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arxiv: 2605.15724 · v1 · pith:W3KJC4JRnew · submitted 2026-05-15 · 🌌 astro-ph.HE

A Pilot Study of Mildly Recycled Pulsars: A Case Study of PSR J2338+4818

Yujie Chen , Yujie Lian , Yujie Wang , Liyun Zhang , Lei Qian , Zhichen Pan , Shuo Cao , Dejiang Yin
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Baoda Li Ruili He Tong Liu Wenze Li Yichi Zhang Yifeng Li Qiaoli Hao Jinyou Song Shuangyuan Chen Xingyi Wang Xianghua Niu Minglei Guo Menglin Huang
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Pith reviewed 2026-05-20 17:10 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords mildly recycled pulsarssingle pulse analysispulse nullinginterstellar scintillationPSR J2338+4818neutron star timingFAST observations
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The pith

No pulse nulling is detected in the mildly recycled pulsar PSR J2338+4818 across multiple observing bands.

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

This paper uses FAST observations to study the single-pulse behavior and interstellar scintillation of PSR J2338+4818 as a pilot case for understanding how mildly recycled pulsars form through short mass-transfer episodes with massive white-dwarf companions. The authors detect 27,228 single pulses with signal-to-noise ratio above 7 and apply a Markov Chain Monte Carlo analysis to test for pulse nulling. No evidence of nulling appears in any session, including in the 1.0-1.5 GHz and 300-600 MHz bands, even though earlier work had suggested possible long-term nulling. The same data yield measured scintillation timescales between 2.93 and 25.26 minutes and bandwidths between 1.68 and 27.41 MHz, with no clear scintillation arcs visible in the secondary spectra.

Core claim

The paper reports an updated timing solution for PSR J2338+4818 together with the result that no pulse nulling occurs during the observed epochs. A preliminary single-pulse search in the commissioning-phase ultra-wideband data and systematic searches in other bands find 27,228 pulses above S/N = 7. The MCMC analysis returns no nulling fraction, and the long-term nulling possibly seen in prior studies is absent from all current observations. Interstellar scintillation is detected, with the quoted ranges of timescale and bandwidth, yet the secondary spectra show no arcs.

What carries the argument

Markov Chain Monte Carlo analysis applied to single-pulse sequences to test for the presence of nulling states.

If this is right

  • Any long-term nulling previously reported must be either transient or confined to epochs not covered here.
  • The pulsar maintains steady emission across the sampled frequencies, consistent with a stable magnetospheric state.
  • Scintillation parameters supply new constraints on the turbulence scale of the interstellar medium along this line of sight.
  • Updated timing ephemeris supports continued precision monitoring to test evolutionary models for mildly recycled pulsars.

Where Pith is reading between the lines

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

  • If nulling remains absent over longer baselines, this object may represent a cleaner example of emission from a partially recycled neutron star than objects that show nulling.
  • The measured scintillation bandwidths and timescales can be combined with dispersion-measure variations to map small-scale structure in the local interstellar plasma.
  • The absence of scintillation arcs suggests that the scattering screen geometry for this pulsar does not produce the usual parabolic signature, which could be checked with higher-resolution dynamic spectra.

Load-bearing premise

The limited set of observation epochs and frequency bands is sufficient to rule out the long-term nulling reported in earlier studies.

What would settle it

A future monitoring campaign that records one or more clear episodes of pulse nulling in PSR J2338+4818 would show that nulling can occur intermittently and was simply missed in the present data set.

Figures

Figures reproduced from arXiv: 2605.15724 by Baoda Li, Dejiang Yin, Jinyou Song, Lei Qian, Liyun Zhang, Menglin Huang, Minglei Guo, Qiaoli Hao, Ruili He, Shuangyuan Chen, Shuo Cao, Tong Liu, Wenze Li, Xianghua Niu, Xingyi Wang, Yichi Zhang, Yifeng Li, Yujie Chen, Yujie Lian, Yujie Wang, Zhichen Pan.

