pith. sign in

arxiv: 2606.23773 · v1 · pith:2ZUNFJ4Knew · submitted 2026-06-22 · 🌌 astro-ph.HE · gr-qc

Modern tidal interaction models for rapid binary population synthesis: II. Binary black hole formation, mergers, and spins

Veome Kapil , Ilya Mandel , Jeff Riley , Evgeni Grishin , Jim Fuller , Emanuele Berti This is my paper

Pith reviewed 2026-06-26 07:10 UTC · model grok-4.3

classification 🌌 astro-ph.HE gr-qc
keywords binary black holestidal dissipationpopulation synthesiseffective spingravitational wavesisolated binary evolutionmerger ratesspin distribution
0
0 comments X

The pith

Isolated binary evolution with updated tides produces mostly low effective spin black hole mergers for current detectors.

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

The paper updates rapid population synthesis with a new self-consistent treatment of tidal dissipation in binaries. This leads to most first-born black holes having zero spin except in chemically homogeneous evolution cases. Second-born black hole spins vary strongly with tidal efficiency and mass transfer history, and are not always orbitally synchronized before the supernova. High effective spin systems form tighter and merge faster, placing them at higher redshifts where current detectors have limited reach. As a result the observed population today is predicted to show strong bias toward low χ_eff, shifting only when detectors access higher redshifts.

Core claim

Using the updated tidal model in COMPAS, the intrinsic χ_eff distribution of merging binary black holes from isolated evolution is strongly biased low for present-day detectors, with roughly one third of systems below 0.05 and only about three percent above 0.5; high χ_eff binaries merge at higher redshifts due to smaller separations at black hole formation and shorter coalescence times, so the fraction above 0.5 rises to about fifteen percent once detectors reach those earlier epochs.

What carries the argument

Self-consistent tidal dissipation implementation that determines spin synchronization efficiency from stellar mass, evolutionary stage, and mass transfer history.

Load-bearing premise

The new tidal dissipation model accurately captures efficiency and its dependence on mass transfer history across all relevant stellar masses and evolutionary stages.

What would settle it

A statistically significant sample of low-redshift merging binary black holes showing substantially more than three percent with χ_eff above 0.5 would contradict the predicted selection bias.

Figures

Figures reproduced from arXiv: 2606.23773 by Emanuele Berti, Evgeni Grishin, Ilya Mandel, Jeff Riley, Jim Fuller, Veome Kapil.

