Pith. sign in

REVIEW 3 major objections 5 minor 298 references

The apparent gap in double-neutron-star eccentricities can arise from a sharp jump in neutron-star remnant masses at about 3 solar masses, provided the second-born neutron star receives only a tiny natal kick.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · deepseek-v4-flash

2026-08-04 00:36 UTC pith:5ZJ5IAQ6

load-bearing objection A plausible, clearly-scoped mechanism for the DNS eccentricity gap, but the load-bearing zero-kick assumption and weak statistical significance mean it's a promising hypothesis, not a confirmed solution. the 3 major comments →

arxiv 2608.00174 v1 pith:5ZJ5IAQ6 submitted 2026-07-31 astro-ph.SR astro-ph.GAastro-ph.HE

On Bimodality in the Eccentricity Distribution of Galactic Double Neutron Stars

Aldana Grichener , Paul Disberg , Ryosuke Hirai , Ilya Mandel This is my paper
classification astro-ph.SR astro-ph.GAastro-ph.HE
keywords double neutron starseccentricity distributionBlaauw kicknatal kicksremnant mass functionultra-stripped supernovaepopulation synthesispulsar timing
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Galactic double neutron stars show an apparent bimodal eccentricity distribution with few systems at intermediate eccentricities, a pattern that standard population models have struggled to reproduce. This paper argues the gap is a natural consequence of a non-monotonic relation between progenitor mass and neutron star mass: a sharp upward jump in remnant mass at a CO core mass near 3 solar masses makes the mass lost in the second supernova jump across a narrow progenitor-mass range. When the second-born neutron star receives no significant natal kick, that mass-loss jump translates directly into a forbidden band of post-supernova eccentricities. A population-synthesis model built on this prescription reproduces the observed orbital period–eccentricity distribution, including the gap, while models with continuous remnant masses or kicks of a few tens of km/s fill it in. The authors are careful to note that the current sample is too small to establish the gap with high statistical confidence.

Core claim

A non-monotonic relationship between the progenitor core mass and the mass of the neutron star remnant, combined with negligible natal kicks for the second-born neutron star, naturally produces a bimodal distribution of Blaauw kicks and therefore a bimodality in double-neutron-star eccentricities consistent with the observed Galactic sample. In the adopted supernova prescription, a carbon-oxygen core just below 3 solar masses loses about 1.2 solar masses during the second supernova, leaving the binary with an eccentricity below about 0.4, while a core just above 3 solar masses loses more than 1.5 solar masses and yields an eccentricity above about 0.55. In the absence of a natal kick, these

What carries the argument

The Blaauw kick — the eccentricity imparted when a binary suddenly loses mass in a supernova — is the carrier of the effect. With no natal kick, the post-explosion eccentricity is set entirely by the retained mass fraction β through e = (1−β)/β. A sharp upward jump in the remnant neutron-star mass near a CO core mass of about 3 solar masses makes the ejected mass (and hence 1−β) jump from about 1.2 to more than 1.5 solar masses across the threshold, translating directly into a forbidden eccentricity range. The zero-kick assumption for ultra-stripped supernovae lets the mass-loss discontinuity show through instead of being smeared out by random kick velocities.

Load-bearing premise

The second-born neutron star in close double neutron stars receives a natal kick small enough (zero in the illustrative model) that the post-supernova eccentricity is set by symmetric mass loss rather than by random kick velocity, and the remnant mass function really has a sharp break near 3 solar masses.

What would settle it

A future pulsar survey that discovers several dozen new Galactic double neutron stars with back-integrated birth eccentricities inside the 0.4–0.58 interval, at the rate expected from a smooth eccentricity distribution, would refute the proposed gap mechanism. More directly, finding a single double neutron star on the low-eccentricity branch whose second-born neutron star has a firmly measured mass above the ~3-solar-mass break and a measured natal kick component above ~50 km/s would contradict the model's central prediction.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Future pulsar surveys that find dozens of new Galactic double neutron stars could either strengthen the evidence for a real eccentricity gap or fill it in, directly testing the model's distinguishing prediction.
  • The model predicts a population of massive double neutron stars at short orbital periods with rapid gravitational-wave merger times, which would be more readily seen by gravitational-wave detectors than by radio pulsar searches.
  • The mechanism implies that most second-born neutron stars in close double neutron stars receive very small natal kicks, with systems like PSR B1534+12 requiring a direction-dependent kick that partially cancels the mass-loss eccentricity.
  • If confirmed, the gap would serve as a probe of the supernova remnant-mass function, fixing the location and sharpness of the break near 3 solar masses.
  • A bimodal second-supernova kick distribution correlated with progenitor mass loss, rather than a single zero-kick assumption, could preserve the gap while accommodating spin-orbit misalignments like those of PSR B1534+12.

Where Pith is reading between the lines

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

  • The same mechanism may explain eccentricity gaps seen in other binary populations, such as Be X-ray binaries and some pulsar–white-dwarf systems, if those binaries also experience a mass-loss discontinuity with low kicks.
  • A sharper test than simply counting systems in the gap would be to measure individual neutron-star masses in new double neutron stars: the model predicts a correlation between the second-born neutron star's mass and the binary eccentricity branch on which it sits.
  • The non-monotonic remnant mass relation invoked here could also produce distinct branches in the black-hole mass distribution of binary black-hole mergers, offering a gravitational-wave observable that could be checked in parallel.
  • If the gap persists with a larger sample, the location of its edges quantitatively constrains the physics of the carbon-burning convective/radiative transition and the composition-shell mass cuts that set the neutron-star mass.