Figure 1
Figure 1. Figure 1: Left: average pulse profiles at different frequencies. Right: timing residuals of PSR J2338+4818, including timing residuals as a function of MJD (upper subplot) and orbital phase (lower subplot). A black dashed vertical line marks the orbital phase of 0.25. To quantify the difference, we computed ∆Pb and σ∆Pb : ∆Pb = |Pb,now − Pb,previous| = 0.06242 days, (6) σ∆Pb = q σ 2 Pb,now + σ 2 Pb,previous ≈ 2.0 × … view at source ↗
Figure 2
Figure 2. Figure 2: The calibrated polarisation profile of PSR J2338+4818 at the central frequency of 1250 MHz from the observation on MJD 60553. The total intensity (I) is shown in black, the linear polarisation (L) in red, and the circular polarisation (V ) in blue. The polarisation position angle is shown in the top panel. where Ipeak is the peak intensity of the pulse and σp is the standard deviation of the off-pulse regi… view at source ↗
Figure 3
Figure 3. Figure 3: The 9 single pulses from PSR J2338+4818. Each subpanel consists of a normalized pulse profile and a frequency-phase diagram. The first row, from left to right, shows the three single pulses with the highest S/N from MJD 60666, MJD 60667, and MJD 60658. The second row displays three single pulses from MJD 60666, where scintillation is clearly noticeable at different times. The third row presents three singl… view at source ↗
Figure 4
Figure 4. Figure 4: Posterior probability distributions (derived from the observation at MJD 60666) of PSR J2338+4818 of the GMM parameters for the null and emission components, derived using the MCMC algorithm (see D. L. Kaplan et al. 2018; A. Anumarlapudi et al. 2023). The diagonal panels show the marginalized one-dimensional posteriors for each parameter, with vertical dashed lines marking the median values. where τ is the… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the integrated profiles for pulses identified as bursts (Pnull < 0.5; N = 59, 569) and nulls (Pnull ≥ 0.5; N = 234) for the observation on MJD 60347, where the profiles consist of 256 phase bins and are normalized for comparison. subsets corresponding to one-quarter, one-half, and the full sample, and stacked separately to form integrated profiles for each subset, with each individual pulse h… view at source ↗
Figure 6
Figure 6. Figure 6: Normalized average pulse profiles (top) and stacked single pulses (bottom) for low S/N pulses from the observation at MJD 60743. From left to right, the number of stacked pulses is 20, 200, 2000, and the total number of pulses satisfying S/N < 3 [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Pulse energy histograms (derived from the 35 observations except the ultra-wideband observation) for the ON-pulse and OFF-pulse windows of PSR J2338+4818. Individual ON and OFF histograms are shown as black hollow and dashed black boxes, respectively. The best-fitting GMM components are shown as filled regions: the null component (blue), the emission component (orange), and the sum of the null and emission… view at source ↗
Figure 8
Figure 8. Figure 8: Dynamic spectra (top panels), ACFs (bottom panels) of PSR J2338+4818. The integration times for these obser￾vations range from 1200 to 7800 s. In these one-dimensional time-domain and frequency-domain ACFs, the red lines show the best-fit results for ∆τd and ∆νd, respectively. of 1.03 M⊙ and a median companion mass of 1.27 M⊙, respectively, under the assumption that the pulsar mass is 1.35 M⊙. We incorpora… view at source ↗
Figure 9
Figure 9. Figure 9: Simulation of the expected uncertainty of the periastron advance rate ˙ω as a function of the total observational baseline for PSR J2338+4818. The simulation assumes a typical FAST observation cadence of 14 days and a TOA precision of 30 µs. Each blue point (Simulated data) in the figure corresponds to a fit including all TOAs accumulated up to that observational baseline. The dotted green, dash-dotted ora… view at source ↗
Figure 10
Figure 10. Figure 10: The estimated flux density of PSR J2338+4818 across all FAST observations (MJD 60190–61090), excluding the ultra-wideband observation. The flux densities are obtained from the observed S/N and integration time using the equation 30. Individual observation epochs are shown as data points and are connected by a solid line. Among all observation epochs, the maximum estimated flux density is 64.25 µJy (MJD 60… view at source ↗
Figure 11
Figure 11. Figure 11: The Pb–e relation for binary pulsars with different types of companions. Binary systems in globular clusters, whose evolution involves companion exchanges or close interactions with other stars, and those with surface magnetic fields B > 1011 G, which are thought to have evolved through a different formation channel (T. M. Tauris & T. Sennels 2000), both are excluded. Gray circles represent the non-mildly… view at source ↗
read the original abstract