Figure 1
Figure 1. Figure 1: Yield of BBH formations and mergers, normal￾ized to total star forming mass, across the three tidal pre￾scriptions considered in this work. This figure integrates over the log-uniform distribution of simulated metallicities. For each tidal dissipation model considered in this work, we obtain BBH samples across a range of masses, separations, and metallicities. To determine potential GW sources, we select o… view at source ↗
Figure 2
Figure 2. Figure 2: Yield of BBHs that merge within 13.8 Gyr by for￾mation scenario, integrated over the log-uniform distribution of simulated metallicities, across the three tidal prescriptions considered in this work. In the broad context of binary evolution, we can think of our three simulations as representing choices on a con￾tinuous axis of tidal dissipation effectiveness, going from weakest (LEGACY) to strongest (PERFE… view at source ↗
Figure 3
Figure 3. Figure 3: Evolution of a BBH progenitor that goes through common envelope with both KAPIL26 (left) and PERFECT (right) tides. The initial parameters in both cases are M1,ZAMS = 26.7M⊙, M2,ZAMS = 24.1M⊙, aZAMS = 502.5R⊙, eZAMS = 0.04, and ZZAMS = 0.0002. The important episodes shown here are: ZAMS, SMT initiated by the primary (SMT1), primary supernova (SN1), common envelope initiated by the secondary (CE2), secondar… view at source ↗
Figure 4
Figure 4. Figure 4: Evolution of a BBH progenitor that goes through only SMT with both KAPIL26 (left) and PERFECT (right) tides. The initial parameters in both cases are M1,ZAMS = 36.6M⊙, M2,ZAMS = 23.6M⊙, aZAMS = 70.2R⊙, eZAMS = 0.351, and ZZAMS = 0.0005. The important episodes shown here are ZAMS, SMT initiated by the primary (SMT1), primary supernova (SN1), SMT initiated by the secondary (SMT2), secondary supernova (SN2), … view at source ↗
Figure 5
Figure 5. Figure 5: Dimensionless BH spin distributions of the pri￾mary (defined as the more massive component at ZAMS) and secondary (defined as the less massive component at ZAMS), across the three simulated populations. The simulations rep￾resent a log-uniform initial stellar metallicity distribution, and are not weighted to represent a realistic cosmic star for￾mation history. calculations. The peak at zero spin correspon… view at source ↗
Figure 6
Figure 6. Figure 6: Dimensionless BH spin distributions of the more massive (top panel) and less massive (bottom panel) BH components across the three simulated populations. The simulations represent a log-uniform initial stellar metallic￾ity distribution, and are not weighted to represent a realistic cosmic star formation history. three populations in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Dimensionless secondary BH spins (with sec￾ondary defined as the less massive component at ZAMS) vs. orbital period prior to secondary SN (note reversed axes), for the BBHs that merge within 13.8 Gyr as obtained with the LEGACY (top), KAPIL26 (middle), and PERFECT (bot￾tom) simulations. The red data points correspond to the secondary receiving fractional fallback ffb < 0.1 after SN2, whereas the blue, purp… view at source ↗
Figure 8
Figure 8. Figure 8: Dimensionless BH spin distributions of the pri￾mary (defined as the more massive ZAMS star) (top panel) and secondary (bottom panel) for the merging BBHs across the three tidal models. The spin distributions are weighted by the appropriate metallicity-specific star formation rates. log-uniform distribution of metallicities. In reality, al￾though there is a broad metallicity distribution at any formation re… view at source ↗
Figure 9
Figure 9. Figure 9: χeff probability distributions of BBH mergers with the LEGACY (left), KAPIL26 (center) and PERFECT (right) tides models, broken into sub-populations corresponding to CE, SMT, and CHE formation channels. 6.1. 1D Spin Distributions We show the expected intrinsic component spin dis￾tributions for the three tidal models considered in this work in [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: For the KAPIL26 population only: total BBH mass (MBH,tot = M1 +M2) vs. mass ratio (q = M2/M1) vs. effective spin (χeff ) for BBHs. q > 1 indicates that the binary experienced mass ratio reversal. All the BBHs merge within 13.8 Gyr of ZAMS formation [PITH_FULL_IMAGE:figures/full_fig_p016_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: For the KAPIL26 population only: effective spin (χeff ) vs. coalescence time (tcoal) for all BBHs that merge within 13.8 Gyr. 0.0 0.2 0.4 0.6 0.8 1.0 eff 0.0 2.5 5.0 7.5 10.0 12.5 P ( e ff ) z=0 z=1 z=2 z=5 [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: The distributions of χeff for binaries at sev￾eral merger redshifts in the KAPIL26 simulation; all binaries merging at that redshift are included, weighted by their re￾spective merger rates, without accounting for observational selection effects. All distributions are independently normal￾ized. to all BBH mergers in the visible Universe. As detec￾tor sensitivity improves through O5 and toward third￾genera… view at source ↗
Figure 13
Figure 13. Figure 13: Left panel: the distribution of χeff among detectable BBHs from the KAPIL26 population, assuming a typical O4-like sensitivity and the assumption that perfect detectors can detect all mergers in the visible Universe. Right panel: the distributions of χeff among detectable BBHs from the KAPIL26 population assuming a typical O4-like sensitivity, split up by formation channel. All distributions are independe… view at source ↗
Figure 14
Figure 14. Figure 14: Dimensionless BH spin distributions for the primary component at ZAMS (top panel) and the secondary component at ZAMS (bottom panel). The default KAPIL26 distribution is shown in blue, and spins obtained by using the S. S. Bavera et al. (2021a) fit on the same population are shown in purple. 0.0 0.2 0.4 0.6 0.8 1.0 eff 0 5 10 P ( e ff ) KAPIL26 Bavera et al. (2021) Fit [PITH_FULL_IMAGE:figures/full_fig_p… view at source ↗
Figure 15
Figure 15. Figure 15: χeff distributions for the merging BBHs with the KAPIL26 population using the fiducial tidal model (blue), and using the S. S. Bavera et al. (2021a) fit (purple) to de￾termine spin magnitudes. A. BAVERA ET AL. (2021) SPIN MAGNITUDES The spin magnitudes of BHs following supernovae in this work depend on our assumption of angular momen￾tum conservation, as described in Sec. 5. However, there are other theor… view at source ↗
Figure 16
Figure 16. Figure 16: χeff probability distributions of merging BBHs with the KAPIL26 (left) and Z77 (right) tides models, split by the CE, SMT, and CHE formation scenarios. The distributions are weighted to reflect the metallicity-specific star formation history of the Universe as per Sec. 6. between the two tidal models, with mild differences aris￾ing for low-spin BHs. The key tidal dissipation mech￾anism involved in synchro… view at source ↗
read the original abstract

