensure explicit cross-references from the abstract and results summary to these sections. revision: yes

  2. Referee: Spectral and timing results sections: The claim that EP's spatial resolution fully isolates the pulsed emission from SNR contamination (central to the flux increase and phase-resolved findings) lacks quantitative limits on residual contamination or tests of background subtraction accuracy, leaving open the possibility that the 20% flux change and correlations are affected by incomplete separation.

    Authors: We acknowledge that the manuscript would benefit from explicit quantitative limits. In the revised version we will add estimates of residual SNR contamination derived from the EP-FXT point-spread function convolved with the known SNR extent, together with tests of background subtraction accuracy using multiple off-source regions and Monte Carlo simulations of possible leakage. These additions will place upper limits on any residual contribution to the pulsed flux and phase-resolved spectra. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational data reporting

full rationale

The manuscript presents timing and spectral measurements from EP-FXT observations of the 2024 magnetar outburst. Reported quantities include multi-peaked pulse profiles with phase shifts, energy-dependent peak transitions above 5.8 keV, a ~20% flux increase in the 0.5-10 keV band, and phase-resolved BB temperature correlations with intensity. All results are obtained via standard X-ray timing analysis and BB+PL spectral fitting applied directly to the data. The claim that EP's spatial resolution separates the magnetar from SNR emission is an instrumental justification, not a derivation that reduces to fitted inputs. No equations, theoretical models, predictions, or self-citations are load-bearing; the derivation chain is empty and self-contained against external data.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard X-ray astronomy practices for modeling magnetar spectra and subtracting background; no new entities or ad-hoc parameters beyond routine spectral fits are introduced.

free parameters (1)
  • Blackbody temperature, power-law index, and normalization in BB+PL spectral model
    Fitted parameters in the spectral model used to describe the 0.5-10 keV data.
axioms (2)
  • domain assumption Magnetar persistent emission can be adequately described by a blackbody plus power-law component
    Standard modeling choice in high-energy astrophysics for magnetars, invoked implicitly for the spectral fits.
  • domain assumption EP-FXT spatial resolution is sufficient to separate point-source pulsed emission from extended supernova remnant emission
    Central to the claim that intrinsic magnetar properties are measured.

pith-pipeline@v0.9.0 · 5575 in / 1571 out tokens · 81867 ms · 2026-05-10T17:35:03.042532+00:00 · methodology

discussion (0)

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Works this paper leans on

70 extracted references · 57 canonical work pages

  1. [1]

    M., et al

    An, H., Hasco¨ et, R., Kaspi, V. M., et al. 2013, ApJ, 779, 163, doi: 10.1088/0004-637X/779/2/163

    work page doi:10.1088/0004-637x/779/2/163 2013

  2. [2]

    F., Hasco¨ et, R., et al

    An, H., Archibald, R. F., Hasco¨ et, R., et al. 2015, ApJ, 807, 93, doi: 10.1088/0004-637X/807/1/93

    work page doi:10.1088/0004-637x/807/1/93 2015

  3. [3]

    F., Kaspi, V

    Archibald, R. F., Kaspi, V. M., Ng, C.-Y., et al. 2013, Nature, 497, 591, doi: 10.1038/nature12159

    work page doi:10.1038/nature12159 2013

  4. [4]

    Arnaud, K. A. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes, 17 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et a...

    work page doi:10.1051/0004-6361/201322068 1996

  5. [5]

    2025, ApJ, 979, 122, doi: 10.3847/1538-4357/ada3c4

    Bai, J., Wang, N., Dai, S., et al. 2025, ApJ, 979, 122, doi: 10.3847/1538-4357/ada3c4

    work page doi:10.3847/1538-4357/ada3c4 2025

  6. [6]

    Beloborodov, A. M. 2009, ApJ, 703, 1044, doi: 10.1088/0004-637X/703/1/1044 —. 2013, ApJ, 762, 13, doi: 10.1088/0004-637X/762/1/13

    work page doi:10.1088/0004-637x/703/1/1044 2009

  7. [7]