Mildly recycled pulsars are neutron stars partially spun up through relatively short mass-transfer phases, typically with massive carbon-oxygen (CO) or oxygen-neon-magnesium (ONeMg) white dwarf companions. PSR J2338+4818, a mildly recycled pulsar, was discovered with the Five-hundred-meter Aperture Spherical Telescope (FAST). As a pilot study on the formation and evolutionary pathways of mildly recycled pulsars, we present the updated timing solution for PSR J2338+4818 and examine its single pulses and scintillation properties. Aided by the sensitivity of FAST, the single pulses of PSR J2338+4818 were systematically studied. 27,228 single pulses with S/N > 7 have been detected in our observations. For the FAST ultra-wideband observation on MJD 61045, the receiver was still in the technical commissioning phase, and then only a preliminary single-pulse search was performed. Pulse nulling was examined using a Markov Chain Monte Carlo (MCMC) method, but no evidence for nulling was found. The possible long-term nulling reported by previous studies did not occur in any of our observations in either the 1.0 to 1.5 GHz band or the 300 to 600 MHz band. Interstellar scintillation is evident in our observations. The measured scintillation timescales and bandwidths range from 2.93 to 25.26 minutes and 1.68 to 27.41 MHz, respectively. In all observations, no clear scintillation arc was found in the secondary spectra of PSR J2338+4818.

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 presents a pilot study of the mildly recycled pulsar PSR J2338+4818, including an updated timing solution, analysis of 27,228 single pulses (S/N > 7) detected across observations in the 1.0-1.5 GHz and 300-600 MHz bands, an MCMC-based search finding no evidence for pulse nulling, and measurements of interstellar scintillation with timescales of 2.93-25.26 minutes and bandwidths of 1.68-27.41 MHz, noting no clear scintillation arcs and that previously reported long-term nulling was absent from the data.

Significance. If the non-detection of nulling and the scintillation parameters hold after verification of data quality and coverage, the work provides direct measurements from a large sample of single pulses that can inform models of emission and propagation in mildly recycled pulsars. The scale of the single-pulse dataset (over 27,000 pulses) is a clear strength for statistical robustness in this pilot study.

major comments (2)
  1. [Abstract and Results section on nulling analysis] The central claim that 'the possible long-term nulling reported by previous studies did not occur in any of our observations' is load-bearing for the nulling conclusion, yet the manuscript provides no quantitative details on the number of epochs, individual session lengths, total integration time, or MJD span. Without this, it is impossible to assess whether the temporal sampling is adequate to rule out long-term off-states (hours to days) even while detecting pulses during on-states.
  2. [Single-pulse and nulling analysis] The MCMC analysis for short-term nulling is presented as showing no evidence, but the manuscript should specify the priors, convergence diagnostics, and how the S/N > 7 threshold and pulse selection were handled to ensure the nulling fraction upper limit is robust and not affected by post-hoc choices.
minor comments (2)
  1. [Observations] Clarify the impact of the commissioning-phase status of the ultra-wideband receiver on MJD 61045 for the preliminary single-pulse search, including any differences in calibration or sensitivity relative to the other observations.
  2. [Scintillation properties] The scintillation parameters are reported as ranges; provide per-epoch values with uncertainties and the method used to measure timescales and bandwidths for reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive feedback on our pilot study of PSR J2338+4818. The comments highlight areas where additional quantitative details and methodological transparency will strengthen the presentation of the nulling analysis. We address each point below and will revise the manuscript to incorporate the requested information.