We present predictions for the merger rates and effective spin ($\chi_{\rm eff}$) distribution of binary black holes (BBHs) from isolated binary evolution, using a new self-consistent tidal dissipation implementation in the rapid binary population synthesis code COMPAS. Most of the first-born black holes (BHs) in our simulated merging BBHs are formed with zero spins, with the exception of BBHs formed from chemically homogeneous evolution. The spins of the second-born BHs with the new model depend significantly on the efficiency of tidal dissipation and mass transfer history, and crucially, are not always consistent with pre-supernova synchronization. High-$\chi_{\rm eff}$ binaries preferentially merge at high redshift due to smaller binary separations at BBH formation and shorter coalescence times, thus rendering them largely inaccessible to current gravitational wave (GW) detectors. We expect the intrinsic spin distribution of merging BBHs formed from isolated evolution to be strongly biased toward low $\chi_{\rm eff}$ with current detectors, with a third of systems having $\chi_{\rm eff} < 0.05$ and only $\sim 3\%$ with $\chi_{\rm eff}>0.5$. However, $\chi_{\rm eff}$ will increase as GW detectors become sensitive to higher redshift sources, with up to $\sim 15\%$ of systems having $\chi_{\rm eff}>0.5$.

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 predictions for BBH merger rates and χ_eff distributions from isolated binary evolution using a new self-consistent tidal dissipation implementation in COMPAS. It claims most first-born BHs form with zero spin (except chemically homogeneous evolution cases), second-born BH spins depend significantly on tidal dissipation efficiency and mass-transfer history (not always pre-SN synchronized), high-χ_eff systems preferentially merge at high redshift due to smaller separations and shorter coalescence times, and the intrinsic distribution for current detectors is biased low (∼1/3 with χ_eff < 0.05, ∼3% with χ_eff > 0.5), increasing to ∼15% >0.5 at higher redshifts accessible to future detectors.

Significance. If the tidal model holds, the results would be significant for GW astrophysics by providing falsifiable predictions for the isolated-channel contribution to the observed BBH spin distribution, including its redshift evolution, and by highlighting how tidal interactions after mass transfer shape second-born BH spins.

major comments (2)
  1. [Tidal model section (implementation and results)] The headline χ_eff fractions and redshift-evolution claim rest on the new tidal dissipation implementation. No benchmarks or comparisons against detailed stellar models (e.g., MESA grids spanning the relevant mass range and post-mass-transfer stages) are referenced to validate the efficiency or its dependence on mass-transfer history; this is load-bearing because the abstract states second-born spins “depend significantly on the efficiency of tidal dissipation and mass transfer history.”
  2. [Results on χ_eff distributions] The reported low-χ_eff bias (1/3 systems <0.05) is presented as robust, yet the model includes a free parameter for tidal dissipation efficiency whose variation range and impact on the quoted percentages are not quantified; without this, it is unclear whether the bias is a genuine prediction or an artifact of the chosen efficiency value.
minor comments (2)
  1. [Abstract] Clarify in the abstract or methods the specific range of tidal dissipation efficiencies explored and whether any observational constraints were used to set it.
  2. [Methods] Add a short table or figure caption explicitly listing the free parameters retained in the new tidal model versus those fixed by the self-consistent treatment.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their insightful comments, which have helped us improve the clarity and robustness of our manuscript. Below we address each major comment in turn, outlining the revisions we intend to make.

read point-by-point responses

  1. Referee: The headline χ_eff fractions and redshift-evolution claim rest on the new tidal dissipation implementation. No benchmarks or comparisons against detailed stellar models (e.g., MESA grids spanning the relevant mass range and post-mass-transfer stages) are referenced to validate the efficiency or its dependence on mass-transfer history; this is load-bearing because the abstract states second-born spins “depend significantly on the efficiency of tidal dissipation and mass transfer history.”