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

3 major / 5 minor

Summary. The paper proposes that the apparent bimodality in the observed Galactic double neutron star (DNS) eccentricity distribution — with a deficit of systems at intermediate eccentricities 0.4 ≲ e ≲ 0.58 — can be explained by a non-monotonic relationship between progenitor mass and neutron star mass, combined with very small or negligible natal kicks in the second supernova (USSN). Using the population synthesis code COMPAS with the Mandel & Müller (2020) remnant-mass prescription and zero USSN kicks (the 'M&M,0' model), the authors show that a mass break near CO core mass M2 = 3 M_sun produces a bimodal Blaauw-kick distribution and hence an eccentricity gap qualitatively similar to the observed one. They compare simulated orbital period–eccentricity and total-mass distributions against a curated sample of 29 Galactic DNSs, and present sensitivity studies in Appendices A and B: alternative remnant-mass prescriptions and non-zero USSN kicks do not reproduce the gap, and a smooth eccentricity distribution is statistically consistent with current data. The paper explicitly acknowledges the small sample size, the statistical non-significance of the gap, and the tension posed by PSR B1534+12, which requires a large second-SN kick component.

Significance. If the proposed mechanism is correct, it would provide a natural, physically motivated explanation for a puzzling feature in the Galactic DNS population, connecting stellar-structure physics (a jump in remnant mass at a CO core mass of ∼3 M_sun) to binary observables. The paper is valuable in laying out this scenario clearly, and it makes a falsifiable prediction: future DNS discoveries will either fill or confirm the eccentricity gap. The population synthesis setup is reproducible (COMPAS version and Zenodo data are provided), and the sensitivity studies in Appendices A and B are a genuine strength: they test alternative remnant-mass prescriptions and kick magnitudes, and they honestly quantify the statistical significance of the gap. The central claim, however, is conditional on an unquantified 'sufficiently small' second-SN kick, and the paper's own analysis shows that at least one observed system violates this condition; this limits the strength of the claim as a quantitative explanation of the observed sample.

major comments (3)
  1. [Section 2 / Table 1 and Figure 2] The central condition that the second-born NS receives a 'sufficiently small' natal kick is never quantified. The fiducial model sets v_kick,USSN = 0, and Fig. A2 shows that non-zero kicks of 5–50 km/s progressively fill the gap. Yet Section 4 reports that PSR B1534+12 requires a perpendicular kick component of 150–220 km/s, which the authors describe as 'clear tension' with the zero-kick assumption. The reader is left with no estimate of the maximum kick magnitude that preserves the gap, nor the expected fraction of DNSs with kicks below that threshold. Since the B1534+12-like system alone appears to require a kick an order of magnitude larger than the values that already erase the gap in Fig. A2, the mechanism is not demonstrated to survive in a realistic population. The authors should quantify the critical kick scale and, ideally, compute the predicted gap visibility under a mixture o
  2. [Appendix B] The model predicts a gap at birth eccentricities, and the comparison in Fig. 2 uses back-integrated observed eccentricities. Table 1 lists J1208–5936 with a back-integrated eccentricity e_b = 0.471, which lies inside the claimed gap [0.4, 0.58]. The paper acknowledges this system in passing ('one system ... having an eccentricity of ∼0.5 after integrating its orbit back in time'), but it is not accounted for in the model comparison. Since the central mechanism strictly excludes systems from the gap at birth, this confident DNS is a direct counterexample at birth eccentricities. The authors should explicitly discuss whether J1208–5936 can be accommodated by the M&M,0 model (e.g., via measurement uncertainty, age uncertainty, or an unusual evolutionary channel), and whether its existence at the expected small frequency is consistent with the model.
  3. [Appendix B] The statistical analysis shows that the observed eccentricity gap is not statistically significant: the KS test gives p ≈ 0.12, and the probability of observing zero systems in [0.4, 0.58] under a smooth distribution is p_0,gap ≈ 0.06 for the 21 confident non-GC DNSs. As the paper itself notes, the data do not strongly reject a smooth, gap-free distribution. This does not invalidate the proposed mechanism as a theoretical possibility, but it does mean that the central observational phenomenon that the model is invoked to explain may itself be a statistical fluctuation. The framing in the Summary — that the model 'can naturally produce' a bimodality 'broadly consistent with the observed Galactic DNS sample' — should be correspondingly tempered, and the authors should more explicitly distinguish between a demonstrated mechanism and a statistically established bimodality.
minor comments (5)
  1. [Section 3.3] The abstract states an 'absence of systems at measured intermediate eccentricities', but Table 1 and the text note that one system (J1208–5936) has a back-integrated eccentricity of 0.471. Please clarify whether the gap is defined in measured or back-integrated eccentricity, and make the wording consistent throughout.
  2. [Appendix B] In the discussion of low-eccentricity systems, the text says these are 'associated with small CO core progenitors' (green dots in Fig. 1). It may help to explicitly state which CO core mass range corresponds to each color, since the color coding is central to the interpretation and is not repeated in the text.
  3. [Section 4] Equation (B1) defines the smooth CDF as P(E ≤ e) = 1 − ln(e)/ln(e_min). It would be useful to state explicitly that this distribution is supported on [e_min, 1) and that e_min = 0.05 is chosen as a lower bound; the motivation for this particular functional form is also worth one sentence.
  4. [General] The phrase 'Using a similar simple spin-orbit tilt argument ... however' is grammatically awkward. Please rephrase for clarity.
  5. [General] The manuscript uses 'case BB mass transfer' inconsistently; it should be 'Case BB' when referring to the evolutionary stage. Also, the typographical artifact 'Manch- ester' in the ATNF catalog reference should be corrected to 'Manchester'.