read point-by-point responses

  1. Referee: [Abstract and Results section on nulling analysis] The central claim that 'the possible long-term nulling reported by previous studies did not occur in any of our observations' is load-bearing for the nulling conclusion, yet the manuscript provides no quantitative details on the number of epochs, individual session lengths, total integration time, or MJD span. Without this, it is impossible to assess whether the temporal sampling is adequate to rule out long-term off-states (hours to days) even while detecting pulses during on-states.

    Authors: We agree that a quantitative summary of the observational coverage is essential for evaluating the robustness of the long-term nulling non-detection. The current manuscript text is indeed limited in this regard. In the revised version, we will add a new subsection (or expanded table) in the Observations section that explicitly lists the number of epochs, individual session lengths, total integration time, and full MJD span across the 1.0-1.5 GHz and 300-600 MHz bands. This will include the specific FAST ultra-wideband observation on MJD 61045 and all other sessions, allowing direct assessment of whether the sampling adequately rules out long-term off-states. revision: yes

  2. Referee: [Single-pulse and nulling analysis] The MCMC analysis for short-term nulling is presented as showing no evidence, but the manuscript should specify the priors, convergence diagnostics, and how the S/N > 7 threshold and pulse selection were handled to ensure the nulling fraction upper limit is robust and not affected by post-hoc choices.

    Authors: We concur that the MCMC methodology requires fuller specification for reproducibility and to confirm the robustness of the nulling fraction upper limit. In the revised manuscript, we will expand the relevant paragraph in the Results or Methods section to detail the priors (e.g., uniform prior on the nulling fraction between 0 and 1), convergence diagnostics (such as Gelman-Rubin statistics and trace inspection), and confirm that the S/N > 7 threshold was applied uniformly to all 27,228 pulses prior to the MCMC fitting with no subsequent post-hoc adjustments to the selection. This will demonstrate that the analysis is not sensitive to arbitrary choices. revision: yes

Circularity Check

0 steps flagged

No circularity; results are direct observational measurements

full rationale

The paper presents empirical results from FAST telescope observations of PSR J2338+4818, including detection of 27,228 single pulses (S/N > 7), MCMC analysis finding no evidence for pulse nulling, and measured scintillation timescales (2.93 to 25.26 minutes) and bandwidths (1.68 to 27.41 MHz). No derivations, models, or predictions are present that reduce to fitted inputs by construction, self-definition, or self-citation chains. All values are direct data products from the observations, with the non-detection of nulling and scintillation properties reported as measurements rather than outputs of any closed-loop fitting or ansatz. The analysis is self-contained as straightforward reporting of telescope data without load-bearing reductions to prior fitted quantities or author-specific uniqueness theorems.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Purely observational study with no theoretical model, derivation, or new physical entities; results rest on telescope data and standard analysis techniques.

pith-pipeline@v0.9.0 · 5910 in / 1082 out tokens · 42747 ms · 2026-05-20T17:10:08.733797+00:00 · methodology

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Works this paper leans on

45 extracted references · 45 canonical work pages · 3 internal anchors

  1. [1]

    Fichtenbauer, T. D. J. 2023, ApJ, 948, 32, doi: 10.3847/1538-4357/acbb68

    work page doi:10.3847/1538-4357/acbb68 2023

  2. [2]

    J., Freire, P

    Berezina, M., Champion, D. J., Freire, P. C. C., et al. 2017, MNRAS, 470, 4421, doi: 10.1093/mnras/stx1518

    work page doi:10.1093/mnras/stx1518 2017

  3. [3]