    Authors: The tidal dissipation model is introduced and its implementation validated against detailed calculations in the companion paper (Paper I). However, we agree that explicit references to benchmarks, particularly for post-mass-transfer stages relevant to second-born BHs, would strengthen the presentation in this work. In the revised manuscript, we will add a new subsection in the methods that summarizes the validation performed in Paper I, including comparisons to MESA grids where available, and discuss the dependence on mass-transfer history. We will also cite additional literature on tidal synchronization in massive binaries. revision: yes

  2. Referee: The reported low-χ_eff bias (1/3 systems <0.05) is presented as robust, yet the model includes a free parameter for tidal dissipation efficiency whose variation range and impact on the quoted percentages are not quantified; without this, it is unclear whether the bias is a genuine prediction or an artifact of the chosen efficiency value.

    Authors: We acknowledge that the sensitivity to the tidal dissipation efficiency parameter was not fully explored in the submitted version. To address this, we will conduct additional simulations varying the efficiency parameter across its physically motivated range and include these results in a new figure or table in the revised manuscript. This will quantify the impact on the χ_eff distribution fractions and demonstrate the robustness of the reported low-χ_eff bias for the fiducial choice. revision: yes

Circularity Check

0 steps flagged

No significant circularity; outputs are simulation results from new model, not reductions to inputs

full rationale

The provided abstract and context describe predictions generated by running the COMPAS population synthesis code with a newly implemented tidal dissipation prescription. No equations, fitting procedures, or self-referential definitions are visible that would make the reported χ_eff distribution or merger rates equivalent to the model inputs by construction. The spin outcomes are stated to depend on dissipation efficiency and mass-transfer history, but this is presented as a model consequence rather than a tautology or fitted prediction. No load-bearing self-citation chain or ansatz smuggling is exhibited in the text. The derivation chain is therefore self-contained against external benchmarks for the purpose of this circularity analysis.

Axiom & Free-Parameter Ledger

1 free parameters · 0 axioms · 0 invented entities

Only the abstract is available, so the ledger is necessarily incomplete. The central claims rest on the accuracy of the new tidal dissipation implementation and on the assumption that the simulated population represents isolated binary evolution.

free parameters (1)
  • tidal dissipation efficiency
    Abstract states that second-born BH spins depend significantly on the efficiency of tidal dissipation, indicating it functions as a key adjustable parameter.

pith-pipeline@v0.9.1-grok · 5801 in / 1399 out tokens · 40479 ms · 2026-06-26T07:10:42.797276+00:00 · methodology

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

164 extracted references · 133 canonical work pages · 52 internal anchors

  1. [1]

    Evidence for additional structure in the effective spin distribution hints at multiple formation pathways in GWTC-5.0

    Alvarez-Lopez, Sofia and Heinzel, Jack and Vitale, Salvatore. Evidence for additional structure in the effective spin distribution hints at multiple formation pathways in GWTC-5.0. 2026. arXiv:2606.12205

    Pith/arXiv arXiv 2026

  2. [2]

    Abac, A. G. and others. GWTC-5.0: Population Properties of Merging Compact Binaries. 2026. arXiv:2605.27226

    Pith/arXiv arXiv 2026

  3. [3]

    Abac, A. G. and others. GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog. 2026. arXiv:2605.27225