Circularity Check

0 steps flagged

No significant circularity: the eccentricity gap is a derived consequence of explicit, externally sourced model inputs, not an input recycled as a prediction.

full rationale

The paper's central mechanism is a chain: assume a break in the NS remnant-mass function (from Mandel & Muller 2020, with independent non-monotonicity support from Schneider et al. 2021/2023 and Boccioli & Fragione 2024) and negligible USSN natal kicks (explicitly labeled 'for illustrative purposes'); then the Blaauw-kick mapping translates the mass break into an eccentricity gap. The gap location is a derived consequence, not a fitted parameter, and the Mandel & Muller prescription is a general supernova remnant-mass model not tuned to DNS eccentricities. The paper itself flags the main weaknesses: the observed gap is not statistically compelling (Appendix B gives KS p ≈ 0.12 and p0,gap ≈ 0.06), B1534+12 is in 'clear tension' with the zero-kick assumption, and Fig. A2 shows the gap fills for nonzero USSN kicks. These are honest caveats rather than hidden circularity. There is self-citation of Mandel & Muller (2020), but it is not load-bearing in a circular sense because the prescription is independent of the target eccentricity data and is corroborated by external studies. No step reduces by construction to its own input.

Axiom & Free-Parameter Ledger

4 free parameters · 6 axioms · 0 invented entities

The central model rests on two externally-motivated ingredients: a broken remnant mass function (from Mandel & Müller 2020) and negligible USSN kicks. Neither is derived in this paper, and the kick assumption is in tension with at least one observed system. No parameters are fitted to the DNS eccentricity data, but the choice of zero-kick model is guided by the target feature.

free parameters (4)
  • USSN natal kick velocity (v_kick,USSN) = 0 km/s in fiducial model (M&M,0); varied 5–50 km/s in Appendix A2
    Chosen to isolate the Blaauw-kick mechanism and reproduce the observed eccentricity gap; not derived from first principles. The paper states 'we run a model where USSN kick velocities are set to zero' (§3.2).
  • Remnant mass break location M2 (CO core mass) = 3 M_sun
    Adopted from Mandel & Müller (2020); sets the threshold where the NS mass jumps and thus determines the location of the eccentricity gap. Not fitted to DNS data in this paper, but load-bearing.
  • NS kick scaling parameter = 630 km/s
    Standard COMPAS parameter from Kapil et al. (2023)/Mandel & Müller (2020); affects kicks for the first SN and non-USSN second SNe.
  • NS kick distribution width sigma_kick,NS = 0.45
    Adopted from Kapil et al. (2023) as amended by Disberg et al. (2026).
axioms (6)
  • domain assumption The Mandel & Müller (2020) broken remnant mass prescription (with break at CO core mass 3 M_sun) is a reasonable approximation to the true progenitor-mass–NS-mass relation.
    Section 3.1 motivates the break physically, but the existence and location of the break are not established; the paper adopts this prescription 'as an illustrative case' (§3.1).
  • domain assumption The second NS in DNSs is typically formed via ultra-stripped supernovae with very small natal kicks.
    Justified by J0737-3039 spin-orbit alignment and the low transverse velocity, but B1534+12 suggests a large kick; the assumption is central to the mechanism (§4, §5).
  • domain assumption The characteristic pulsar age is approximately equal to the DNS age for back-integration.
    Section 2 notes this is 'generally consistent with kinematic ages' but also cites caveats about characteristic ages.
  • domain assumption All simulation stars can be modeled at solar metallicity without affecting DNS properties.
    The paper states that a lognormal metallicity distribution has negligible impact on the trends (Section 3.2).
  • standard math The orbital eccentricity after the second SN follows e=(1-β)/β in the no-natal-kick limit.
    Standard two-body mass-loss result used in Fig. 1 and Section 4.
  • domain assumption Stripped helium stars in COMPAS undergo complete envelope removal (case BB mass transfer).
    Section 5 notes this is an assumption and that partial stripping could also create a bifurcation.

pith-pipeline@v1.3.0-alltime-deepseek · 18181 in / 15284 out tokens · 149176 ms · 2026-08-04T00:36:01.160828+00:00 · methodology

0 comments
read the original abstract

The detection of Galactic double neutron stars (DNSs) through pulsar timing offers a unique opportunity to probe massive stellar and binary evolution. The observed DNS population exhibits an apparently bimodal eccentricity distribution, with an absence of systems at measured intermediate eccentricities, $0.4 \lesssim e_{\rm m} \lesssim 0.58$, whose origin remains unclear. We propose that this possible gap can arise naturally if the relationship between the progenitor masses and neutron star (NS) masses is non-monotonic, provided that the second-born NS receives a sufficiently small natal kick. We illustrate this scenario using the population synthesis code COMPAS, and find that our DNS population model can reproduce the observed orbital period-eccentricity distribution relatively well, including the apparent bimodality. Although a larger observed sample is required to draw more robust conclusions, our results suggest that this model provides a natural pathway for explaining current observations of Galactic DNSs through isolated binary evolution.