    Bhat, N. D. R., Rao, A. P., & Gupta, Y. 1999, ApJS, 121, 483, doi: 10.1086/313198

    work page doi:10.1086/313198 1999

  4. [4]

    Bhattacharya, D., & van den Heuvel, E. P. J. 1991, PhR, 203, 1, doi: 10.1016/0370-1573(91)90064-S

    work page doi:10.1016/0370-1573(91)90064-s 1991

  5. [5]

    Cruces, M., Reisenegger, A., & Tauris, T. M. 2019, MNRAS, 490, 2013, doi: 10.1093/mnras/stz2701

    work page doi:10.1093/mnras/stz2701 2019

  6. [6]

    J., Li, D., et al

    Cruces, M., Champion, D. J., Li, D., et al. 2021, MNRAS, 508, 300, doi: 10.1093/mnras/stab2540

    work page doi:10.1093/mnras/stab2540 2021

  7. [7]

    Dewi, J. D. M., Podsiadlowski, P., & Pols, O. R. 2005, MNRAS, 363, L71, doi: 10.1111/j.1745-3933.2005.00085.x

    work page doi:10.1111/j.1745-3933.2005.00085.x 2005

  8. [8]

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

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306, doi: 10.1086/670067

    work page doi:10.1086/670067 2013

  9. [9]

    Freire, P. C. C., & Ridolfi, A. 2018, MNRAS, 476, 4794, doi: 10.1093/mnras/sty524

    work page doi:10.1093/mnras/sty524 2018

  10. [10]

    1990, in Astronomical Society of the Pacific Conference Series, Vol

    Iben, Jr., I. 1990, in Astronomical Society of the Pacific Conference Series, Vol. 11, Confrontation Between Stellar Pulsation and Evolution, ed. C. Cacciari & G. Clementini, 483–493

    work page 1990

  11. [11]

    Iben, Jr., I., & Tutukov, A. V. 1984, ApJS, 54, 335, doi: 10.1086/190932

    work page doi:10.1086/190932 1984

  12. [12]

    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

  13. [13]

    2018, ApJ, 855, 14, doi: 10.3847/1538-4357/aaab62

    Vallisneri, M. 2018, ApJ, 855, 14, doi: 10.3847/1538-4357/aaab62

    work page doi:10.3847/1538-4357/aaab62 2018

  14. [14]

    W., & Lee, K

    Karuppusamy, R., Stappers, B. W., & Lee, K. J. 2012, A&A, 538, A7, doi: 10.1051/0004-6361/201117667

    work page doi:10.1051/0004-6361/201117667 2012

  15. [15]

    2019, Journal of Astrophysics and Astronomy, 40, 42, doi: 10.1007/s12036-019-9608-z

    Konar, S., & Deka, U. 2019, Journal of Astrophysics and Astronomy, 40, 42, doi: 10.1007/s12036-019-9608-z

    work page doi:10.1007/s12036-019-9608-z 2019

  16. [16]

    2016, MNRAS, 458, 868, doi: 10.1093/mnras/stw189

    Lazarus, P., Karuppusamy, R., Graikou, E., et al. 2016, MNRAS, 458, 868, doi: 10.1093/mnras/stw189

    work page doi:10.1093/mnras/stw189 2016

  17. [17]

    2002, ApJ, 564, 930, doi: 10.1086/324331

    Li, X.-D. 2002, ApJ, 564, 930, doi: 10.1086/324331

    work page doi:10.1086/324331 2002

  18. [18]

    R., & Kramer, M

    Lorimer, D. R., & Kramer, M. 2004, Handbook of Pulsar Astronomy

    work page 2004

  19. [19]

    2021, ApJ, 911, 45, doi: 10.3847/1538-4357/abe62f

    Luo, J., Ransom, S., Demorest, P., et al. 2021, ApJ, 911, 45, doi: 10.3847/1538-4357/abe62f

    work page doi:10.3847/1538-4357/abe62f 2021

  20. [20]