    Pith/arXiv arXiv 2026

  4. [4]

    and Broekgaarden, Floor S

    Vigna-G\'omez, Alejandro and MacLeod, Morgan and Neijssel, Coenraad J. and Broekgaarden, Floor S. and Justham, Stephen and Howitt, George and de Mink, Selma E. and Vinciguerra, Serena and Mandel, Ilya. Common-Envelope Episodes that lead to Double Neutron Star formation. Publ. Astron. Soc. Aust. 2020. doi:10.1017/pasa.2020.31. arXiv:2001.09829

    work page doi:10.1017/pasa.2020.31 2020

  5. [5]

    Monthly Notices of the Royal Astronomical Society , volume =

    Vick, Michelle and Lai, Dong , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2020 , month =. doi:10.1093/mnras/staa1784 , url =

    work page doi:10.1093/mnras/staa1784 2020

  6. [6]

    Monthly Notices of the Royal Astronomical Society , volume =

    Vick, Michelle and Lai, Dong , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2018 , month =. doi:10.1093/mnras/sty225 , url =

    work page doi:10.1093/mnras/sty225 2018

  7. [7]

    and Tout, Christopher A

    Hurley, Jarrod R. and Tout, Christopher A. and Pols, Onno R. Evolution of binary stars and the effect of tides on binary populations. Mon. Not. R. Astron. Soc. 2002. doi:10.1046/j.1365-8711.2002.05038.x. arXiv:astro-ph/0201220

    work page doi:10.1046/j.1365-8711.2002.05038.x 2002

  8. [8]

    , volume =

    Tidal evolution in close binary systems. , volume =. Astronomy and Astrophysics , author =. 1981 , pages =

    1981

  9. [9]

    , volume =

    Tidal friction in close binary systems. , volume =. Astronomy and Astrophysics , author =. 1977 , pages =

    1977

  10. [10]

    Flipping spins in mass transferring binaries and origin of spin-orbit misalignment in binary black holes

    Stegmann, Jakob and Antonini, Fabio. Flipping spins in mass transferring binaries and origin of spin-orbit misalignment in binary black holes. Phys. Rev. D. 2021. doi:10.1103/PhysRevD.103.063007. arXiv:2012.06329

    work page doi:10.1103/physrevd.103.063007 2021

  11. [11]

    Dynamical Formation of Close Binaries During the Pre-main-sequence Phase

    Moe, Maxwell and Kratter, Kaitlin M. Dynamical Formation of Close Binaries During the Pre-main-sequence Phase. Astrophys. J. 2018. doi:10.3847/1538-4357/aaa6d2. arXiv:1706.09894

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaa6d2 2018

  12. [12]

    The Role of Chaos in the Circularization of Tidal Capture Binaries. I. The Chaos Boundary. Astrophys. J. doi:10.1086/176178 , adsurl =

    work page doi:10.1086/176178

  13. [13]

    Compact Object Modeling with the StarTrack Population Synthesis Code

    Belczynski, Krzystof and Kalogera, Vassiliki and Rasio, Frederic A. and Taam, Ronald E. and Zezas, Andreas and Bulik, Tomasz and Maccarone, Thomas J. and Ivanova, Natalia. Compact object modeling with the startrack population synthesis code. Astrophys. J. Supp. S. 2008. doi:10.1086/521026. arXiv:astro-ph/0511811

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/521026 2008

  14. [14]

    Astronomy and Astrophysics, vol

    Stability of tidal equilibrium , author=. Astronomy and Astrophysics, vol. 92, no. 1-2, Dec. 1980, p. 167-170. , volume=

    1980

  15. [15]

    Song, H. F. and Meynet, G. and Maeder, A. and Ekstr. Close binary evolution -. Astronomy & Astrophysics , language =. 2018 , bdsk-url-1 =. doi:10.1051/0004-6361/201731073 , issn =

    work page doi:10.1051/0004-6361/201731073 2018

  16. [16]

    The spin of the second-born black hole in coalescing binary black holes

    Qin, Y. and Fragos, T. and Meynet, G. and Andrews, J. and S rensen, M. and Song, H. F. The spin of the second-born black hole in coalescing binary black holes. Astron. Astrophys. 2018. doi:10.1051/0004-6361/201832839. arXiv:1802.05738

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201832839 2018

  17. [17]

    Type Ib/c supernovae in binary systems I. Evolution and properties of the progenitor stars