Figures

Figures reproduced from arXiv: 2608.00174 by Aldana Grichener, Ilya Mandel, Paul Disberg, Ryosuke Hirai.

Figure 1
Figure 1. Figure 1: Properties of DNSs evolved with the I. Mandel & B. M¨uller (2020) prescription for the remnant mass and kick distribution, assuming the USSN kicks equal zero; M&M,0. The different colors correspond to different CO core mass regimes in the I. Mandel & B. M¨uller (2020) formalism, where M1 = 2M⊙, M2 = 3M⊙, and M3 = 7M⊙. Left panel: mass of the NS formed in the second SN explosion vs the CO core mass, which i… view at source ↗
Figure 2
Figure 2. Figure 2: Observables of Galactic DNSs. Dots show the results of the M&M,0 model, with colors defined as in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Same as the right panel of [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

298 extracted references · 17 canonical work pages

  1. [1]

    P., Abbott , R., Abbott , T

    Abbott , B. P., Abbott , R., Abbott , T. D., et al. 2020, title GW190425: Observation of a Compact Binary Coalescence with Total Mass 3.4 M _ , , 892, L3, 10.3847/2041-8213/ab75f5

    doi:10.3847/2041-8213/ab75f5 2020

  2. [2]

    J., Farr , W

    Andrews , J. J., Farr , W. M., Kalogera , V., & Willems , B. 2015, title Evolutionary Channels for the Formation of Double Neutron Stars , , 801, 32, 10.1088/0004-637X/801/1/32

    work page doi:10.1088/0004-637x/801/1/32 2015

  3. [3]

    J., & Mandel , I

    Andrews , J. J., & Mandel , I. 2019, title Double Neutron Star Populations and Formation Channels , , 880, L8, 10.3847/2041-8213/ab2ed1

    doi:10.3847/2041-8213/ab2ed1 2019

  4. [4]

    Arnett , W. D. 1972, title Advanced Evolution of Massive Stars. II. Carbon Burning , , 176, 699, 10.1086/151672

    work page doi:10.1086/151672 1972

  5. [5]

    J., & Scott , P

    Asplund , M., Grevesse , N., Sauval , A. J., & Scott , P. 2009, title The Chemical Composition of the Sun , , 47, 481, 10.1146/annurev.astro.46.060407.145222

    arXiv 2009

  6. [6]

    D., Dutta , A., Freire , P

    Barr , E. D., Dutta , A., Freire , P. C. C., et al. 2024, title A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes , Science, 383, 275, 10.1126/science.adg3005

    doi:10.1126/science.adg3005 2024

  7. [7]

    2016, title Formation of double neutron star systems as implied by observations , , 456, 4089, 10.1093/mnras/stv2903

    Beniamini , P., & Piran , T. 2016, title Formation of double neutron star systems as implied by observations , , 456, 4089, 10.1093/mnras/stv2903

    doi:10.1093/mnras/stv2903 2016

  8. [8]

    1961, title On the origin of the O- and B-type stars with high velocities (the ''run-away'' stars), and some related problems , Bull

    Blaauw , A. 1961, title On the origin of the O- and B-type stars with high velocities (the ''run-away'' stars), and some related problems , Bull. Astron. Inst. Netherlands, 15, 265

    1961

  9. [9]

    Boccioli , L., & Fragione , G. 2024, title Remnant masses from 1D+ core-collapse supernovae simulations: Bimodal neutron star mass distribution and black holes in the low-mass gap , , 110, 023007, 10.1103/PhysRevD.110.023007

    doi:10.1103/physrevd.110.023007 2024

  10. [10]

    P., & Kasen , D

    Boccioli , L., Vartanyan , D., O'Connor , E. P., & Kasen , D. 2025, title Neutrino heating in 1D, 2D, and 3D core-collapse supernovae: characterizing the explosion of high-compactness stars , , 540, 3885, 10.1093/mnras/staf963

    doi:10.1093/mnras/staf963 2025

  11. [11]

    2019, title Anticipated Performance of the Square Kilometre Array -- Phase 1 (SKA1) , arXiv e-prints, arXiv:1912.12699, 10.48550/arXiv.1912.12699

    Braun , R., Bonaldi , A., Bourke , T., Keane , E., & Wagg , J. 2019, title Anticipated Performance of the Square Kilometre Array -- Phase 1 (SKA1) , arXiv e-prints, arXiv:1912.12699, 10.48550/arXiv.1912.12699

    Pith/arXiv arXiv doi:10.48550/arxiv.1912.12699 2019

  12. [12]

    E., Heger , A., Langer , N., et al

    Brown , G. E., Heger , A., Langer , N., et al. 2001, title Formation of high mass X-ray black hole binaries , , 6, 457, 10.1016/S1384-1076(01)00077-X

    doi:10.1016/s1384-1076(01)00077-x 2001

  13. [13]

    2003, title An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system, Nature, 426, 531

    Burgay, M., et al. 2003, title An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system, Nature, 426, 531

    2003

  14. [14]

    2024, title Physical Correlations and Predictions Emerging from Modern Core-Collapse Supernova Theory , arXiv e-prints, arXiv:2401.06840, 10.48550/arXiv.2401.06840

    Burrows , A., Wang , T., & Vartanyan , D. 2024, title Physical Correlations and Predictions Emerging from Modern Core-Collapse Supernova Theory , arXiv e-prints, arXiv:2401.06840, 10.48550/arXiv.2401.06840