    M., & Li, X

    Beloborodov, A. M., & Li, X. 2016, ApJ, 833, 261, doi: 10.3847/1538-4357/833/2/261

    work page doi:10.3847/1538-4357/833/2/261 2016

  8. [8]

    2020, ApJL, 902, L2, doi: 10.3847/2041-8213/aba82a

    Borghese, A., Coti Zelati, F., Rea, N., et al. 2020, ApJL, 902, L2, doi: 10.3847/2041-8213/aba82a

    work page doi:10.3847/2041-8213/aba82a 2020

  9. [9]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Burgay, M., Rea, N., Israel, G. L., et al. 2006, MNRAS, 372, 410, doi: 10.1111/j.1365-2966.2006.10872.x

    work page doi:10.1111/j.1365-2966.2006.10872.x 2006

  10. [10]

    2024, GRB Coordinates Network, 37606, 1 16

    Cai, C., Li, X.-B., Xiong, S.-L., et al. 2024, GRB Coordinates Network, 37606, 1 16

    2024

  11. [11]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Chen, Y., Cui, W., Han, D., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11444, Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, ed. J.-W. A. den Herder, S. Nikzad, & K. Nakazawa, 114445B, doi: 10.1117/12.2562311 Coti Zelati, F., Rea, N., Pons, J. A., Campana, S., &

    work page doi:10.1117/12.2562311 2020

  12. [12]

    2018, MNRAS, 474, 961, doi: 10.1093/mnras/stx2679

    Esposito, P. 2018, MNRAS, 474, 961, doi: 10.1093/mnras/stx2679

    work page doi:10.1093/mnras/stx2679 2018

  13. [13]

    J., Dichiara, S., Lien, A

    DeLaunay, J. J., Dichiara, S., Lien, A. Y., Parsotan, T. M., & Neil Gehrels Swift Observatory Team. 2024, GRB Coordinates Network, 37211, 1

    2024

  14. [14]

    Dib, R., & Kaspi, V. M. 2014, ApJ, 784, 37, doi: 10.1088/0004-637X/784/1/37

    work page doi:10.1088/0004-637x/784/1/37 2014

  15. [15]

    M., & Neil Gehrels Swift Observatory Team

    Dichiara, S., Palmer, D. M., & Neil Gehrels Swift Observatory Team. 2024, GRB Coordinates Network, 37222, 1

    2024

  16. [16]

    C., & Thompson, C

    Duncan, R. C., & Thompson, C. 1992, ApJL, 392, L9, doi: 10.1086/186413

    work page doi:10.1086/186413 1992

  17. [17]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Edwards, R. T., Hobbs, G. B., & Manchester, R. N. 2006, MNRAS, 372, 1549, doi: 10.1111/j.1365-2966.2006.10870.x

    work page doi:10.1111/j.1365-2966.2006.10870.x 2006

  18. [18]

    2017, ApJS, 231, 8, doi: 10.3847/1538-4365/aa6f0a

    Enoto, T., Shibata, S., Kitaguchi, T., et al. 2017, ApJS, 231, 8, doi: 10.3847/1538-4365/aa6f0a

    work page doi:10.3847/1538-4365/aa6f0a 2017

  19. [19]

    2025, ApJ, 980, 99, doi: 10.3847/1538-4357/ada936

    Fu, Y.-C., Lin, L., Ge, M.-Y., et al. 2025, ApJ, 980, 99, doi: 10.3847/1538-4357/ada936

    work page doi:10.3847/1538-4357/ada936 2025

  20. [20]

    M., Ding, G

    Fu, Y.-C., Song, L. M., Ding, G. Q., et al. 2023, MNRAS, 521, 893, doi: 10.1093/mnras/stad614

    work page doi:10.1093/mnras/stad614 2023

  21. [21]

    P., Kaspi, V

    Gavriil, F. P., Kaspi, V. M., & Woods, P. M. 2004, ApJ, 607, 959, doi: 10.1086/383564

    work page doi:10.1086/383564 2004

  22. [22]

    Y., Lu, F

    Ge, M. Y., Lu, F. J., Qu, J. L., et al. 2012, ApJS, 199, 32, doi: 10.1088/0067-0049/199/2/32

    work page doi:10.1088/0067-0049/199/2/32 2012

  23. [23]