    Yoon, Sung-Chul and Woosley, Stan E. and Langer, Norbert. Type Ib/c supernovae in binary systems I. Evolution and properties of the progenitor stars. Astrophys. J. 2010. doi:10.1088/0004-637X/725/1/940. arXiv:1004.0843

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/725/1/940 2010

  18. [18]

    Astrophys

    On formation of close binaries by two-body tidal capture. Astrophys. J. doi:10.1086/155143 , adsurl =

    work page doi:10.1086/155143

  19. [19]

    om, Sylvia and Eggenberger, Patrick and Meynet, Georges and Fragos, Tassos and Song, Han Feng , title =

    Sciarini, Luca and Ekstr\"om, Sylvia and Eggenberger, Patrick and Meynet, Georges and Fragos, Tassos and Song, Han Feng , title = ". Astron. Astrophys. 2024. doi:10.1051/0004-6361/202348424. arXiv:2312.08437

    work page doi:10.1051/0004-6361/202348424 2024

  20. [20]

    Chaotic dynamics of wide triples induced by galactic tides: a novel channel for producing compact binaries, mergers, and collisions

    Grishin, Evgeni and Perets, Hagai B. Chaotic dynamics of wide triples induced by galactic tides: a novel channel for producing compact binaries, mergers, and collisions. Mon. Not. R. Astron. Soc. 2022. doi:10.1093/mnras/stac706. arXiv:2112.11475

    work page doi:10.1093/mnras/stac706 2022

  21. [21]

    Rasio, F. A. and Tout, C. A. and Lubow, S. H. and Livio, M. Tidal decay of close planetary orbits. Astrophys. J. 1996. doi:10.1086/177941. arXiv:astro-ph/9605059

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/177941 1996

  22. [22]

    Preece and Adrian S

    Holly P. Preece and Adrian S. Hamers and Patrick G. Neunteufel and Adam L. Schaefer and Christopher A. Tout , doi =. The Equilibrium Tide: An Updated Prescription for Population Synthesis Codes , url =. The Astrophysical Journal , month =. 2022 , bdsk-url-1 =

    2022

  23. [23]

    The Equilibrium-Tide Model for Tidal Friction

    Eggleton, Peter P. and Kiseleva, Ludmila G. and Hut, Piet. The Equilibrium tide model for tidal friction. Astrophys. J. 1998. doi:10.1086/305670. arXiv:astro-ph/9801246

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/305670 1998

  24. [24]

    and Waldman, Roni , title = "

    Kushnir, Doron and Zaldarriaga, Matias and Kollmeier, Juna A. and Waldman, Roni , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2017 , month =. doi:10.1093/mnras/stx255 , url =

    work page doi:10.1093/mnras/stx255 2017

  25. [25]

    doi:10.1051/0004-6361/202040174 , journal =

    Dynamical tide in stellar radiative zones - General formalism and evolution for low-mass stars , url =. doi:10.1051/0004-6361/202040174 , journal =

    work page doi:10.1051/0004-6361/202040174

  26. [26]

    Tidal dissipation in stars and giant planets

    Ogilvie, Gordon I. Tidal dissipation in stars and giant planets. Annu. Rev. Astron. Astrophys. 2014. doi:10.1146/annurev-astro-081913-035941. arXiv:1406.2207

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081913-035941 2014

  27. [27]

    Monthly Notices of the Royal Astronomical Society , keywords =

    Tidal dissipation in evolving low-mass and solar-type stars with predictions for planetary orbital decay. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/staa2405 , archivePrefix =. 2008.03262 , primaryClass =

    work page doi:10.1093/mnras/staa2405 2008

  28. [28]

    Monthly Notices of the Royal Astronomical Society , volume =

    Duguid, Craig D and Barker, Adrian J and Jones, C A , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2020 , month =. doi:10.1093/mnras/staa2216 , url =

    work page doi:10.1093/mnras/staa2216 2020

  29. [29]

    , keywords =

    Hurley, Jarrod R. and Pols, Onno R. and Tout, Christopher A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. R. Astron. Soc. 2000. doi:10.1046/j.1365-8711.2000.03426.x. arXiv:astro-ph/0001295

    work page doi:10.1046/j.1365-8711.2000.03426.x 2000

  30. [30]