    Pith/arXiv arXiv doi:10.48550/arxiv.2401.06840 2024

  15. [15]

    J., Bavera , S

    Chattaraj , A., Andrews , J. J., Bavera , S. S., et al. 2025, title Forming Double Neutron Stars using Detailed Binary Evolution Models with POSYDON: Comparison to the Galactic Systems , arXiv e-prints, arXiv:2508.00186, 10.48550/arXiv.2508.00186

    Pith/arXiv arXiv doi:10.48550/arxiv.2508.00186 2025

  16. [16]

    2023, title The MPIfR-MeerKAT Galactic Plane Survey

    Colom i Bernadich , M., Balakrishnan , V., Barr , E., et al. 2023, title The MPIfR-MeerKAT Galactic Plane Survey. II. The eccentric double neutron star system PSR J1208 - 5936 and a neutron star merger rate update , , 678, A187, 10.1051/0004-6361/202346953

    doi:10.1051/0004-6361/202346953 2023

  17. [17]

    M., Ofek , E

    De , K., Kasliwal , M. M., Ofek , E. O., et al. 2018, title A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary , Science, 362, 201, 10.1126/science.aas8693

    doi:10.1126/science.aas8693 2018

  18. [18]

    F., da Silva , L., Porto de Mello , G

    del Peloso , E. F., da Silva , L., Porto de Mello , G. F., & Arany-Prado , L. I. 2005, title The age of the Galactic thin disk from Th/Eu nucleocosmochronology. III. Extended sample , , 440, 1153, 10.1051/0004-6361:20053307

    doi:10.1051/0004-6361:20053307 2005

  19. [19]

    T., Bailes , M., & Tingay , S

    Deller , A. T., Bailes , M., & Tingay , S. J. 2009, title Implications of a VLBI Distance to the Double Pulsar J0737-3039A/B , Science, 323, 1327, 10.1126/science.1167969

    doi:10.1126/science.1167969 2009

  20. [20]

    T., Swiggum , J

    Ding , H., Deller , A. T., Swiggum , J. K., et al. 2024, title VLBA Astrometry of the Galactic Double Neutron Stars PSR J0509+3801 and PSR J1930 1852: A Preliminary Transverse Velocity Distribution of Double Neutron Stars and its Implications , , 970, 90, 10.3847/1538-4357/ad4883

    doi:10.3847/1538-4357/ad4883 2024

  21. [21]

    2026, title Reconciling the Systemic Kicks of Observed Millisecond Pulsars, Spider Pulsars, and Low-mass X-Ray Binaries, , 1000, L56, 10.3847/2041-8213/ae52f1

    Disberg, P., Bahramian, A., & Mandel, I. 2026, title Reconciling the Systemic Kicks of Observed Millisecond Pulsars, Spider Pulsars, and Low-mass X-Ray Binaries, , 1000, L56, 10.3847/2041-8213/ae52f1

    work page doi:10.3847/2041-8213/ae52f1 2026

  22. [22]

    Disberg , P., Gaspari , N., & Levan , A. J. 2024 a , title Kinematic constraints on the ages and kick velocities of Galactic neutron star binaries , , 689, A348, 10.1051/0004-6361/202450790

    doi:10.1051/0004-6361/202450790 2024

  23. [23]

    Disberg , P., Gaspari , N., & Levan , A. J. 2024 b , title Deceleration of kicked objects due to the Galactic potential , , 687, A272, 10.1051/0004-6361/202449996

    doi:10.1051/0004-6361/202449996 2024

  24. [24]

    Disberg , P., Gaspari , N., & Levan , A. J. 2025, title A kinematically constrained kick distribution for isolated neutron stars , , 700, A75, 10.1051/0004-6361/202554349

    doi:10.1051/0004-6361/202554349 2025

  25. [25]

    2025, title The Kick Velocity Distribution of Isolated Neutron Stars , , 989, L8, 10.3847/2041-8213/adf286

    Disberg , P., & Mandel , I. 2025, title The Kick Velocity Distribution of Isolated Neutron Stars , , 989, L8, 10.3847/2041-8213/adf286

    doi:10.3847/2041-8213/adf286 2025

  26. [26]

    2023, title Failed supernovae as a natural explanation for the binary black hole mass distribution , , 676, A31, 10.1051/0004-6361/202245693

    Disberg , P., & Nelemans , G. 2023, title Failed supernovae as a natural explanation for the binary black hole mass distribution , , 676, A31, 10.1051/0004-6361/202245693

    doi:10.1051/0004-6361/202245693 2023

  27. [27]

    Ertl , T., Ugliano , M., Janka , H.-T., Marek , A., & Arcones , A. 2016, title Erratum: Progenitor-explosion Connection and Remnant Birth Masses for Neutrino-driven Supernovae of Iron-core Progenitors (2012, ApJ, 757, 69) , , 821, 69, 10.3847/0004-637X/821/1/69

    work page doi:10.3847/0004-637x/821/1/69 2016

  28. [28]

    D., Stairs , I

    Ferdman , R. D., Stairs , I. H., Kramer , M., et al. 2013, title The Double Pulsar: Evidence for Neutron Star Formation without an Iron Core-collapse Supernova , , 767, 85, 10.1088/0004-637X/767/1/85

    doi:10.1088/0004-637x/767/1/85 2013

  29. [29]

    P., & van den Heuvel , E

    Flannery , B. P., & van den Heuvel , E. P. J. 1975, title On the origin of the binary pulsar PSR 1913 + 16 , , 39, 61