    Y., Lu, F

    Ge, M. Y., Lu, F. J., Yan, L. L., et al. 2019, Nature Astronomy, 3, 1122, doi: 10.1038/s41550-019-0853-5

    work page doi:10.1038/s41550-019-0853-5 2019

  24. [24]

    2024, Research in Astronomy and Astrophysics, 24, 015016, doi: 10.1088/1674-4527/ad0f0c

    Ge, M.-Y., Yang, Y.-P., Lu, F.-J., et al. 2024, Research in Astronomy and Astrophysics, 24, 015016, doi: 10.1088/1674-4527/ad0f0c

    work page doi:10.1088/1674-4527/ad0f0c 2024

  25. [25]

    V., Vasisht, G., & Dotani, T

    Gotthelf, E. V., Vasisht, G., & Dotani, T. 1999, ApJL, 522, L49, doi: 10.1086/312220

    work page doi:10.1086/312220 1999

  26. [26]

    apj , keywords =

    Huppenkothen, D., Bachetti, M., Stevens, A. L., et al. 2019, ApJ, 881, 39, doi: 10.3847/1538-4357/ab258d

    work page doi:10.3847/1538-4357/ab258d 2019

  27. [27]

    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

    work page doi:10.1088/1674-4527/20/5/64 2020

  28. [28]

    1998, Nature, 393, 235, doi: 10.1038/30410

    Kouveliotou, C., Dieters, S., Strohmayer, T., et al. 1998, Nature, 393, 235, doi: 10.1038/30410

    work page doi:10.1038/30410 1998

  29. [29]

    A., Becker, R

    Kriss, G. A., Becker, R. H., Helfand, D. J., & Canizares, C. R. 1985, ApJ, 288, 703, doi: 10.1086/162836

    work page doi:10.1086/162836 1985

  30. [30]

    R., & Collmar, W

    Kuiper, L., Hermsen, W., den Hartog, P. R., & Collmar, W. 2006, ApJ, 645, 556, doi: 10.1086/504317

    work page doi:10.1086/504317 2006

  31. [31]

    2004, ApJ, 613, 1173, doi: 10.1086/423129

    Kuiper, L., Hermsen, W., & Mendez, M. 2004, ApJ, 613, 1173, doi: 10.1086/423129

    work page doi:10.1086/423129 2004

  32. [32]

    M., Champion, D

    Lazarus, P., Kaspi, V. M., Champion, D. J., Hessels, J. W. T., & Dib, R. 2012, ApJ, 744, 97, doi: 10.1088/0004-637X/744/2/97

    work page doi:10.1088/0004-637x/744/2/97 2012

  33. [33]

    Leahy, D. A. 1987, A&A, 180, 275

    1987

  34. [34]

    2011, ApJL, 740, L16, doi: 10.1088/2041-8205/740/1/L16

    Lin, L., Kouveliotou, C., G¨ oˇ g¨ u¸ s, E., et al. 2011, ApJL, 740, L16, doi: 10.1088/2041-8205/740/1/L16

    work page doi:10.1088/2041-8205/740/1/l16 2011

  35. [35]

    F., Wang, P., et al

    Lin, L., Zhang, C. F., Wang, P., et al. 2020, Nature, 587, 63, doi: 10.1038/s41586-020-2839-y

    work page doi:10.1038/s41586-020-2839-y 2020

  36. [36]

    2025, Nature Astronomy, doi: 10.1038/s41550-024-02449-8

    Liu, Y., Sun, H., Xu, D., et al. 2025, Nature Astronomy, doi: 10.1038/s41550-024-02449-8

    work page doi:10.1038/s41550-024-02449-8 2025

  37. [37]

    2012, Pulsar Astronomy

    Lyne, A., & Graham-Smith, F. 2012, Pulsar Astronomy

    2012

  38. [38]

    Lyutikov, M., & Gavriil, F. P. 2006, MNRAS, 368, 690, doi: 10.1111/j.1365-2966.2006.10140.x

    work page doi:10.1111/j.1365-2966.2006.10140.x 2006

  39. [39]