    2024, A&A, 683, A183, doi: 10.1051/0004-6361/202348247

    Men, Y., & Barr, E. 2024, A&A, 683, A183, doi: 10.1051/0004-6361/202348247

    work page doi:10.1051/0004-6361/202348247 2024

  21. [21]

    2011, International Journal of Modern Physics D, 20, 989, doi: 10.1142/S0218271811019335 ¨Ozel, F., & Freire, P

    Nan, R., Li, D., Jin, C., et al. 2011, International Journal of Modern Physics D, 20, 989, doi: 10.1142/S0218271811019335 ¨Ozel, F., & Freire, P. 2016, ARA&A, 54, 401, doi: 10.1146/annurev-astro-081915-023322

    work page doi:10.1142/s0218271811019335 2011

  22. [22]

    T., Perera, B

    Palliyaguru, N. T., Perera, B. B. P., McLaughlin, M. A., Os lowski, S., & Siebert, G. L. 2023, MNRAS, 520, 2747, doi: 10.1093/mnras/stad194

    work page doi:10.1093/mnras/stad194 2023

  23. [23]

    2020, The Innovation, 1, 100053, doi: 10.1016/j.xinn.2020.100053

    Qian, L., Yao, R., Sun, J., et al. 2020, The Innovation, 1, 100053, doi: 10.1016/j.xinn.2020.100053

    work page doi:10.1016/j.xinn.2020.100053 2020

  24. [24]

    Reardon, D. J. 2020, Scintools: Pulsar scintillation data tools,, Astrophysics Source Code Library, record ascl:2011.019 http://ascl.net/2011.019

    work page 2020

  25. [25]

    J., Coles, W

    Reardon, D. J., Coles, W. A., Hobbs, G., et al. 2019, MNRAS, 485, 4389, doi: 10.1093/mnras/stz643

    work page doi:10.1093/mnras/stz643 2019

  26. [26]

    J., Coles, W

    Reardon, D. J., Coles, W. A., Bailes, M., et al. 2020, ApJ, 904, 104, doi: 10.3847/1538-4357/abbd40 21

    work page doi:10.3847/1538-4357/abbd40 2020

  27. [27]

    J., Main, R., Ocker, S

    Reardon, D. J., Main, R., Ocker, S. K., et al. 2025, Nature Astronomy, 9, 1053, doi: 10.1038/s41550-025-02534-6

    work page doi:10.1038/s41550-025-02534-6 2025

  28. [28]

    Rickett, B. J. 1990, ARA&A, 28, 561, doi: 10.1146/annurev.aa.28.090190.003021

    work page doi:10.1146/annurev.aa.28.090190.003021 1990

  29. [29]

    J., & Lyne, A

    Rickett, B. J., & Lyne, A. G. 1990, MNRAS, 244, 68

    work page 1990

  30. [30]

    Ritchings, R. T. 1976, MNRAS, 176, 249, doi: 10.1093/mnras/176.2.249

    work page doi:10.1093/mnras/176.2.249 1976

  31. [31]

    2022, MNRAS, 512, 5782, doi: 10.1093/mnras/stac821

    Sengar, R., Balakrishnan, V., Stevenson, S., et al. 2022, MNRAS, 512, 5782, doi: 10.1093/mnras/stac821

    work page doi:10.1093/mnras/stac821 2022

  32. [32]

    Stovall, K., Freire, P. C. C., Chatterjee, S., et al. 2018, ApJL, 854, L22, doi: 10.3847/2041-8213/aaad06

    work page doi:10.3847/2041-8213/aaad06 2018

  33. [33]

    L., Archibald, A

    Susobhanan, A., Kaplan, D. L., Archibald, A. M., et al. 2024, ApJ, 971, 150, doi: 10.3847/1538-4357/ad59f7

    work page doi:10.3847/1538-4357/ad59f7 2024

  34. [34]