    Fits for the convective envelope mass in massive stars

    Picker, Lewis and Hirai, Ryosuke and Mandel, Ilya. Fits for the convective envelope mass in massive stars. 2024. arXiv:2402.13180

    arXiv 2024

  31. [31]

    Tides in rotating barotropic fluid bodies: the contribution of inertial waves and the role of internal structure

    Ogilvie, Gordon I. Tides in rotating barotropic fluid bodies: the contribution of inertial waves and the role of internal structure. Mon. Not. R. Astron. Soc. 2013. doi:10.1093/mnras/sts362. arXiv:1211.0837

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts362 2013

  32. [32]

    Astronomy and Astrophysics , keywords =

    The dynamical tide in close binaries. Astronomy and Astrophysics , keywords =

  33. [33]

    Calibration of Equilibrium Tide Theory for Extrasolar Planet Systems

    Hansen, Brad. Calibration of Equilibrium Tide Theory for Extrasolar Planet Systems. Astrophys. J. 2010. doi:10.1088/0004-637X/723/1/285. arXiv:1009.3027

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/723/1/285 2010

  34. [34]

    2024 , eprint=

    Rotational synchronisation of B-type binaries in 30 Doradus , author=. 2024 , eprint=

    2024

  35. [35]

    Love, A. E. H. , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 1909 , month =. doi:10.1093/mnras/69.6.476 , url =

    work page doi:10.1093/mnras/69.6.476 1909

  36. [36]

    Sloan Low-Mass Wide Pairs of Kinematically Equivalent Stars (SLoWPoKES): A Catalog of Very Wide, Low-mass Pairs

    Dhital, Saurav and West, Andrew A. and Stassun, Keivan G. and Bochanski, John J. Sloan Low-Mass Wide Pairs of Kinematically Equivalent Stars (SLoWPoKES): A Catalog of Very Wide, Low-mass Pairs. Astron. J. 2010. doi:10.1088/0004-6256/139/6/2566. arXiv:1004.2755

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/139/6/2566 2010

  37. [37]

    The Sloan Digital Sky Survey: Technical Summary

    York, Donald G. and others. The Sloan Digital Sky Survey: Technical Summary. Astron. J. 2000. doi:10.1086/301513. arXiv:astro-ph/0006396

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301513 2000

  38. [38]

    The Seventh Data Release of the Sloan Digital Sky Survey

    Abazajian, Kevork N. and others. The Seventh Data Release of the Sloan Digital Sky Survey. Astrophys. J. Supp. S. 2009. doi:10.1088/0067-0049/182/2/543. arXiv:0812.0649

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/182/2/543 2009

  39. [39]

    Monthly Notices of the Royal Astronomical Society , volume =

    Hwang, Hsiang-Chih and Ting, Yuan-Sen and Zakamska, Nadia L , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month =. doi:10.1093/mnras/stac675 , url =

    work page doi:10.1093/mnras/stac675 2022

  40. [40]

    10.1051/0004-6361/202244144

    Combining HIPPARCOS and Gaia data for the study of binaries: The BINARYS tool , DOI= "10.1051/0004-6361/202244144", url= "https://doi.org/10.1051/0004-6361/202244144", journal =

    work page doi:10.1051/0004-6361/202244144

  41. [41]

    Perryman, M. A. C. and others. The Hipparcos catalogue. Astron. Astrophys. 1997

    1997

  42. [42]

    10.1051/0004-6361/202243782

    Gaia Data Release 3 - Stellar multiplicity, a teaser for the hidden treasure , DOI= "10.1051/0004-6361/202243782", url= "https://doi.org/10.1051/0004-6361/202243782", journal =

    work page doi:10.1051/0004-6361/202243782

  43. [43]

    Mathieu , title =

    Søren Meibom and Robert D. Mathieu , title =. The Astrophysical Journal , abstract =. 2005 , month =. doi:10.1086/427082 , url =

    work page doi:10.1086/427082 2005

  44. [44]