    2024, GRB Coordinates Network, 38148, 1

    Mereghetti, S., Gotz, D., Ferrigno, C., et al. 2024, GRB Coordinates Network, 38148, 1

    2024

  40. [40]

    , keywords =

    Mereghetti, S., Pons, J. A., & Melatos, A. 2015, SSRv, 191, 315, doi: 10.1007/s11214-015-0146-y

    work page doi:10.1007/s11214-015-0146-y 2015

  41. [41]

    2010, PASJ, 62, 1249, doi: 10.1093/pasj/62.5.1249

    Morii, M., Kitamoto, S., Shibazaki, N., et al. 2010, PASJ, 62, 1249, doi: 10.1093/pasj/62.5.1249

    work page doi:10.1093/pasj/62.5.1249 2010

  42. [42]

    P., et al

    Ng, M., Younes, G., Hu, C. P., et al. 2024, The Astronomer’s Telegram, 16789, 1

    2024

  43. [43]

    The McGill Magnetar Catalog.ApJ Suppl

    Olausen, S. A., & Kaspi, V. M. 2014, ApJS, 212, 6, doi: 10.1088/0067-0049/212/1/6

    work page doi:10.1088/0067-0049/212/1/6 2014

  44. [44]

    2026, ApJ, 999, 85, doi: 10.3847/1538-4357/ae4007

    Peng, H.-L., Weng, S.-S., Ge, M.-Y., et al. 2026, ApJ, 999, 85, doi: 10.3847/1538-4357/ae4007

    work page doi:10.3847/1538-4357/ae4007 2026

  45. [45]

    Ranasinghe, S., & Leahy, D. A. 2018, AJ, 155, 204, doi: 10.3847/1538-3881/aab9be

    work page doi:10.3847/1538-3881/aab9be 2018

  46. [46]

    2026, in Encyclopedia of

    Rea, N., & De Grandis, D. 2026, in Encyclopedia of

    2026

  47. [47]

    3, 205–222, doi: 10.1016/B978-0-443-21439-4.00096-1

    Astrophysics, Vol. 3, 205–222, doi: 10.1016/B978-0-443-21439-4.00096-1

    work page doi:10.1016/b978-0-443-21439-4.00096-1

  48. [48]

    2025, ApJL, 985, L34, doi: 10.3847/2041-8213/adbffb

    Rigoselli, M., Taverna, R., Mereghetti, S., et al. 2025, ApJL, 985, L34, doi: 10.3847/2041-8213/adbffb

    work page doi:10.3847/2041-8213/adbffb 2025

  49. [49]

    J., Veres, P., de Barra, C., et al

    Roberts, O. J., Veres, P., de Barra, C., et al. 2024, GRB Coordinates Network, 37234, 1

    2024

  50. [50]

    A., Harding, A

    Stewart, R., Younes, G. A., Harding, A. K., et al. 2025, ApJL, 985, L35, doi: 10.3847/2041-8213/adbffa SVOM/GRM Team, Wang, C.-W., Dong, Y.-W., et al. 2024a, GRB Coordinates Network, 37297, 1 SVOM/GRM Team, Zhang, W.-L., Tan, W.-J., et al. 2024b, GRB Coordinates Network, 38192, 1

    work page doi:10.3847/2041-8213/adbffa 2025

  51. [51]

    Thompson, C., & Duncan, R. C. 1993, ApJ, 408, 194, doi: 10.1086/172580

    work page doi:10.1086/172580 1993

  52. [52]

    Thompson, C., Lyutikov, M., & Kulkarni, S. R. 2002, ApJ, 574, 332, doi: 10.1086/340586

    work page doi:10.1086/340586 2002

  53. [53]

    W., & Leahy, D

    Tian, W. W., & Leahy, D. A. 2008, ApJ, 677, 292, doi: 10.1086/529120 17

    work page doi:10.1086/529120 2008

  54. [54]

    2010, Research in Astronomy and Astrophysics, 10, 553, doi: 10.1088/1674-4527/10/6/005