    1975

  30. [30]

    L., Belczynski , K., Wiktorowicz , G., et al

    Fryer , C. L., Belczynski , K., Wiktorowicz , G., et al. 2012, title Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity , , 749, 91, 10.1088/0004-637X/749/1/91

    doi:10.1088/0004-637x/749/1/91 2012

  31. [31]

    2018, title The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks , , 480, 2011, 10.1093/mnras/sty1999

    Giacobbo , N., & Mapelli , M. 2018, title The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks , , 480, 2011, 10.1093/mnras/sty1999

    doi:10.1093/mnras/sty1999 2018

  32. [32]

    2023, title Mergers of neutron stars and black holes with cores of giant stars: a population synthesis study , , 523, 221, 10.1093/mnras/stad1449

    Grichener , A. 2023, title Mergers of neutron stars and black holes with cores of giant stars: a population synthesis study , , 523, 221, 10.1093/mnras/stad1449

    doi:10.1093/mnras/stad1449 2023

  33. [33]

    Grichener , A. 2025, title Mergers of compact objects with cores of massive stars: evolutionary pathways, r-process nucleosynthesis and multi-messenger signatures , , 370, 11, 10.1007/s10509-025-04402-1

    work page doi:10.1007/s10509-025-04402-1 2025

  34. [34]

    A., & Taylor , J

    Hulse , R. A., & Taylor , J. H. 1975, title Discovery of a pulsar in a binary system , , 195, L51, 10.1086/181708

    doi:10.1086/181708 1975

  35. [35]

    R., Pols , O

    Hurley , J. R., Pols , O. R., & Tout , C. A. 2000, title Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity , , 315, 543, 10.1046/j.1365-8711.2000.03426.x

    arXiv 2000

  36. [36]

    R., Tout , C

    Hurley , J. R., Tout , C. A., & Pols , O. R. 2002, title Evolution of binary stars and the effect of tides on binary populations , , 329, 897, 10.1046/j.1365-8711.2002.05038.x

    arXiv 2002

  37. [37]

    Igoshev , A. P. 2019, title Ages of radio pulsar: long-term magnetic field evolution , , 482, 3415, 10.1093/mnras/sty2945

    doi:10.1093/mnras/sty2945 2019

  38. [38]

    Igoshev , A. P. 2020, title The observed velocity distribution of young pulsars - II. Analysis of complete PSR , , 494, 3663, 10.1093/mnras/staa958

    doi:10.1093/mnras/staa958 2020

  39. [39]

    L., Belfiore , A., Stella , L., et al

    Israel , G. L., Belfiore , A., Stella , L., et al. 2017, title An accreting pulsar with extreme properties drives an ultraluminous x-ray source in NGC 5907 , Science, 355, 817, 10.1126/science.aai8635

    doi:10.1126/science.aai8635 2017

  40. [40]

    2020, Common Envelope Evolution (IOP Publishing), 10.1088/2514-3433/abb6f0

    Ivanova , N., Justham , S., & Ricker , P. 2020, Common Envelope Evolution (IOP Publishing), 10.1088/2514-3433/abb6f0

    doi:10.1088/2514-3433/abb6f0 2020

  41. [41]

    A., Cameron , P

    Jacoby , B. A., Cameron , P. B., Jenet , F. A., et al. 2006, title Measurement of Orbital Decay in the Double Neutron Star Binary PSR B2127+11C , , 644, L113, 10.1086/505742

    doi:10.1086/505742 2006

  42. [42]

    Kaaret , P., Feng , H., & Roberts , T. P. 2017, title Ultraluminous X-Ray Sources , , 55, 303, 10.1146/annurev-astro-091916-055259

    doi:10.1146/annurev-astro-091916-055259 2017

  43. [43]

    2023, title Calibration of neutron star natal kick velocities to isolated pulsar observations , , 519, 5893, 10.1093/mnras/stad019

    Kapil , V., Mandel , I., Berti , E., & M \"u ller , B. 2023, title Calibration of neutron star natal kick velocities to isolated pulsar observations , , 519, 5893, 10.1093/mnras/stad019

    doi:10.1093/mnras/stad019 2023

  44. [44]

    J., Kramer , M., Lyne , A

    Keith , M. J., Kramer , M., Lyne , A. G., et al. 2009, title PSR J1753-2240: a mildly recycled pulsar in an eccentric binary system , , 393, 623, 10.1111/j.1365-2966.2008.14234.x

    arXiv 2009

  45. [45]

    H., Manchester , R

    Kramer , M., Stairs , I. H., Manchester , R. N., et al. 2006, title Tests of General Relativity from Timing the Double Pulsar , Science, 314, 97, 10.1126/science.1132305

    doi:10.1126/science.1132305 2006

  46. [46]

    2001, title On the variation of the initial mass function , , 322, 231, 10.1046/j.1365-8711.2001.04022.x

    Kroupa , P. 2001, title On the variation of the initial mass function , , 322, 231, 10.1046/j.1365-8711.2001.04022.x

    arXiv 2001

  47. [47]

    Laplace , E., Schneider , F. R. N., & Podsiadlowski , P. 2025, title It's written in the massive stars: The role of stellar physics in the formation of black holes , , 695, A71, 10.1051/0004-6361/202451077

    doi:10.1051/0004-6361/202451077 2025

  48. [48]