    K., Rosen, R., McLaughlin, M

    Swiggum, J. K., Rosen, R., McLaughlin, M. A., et al. 2015, ApJ, 805, 156, doi: 10.1088/0004-637X/805/2/156

    work page doi:10.1088/0004-637x/805/2/156 2015

  35. [35]

    , author Padovani, P

    Tauris, T. M., Langer, N., & Kramer, M. 2011, MNRAS, 416, 2130, doi: 10.1111/j.1365-2966.2011.19189.x

    work page doi:10.1111/j.1365-2966.2011.19189.x 2011

  36. [36]

    , author Tavecchio, F

    Tauris, T. M., Langer, N., & Kramer, M. 2012, MNRAS, 425, 1601, doi: 10.1111/j.1365-2966.2012.21446.x

    work page doi:10.1111/j.1365-2966.2012.21446.x 2012

  37. [37]

    Formation of the binary pulsars PSR B2303+46 and PSR J1141-6545 - young neutron stars with old white dwarf companions

    Tauris, T. M., & Sennels, T. 2000, A&A, 355, 236, doi: 10.48550/arXiv.astro-ph/9909149

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9909149 2000

  38. [38]

    M., & van den Heuvel, E

    Tauris, T. M., & van den Heuvel, E. P. J. 2006, in Compact stellar X-ray sources, ed. W. H. G. Lewin & M. van der

    work page 2006

  39. [39]

    Formation and Evolution of Compact Stellar X-ray Sources

    Klis, Vol. 39, 623–665, doi: 10.48550/arXiv.astro-ph/0303456

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0303456

  40. [40]

    M., & van den Heuvel, E

    Tauris, T. M., & van den Heuvel, E. P. J. 2023, Physics of Binary Star Evolution. From Stars to X-ray Binaries and Gravitational Wave Sources, doi: 10.48550/arXiv.2305.09388

    work page doi:10.48550/arxiv.2305.09388 2023

  41. [41]

    M., van den Heuvel, E

    Tauris, T. M., van den Heuvel, E. P. J., & Savonije, G. J. 2000, ApJL, 530, L93, doi: 10.1086/312496

    work page doi:10.1086/312496 2000

  42. [42]

    M., Kramer, M., Freire, P

    Tauris, T. M., Kramer, M., Freire, P. C. C., et al. 2017, ApJ, 846, 170, doi: 10.3847/1538-4357/aa7e89

    work page doi:10.3847/1538-4357/aa7e89 2017

  43. [43]

    Taylor, J., Ransom, S., & Padmanabh, P. V. 2024, ApJ, 964, 128, doi: 10.3847/1538-4357/ad1ce9 van Straten, W., & Bailes, M. 2011, PASA, 28, 1, doi: 10.1071/AS10021 van Straten, W., Demorest, P., & Oslowski, S. 2012, Astronomical Research and Technology, 9, 237, doi: 10.48550/arXiv.1205.6276

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad1ce9 2024

  44. [44]

    2008, in American Institute of Physics Conference Series, Vol

    Willems, B., Andrews, J., Kalogera, V., & Belczynski, K. 2008, in American Institute of Physics Conference Series, Vol. 983, 40 Years of Pulsars: Millisecond Pulsars, Magnetars and More, ed. C. Bassa, Z. Wang, A. Cumming, & V. M. Kaspi (AIP), 464–468, doi: 10.1063/1.2900275

    work page doi:10.1063/1.2900275 2008

  45. [45]

    2023, Research in Astronomy and Astrophysics, 23, 075016, doi: 10.1088/1674-4527/acd58e

    Zhang, C.-P., Jiang, P., Zhu, M., et al. 2023, Research in Astronomy and Astrophysics, 23, 075016, doi: 10.1088/1674-4527/acd58e

    work page doi:10.1088/1674-4527/acd58e 2023