    Tong, H., Xu, R.-X., Peng, Q.-H., & Song, L.-M. 2010, Research in Astronomy and Astrophysics, 10, 553, doi: 10.1088/1674-4527/10/6/005

    work page doi:10.1088/1674-4527/10/6/005 2010

  55. [55]

    Vasisht, G., & Gotthelf, E. V. 1997, ApJL, 486, L129, doi: 10.1086/310843

    work page doi:10.1086/310843 1997

  56. [56]

    2015, ApJ, 815, 15, doi: 10.1088/0004-637X/815/1/15

    Weng, S.-S., & G¨ o˘ g¨ u¸ s, E. 2015, ApJ, 815, 15, doi: 10.1088/0004-637X/815/1/15

    work page doi:10.1088/0004-637x/815/1/15 2015

  57. [57]

    M., Kaspi, V

    Woods, P. M., Kaspi, V. M., Thompson, C., et al. 2004, ApJ, 605, 378, doi: 10.1086/382233

    work page doi:10.1086/382233 2004

  58. [58]

    I., Zhang, B.-B., Yang, J., et al

    Yin, Y.-H. I., Zhang, B.-B., Yang, J., et al. 2024, ApJL, 975, L27, doi: 10.3847/2041-8213/ad8652

    work page doi:10.3847/2041-8213/ad8652 2024

  59. [59]

    G., Kouveliotou, C., et al

    Younes, G., Baring, M. G., Kouveliotou, C., et al. 2017a, ApJ, 851, 17, doi: 10.3847/1538-4357/aa96fd

    work page doi:10.3847/1538-4357/aa96fd

  60. [60]

    P., Enoto, T., et al

    Younes, G., Hu, C. P., Enoto, T., et al. 2024, The Astronomer’s Telegram, 16802, 1

    2024

  61. [61]

    2017b, ApJ, 847, 85, doi: 10.3847/1538-4357/aa899a

    Younes, G., Kouveliotou, C., Jaodand, A., et al. 2017b, ApJ, 847, 85, doi: 10.3847/1538-4357/aa899a

    work page doi:10.3847/1538-4357/aa899a

  62. [62]

    2020, ApJL, 904, L21, doi: 10.3847/2041-8213/abc94c

    Younes, G., G¨ uver, T., Kouveliotou, C., et al. 2020, ApJL, 904, L21, doi: 10.3847/2041-8213/abc94c

    work page doi:10.3847/2041-8213/abc94c 2020

  63. [63]

    K., Baring, M

    Younes, G., Lander, S. K., Baring, M. G., et al. 2025, ApJ, 989, 89, doi: 10.3847/1538-4357/ade716

    work page doi:10.3847/1538-4357/ade716 2025

  64. [64]

    doi:10.1007/978-981-16-4544-0\_151-1

    Yuan, W., Zhang, C., Chen, Y., & Ling, Z. 2022, in Handbook of X-ray and Gamma-ray Astrophysics, ed. C. Bambi & A. Sangangelo, 86, doi: 10.1007/978-981-16-4544-0 151-1

    work page doi:10.1007/978-981-16-4544-0 2022

  65. [65]

    2025, Science China

    Yuan, W., Dai, L., Feng, H., et al. 2025, Science China

    2025

  66. [66]

    Physics, Mechanics, and Astronomy, 68, 239501, doi: 10.1007/s11433-024-2600-3

    work page doi:10.1007/s11433-024-2600-3

  67. [67]

    2025, Science China

    Zhang, W., Yuan, W., Ling, Z., et al. 2025, Science China

    2025

  68. [68]

    Physics, Mechanics, and Astronomy, 68, 219511, doi: 10.1007/s11433-024-2524-4

    work page doi:10.1007/s11433-024-2524-4

  69. [69]

    2024, GRB Coordinates Network, 37240, 1

    Zhang, W.-L., Xiong, S.-L., Tan, W.-J., Huang, Y., & Gecam Team. 2024, GRB Coordinates Network, 37240, 1

    2024

  70. [70]

    Zhu, W., & Kaspi, V. M. 2010, ApJ, 719, 351, doi: 10.1088/0004-637X/719/1/351

    work page doi:10.1088/0004-637x/719/1/351 2010