    G., & Lorimer , D

    Lyne , A. G., & Lorimer , D. R. 1994, title High birth velocities of radio pulsars , , 369, 127, 10.1038/369127a0

    doi:10.1038/369127a0 1994

  49. [49]

    G., Pritchard , R

    Lyne , A. G., Pritchard , R. S., Graham-Smith , F., & Camilo , F. 1996, title Very low braking index for the Vela pulsar , , 381, 497, 10.1038/381497a0

    work page doi:10.1038/381497a0 1996

  50. [50]

    2015, title On the Accretion-fed Growth of Neutron Stars during Common Envelope , , 798, L19, 10.1088/2041-8205/798/1/L19

    MacLeod , M., & Ramirez-Ruiz , E. 2015, title On the Accretion-fed Growth of Neutron Stars during Common Envelope , , 798, L19, 10.1088/2041-8205/798/1/L19

    doi:10.1088/2041-8205/798/1/l19 2015

  51. [51]

    Maltsev , K., Schneider , F. R. N., Mandel , I., et al. 2025, title Explodability criteria for the neutrino-driven supernova mechanism , arXiv e-prints, arXiv:2503.23856, 10.48550/arXiv.2503.23856

    Pith/arXiv arXiv doi:10.48550/arxiv.2503.23856 2025

  52. [52]

    N., Hobbs , G

    Manchester , R. N., Hobbs , G. B., Teoh , A., & Hobbs , M. 2005, title The Australia Telescope National Facility Pulsar Catalogue , , 129, 1993, 10.1086/428488

    doi:10.1086/428488 2005

  53. [53]

    Mandel , I., & Broekgaarden , F. S. 2022, title Rates of compact object coalescences , Living Reviews in Relativity, 25, 1, 10.1007/s41114-021-00034-3

    doi:10.1007/s41114-021-00034-3 2022

  54. [54]

    2020, title Simple recipes for compact remnant masses and natal kicks , , 499, 3214, 10.1093/mnras/staa3043

    Mandel , I., & M \"u ller , B. 2020, title Simple recipes for compact remnant masses and natal kicks , , 499, 3214, 10.1093/mnras/staa3043

    doi:10.1093/mnras/staa3043 2020

  55. [55]

    2021, title Binary population synthesis with probabilistic remnant mass and kick prescriptions , , 500, 1380, 10.1093/mnras/staa3390

    Mandel , I., M \"u ller , B., Riley , J., et al. 2021, title Binary population synthesis with probabilistic remnant mass and kick prescriptions , , 500, 1380, 10.1093/mnras/staa3390

    work page doi:10.1093/mnras/staa3390 2021

  56. [56]

    2025, title The Neutron Star Merger Delay-time Distribution, R-process ``Knees,'' and the Metal Budget of the Galaxy , , 982, 179, 10.3847/1538-4357/ada3bd

    Maoz , D., & Nakar , E. 2025, title The Neutron Star Merger Delay-time Distribution, R-process ``Knees,'' and the Metal Budget of the Galaxy , , 982, 179, 10.3847/1538-4357/ada3bd

    doi:10.3847/1538-4357/ada3bd 2025

  57. [57]

    Massey Jr, F. J. 1951, title The Kolmogorov-Smirnov test for goodness of fit, Journal of the American statistical Association, 46, 68

    1951

  58. [58]

    J., Mazzali , P

    Moriya , T. J., Mazzali , P. A., Tominaga , N., et al. 2017, title Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars , , 466, 2085, 10.1093/mnras/stw3225

    doi:10.1093/mnras/stw3225 2017

  59. [59]

    M \"u ller , B., Heger , A., Liptai , D., & Cameron , J. B. 2016, title A simple approach to the supernova progenitor-explosion connection , , 460, 742, 10.1093/mnras/stw1083

    doi:10.1093/mnras/stw1083 2016

  60. [60]

    2025, title Formation of heavy double neutron stars I

    Nair , A., & Stevenson , S. 2025, title Formation of heavy double neutron stars I. Eddington-limited accretion for a 1.4 M _ neutron star at solar metallicity , , 543, 233, 10.1093/mnras/staf1397

    doi:10.1093/mnras/staf1397 2025

  61. [61]

    2015, title Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors , , 67, 107, 10.1093/pasj/psv073

    Nakamura , K., Takiwaki , T., Kuroda , T., & Kotake , K. 2015, title Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors , , 67, 107, 10.1093/pasj/psv073

    doi:10.1093/pasj/psv073 2015

  62. [62]

    U., Tauris , T

    Ng , C., Kruckow , M. U., Tauris , T. M., et al. 2018, title PSR J1755-2550: a young radio pulsar with a massive, compact companion , , 476, 4315, 10.1093/mnras/sty482

    work page doi:10.1093/mnras/sty482 2018

  63. [63]

    \"O pik , E. 1924, title Statistical Studies of Double Stars: On the Distribution of Relative Luminosities and Distances of Double Stars in the Harvard Revised Photometry North of Declination -31 , Publications of the Tartu Astrofizica Observatory, 25, 1

    1924

  64. [64]

    A., & Sukhbold , T

    Patton , R. A., & Sukhbold , T. 2020, title Towards a realistic explosion landscape for binary population synthesis , , 499, 2803, 10.1093/mnras/staa3029

    doi:10.1093/mnras/staa3029 2020

  65. [66]

    S., & Sigurdsson , S

    Phinney , E. S., & Sigurdsson , S. 1991, title Ejection of pulsars and binaries to the outskirts of globular clusters , , 349, 220, 10.1038/349220a0

    doi:10.1038/349220a0 1991

  66. [67]

    R., Schr \"o der , K.-P., Hurley , J

    Pols , O. R., Schr \"o der , K.-P., Hurley , J. R., Tout , C. A., & Eggleton , P. P. 1998, title Stellar evolution models for Z = 0.0001 to 0.03 , , 298, 525, 10.1046/j.1365-8711.1998.01658.x

    arXiv 1998

  67. [68]

    M., Farrow , N., Stevenson , S., Thrane , E., & Zhu , X.-J

    Romero-Shaw , I. M., Farrow , N., Stevenson , S., Thrane , E., & Zhu , X.-J. 2020, title On the origin of GW190425 , , 496, L64, 10.1093/mnrasl/slaa084

    doi:10.1093/mnrasl/slaa084 2020

  68. [69]

    E., de Koter , A., et al

    Sana , H., de Mink , S. E., de Koter , A., et al. 2012, title Binary Interaction Dominates the Evolution of Massive Stars , Science, 337, 444, 10.1126/science.1223344

    doi:10.1126/science.1223344 2012

  69. [70]

    Schneider , F. R. N., Podsiadlowski , P., & Laplace , E. 2023, title Bimodal Black Hole Mass Distribution and Chirp Masses of Binary Black Hole Mergers , , 950, L9, 10.3847/2041-8213/acd77a

    doi:10.3847/2041-8213/acd77a 2023

  70. [71]

    Schneider , F. R. N., Podsiadlowski , P., & M \"u ller , B. 2021, title Pre-supernova evolution, compact-object masses, and explosion properties of stripped binary stars , , 645, A5, 10.1051/0004-6361/202039219

    doi:10.1051/0004-6361/202039219 2021

  71. [72]

    2018, title On the Role of Supernova Kicks in the Formation of Galactic Double Neutron Star Systems , , 867, 124, 10.3847/1538-4357/aae648

    Shao , Y., & Li , X.-D. 2018, title On the Role of Supernova Kicks in the Formation of Galactic Double Neutron Star Systems , , 867, 124, 10.3847/1538-4357/aae648

    work page doi:10.3847/1538-4357/aae648 2018

  72. [73]

    2022, title Remnant masses of core collapse supernovae in the jittering jets explosion mechanism , , 513, 4224, 10.1093/mnras/stac1075

    Shishkin , D., & Soker , N. 2022, title Remnant masses of core collapse supernovae in the jittering jets explosion mechanism , , 513, 4224, 10.1093/mnras/stac1075

    doi:10.1093/mnras/stac1075 2022

  73. [74]

    Stairs, I. H. 2004, title Pulsars in binary systems: Probing binary stellar evolution and general relativity, 304, 547

    2004

  74. [75]

    2017, title Formation of the first three gravitational-wave observations through isolated binary evolution , Nat

    Stevenson , S., Vigna-G \'o mez , A., Mandel , I., et al. 2017, title Formation of the first three gravitational-wave observations through isolated binary evolution , Nat. Commun., 8, 14906, 10.1038/ncomms14906

    doi:10.1038/ncomms14906 2017

  75. [76]

    2020, title Missing red supergiants and carbon burning , , 492, 2578, 10.1093/mnras/staa059

    Sukhbold , T., & Adams , S. 2020, title Missing red supergiants and carbon burning , , 492, 2578, 10.1093/mnras/staa059

    doi:10.1093/mnras/staa059 2020

  76. [77]

    E., Brown , J

    Sukhbold , T., Ertl , T., Woosley , S. E., Brown , J. M., & Janka , H.-T. 2016, title Core-collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions , , 821, 38, 10.3847/0004-637X/821/1/38

    doi:10.3847/0004-637x/821/1/38 2016

  77. [78]

    2016, title Progenitor-dependent Explosion Dynamics in Self-consistent, Axisymmetric Simulations of Neutrino-driven Core-collapse Supernovae , , 825, 6, 10.3847/0004-637X/825/1/6

    Summa , A., Hanke , F., Janka , H.-T., et al. 2016, title Progenitor-dependent Explosion Dynamics in Self-consistent, Axisymmetric Simulations of Neutrino-driven Core-collapse Supernovae , , 825, 6, 10.3847/0004-637X/825/1/6

    doi:10.3847/0004-637x/825/1/6 2016

  78. [79]

    M., Langer , N., & Kramer , M

    Tauris , T. M., Langer , N., & Kramer , M. 2012, title Formation of millisecond pulsars with CO white dwarf companions - II. Accretion, spin-up, true ages and comparison to MSPs with He white dwarf companions , , 425, 1601, 10.1111/j.1365-2966.2012.21446.x

    arXiv 2012

  79. [80]

    M., Langer , N., & Podsiadlowski , P

    Tauris , T. M., Langer , N., & Podsiadlowski , P. 2015, title Ultra-stripped supernovae: progenitors and fate , , 451, 2123, 10.1093/mnras/stv990

    doi:10.1093/mnras/stv990 2015

  80. [81]

    M., Kramer , M., Freire , P

    Tauris , T. M., Kramer , M., Freire , P. C. C., et al. 2017, title Formation of Double Neutron Star Systems , , 846, 170, 10.3847/1538-4357/aa7e89

    doi:10.3847/1538-4357/aa7e89 2017

Showing first 80 references.