    J. J. Zanazzi , title =. The Astrophysical Journal Letters , abstract =. 2022 , month =. doi:10.3847/2041-8213/ac6516 , url =

    work page doi:10.3847/2041-8213/ac6516 2022

  45. [45]

    and Mayor, M

    Duquennoy, A. and Mayor, M. Multiplicity among solar - type stars in the solar neighbourhood. 2. Distribution of the orbital elements in an unbiased sample. Astron. Astrophys. 1991

    1991

  46. [46]

    Peacock, J. A. , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 1983 , month =. doi:10.1093/mnras/202.3.615 , url =

    work page doi:10.1093/mnras/202.3.615 1983

  47. [47]

    E. M. Leiner and R. D. Mathieu and N. M. Gosnell and A. M. Geller , title =. The Astronomical Journal , abstract =. 2015 , month =. doi:10.1088/0004-6256/150/1/10 , url =

    work page doi:10.1088/0004-6256/150/1/10 2015

  48. [48]

    Statistical view of orbital circularisation with 14 000 characterised TESS eclipsing binaries

  49. [49]

    10.1051/0004-6361/201833816

    Orbital properties of binary post-AGB stars , DOI= "10.1051/0004-6361/201833816", url= "https://doi.org/10.1051/0004-6361/201833816", journal =

    work page doi:10.1051/0004-6361/201833816

  50. [50]

    Behr and Andrew T

    Bradford B. Behr and Andrew T. Cenko and Arsen R. Hajian and Robert S. McMillan and Marc Murison and Jeff Meade and Robert Hindsley , title =. The Astronomical Journal , abstract =. 2011 , month =. doi:10.1088/0004-6256/142/1/6 , url =

    work page doi:10.1088/0004-6256/142/1/6 2011

  51. [51]

    Vitesses radiales et

    Prevot, L , journal=. Vitesses radiales et

  52. [52]

    10.1051/aas:2000237

    Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses , DOI= "10.1051/aas:2000237", url= "https://doi.org/10.1051/aas:2000237", journal =

    work page doi:10.1051/aas:2000237

  53. [53]

    Evolution of the Convective Core Mass during the Main Sequence

    Shikauchi, Minori and Hirai, Ryosuke and Mandel, Ilya. Evolution of the Convective Core Mass during the Main Sequence. 2024. arXiv:2409.00460

    arXiv 2024

  54. [54]

    and Fragos, Tassos and Qin, Ying and Zapartas, Emmanouil and Neijssel, Coenraad J

    Bavera, Simone S. and Fragos, Tassos and Qin, Ying and Zapartas, Emmanouil and Neijssel, Coenraad J. and Mandel, Ilya and Batta, Aldo and Gaebel, Sebastian M. and Kimball, Chase and Stevenson, Simon. The origin of spin in binary black holes: Predicting the distributions of the main observables of Advanced LIGO. Astron. Astrophys. 2020. doi:10.1051/0004-63...

    work page doi:10.1051/0004-6361/201936204 2020

  55. [55]

    Double Compact Objects III: Gravitational Wave Detection Rates

    Dominik, Michal and Berti, Emanuele and O'Shaughnessy, Richard and Mandel, Ilya and Belczynski, Krzysztof and Fryer, Christopher and Holz, Daniel E. and Bulik, Tomasz and Pannarale, Francesco. Double Compact Objects III: Gravitational Wave Detection Rates. Astrophys. J. 2015. doi:10.1088/0004-637X/806/2/263. arXiv:1405.7016

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/806/2/263 2015

  56. [56]

    Gallegos-Garcia, Monica and Berry, Christopher P. L. and Marchant, Pablo and Kalogera, Vicky. Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates. Astrophys. J. 2021. doi:10.3847/1538-4357/ac2610. arXiv:2107.05702

    work page doi:10.3847/1538-4357/ac2610 2021

  57. [57]

    and others

    Bavera, Simone S. and others. Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts. Astron. Astrophys. 2022. doi:10.1051/0004-6361/202141979. arXiv:2106.15841

    work page doi:10.1051/0004-6361/202141979 2022

  58. [58]

    , keywords =

    Kroupa, Pavel. On the variation of the initial mass function. Mon. Not. R. Astron. Soc. 2001. doi:10.1046/j.1365-8711.2001.04022.x. arXiv:astro-ph/0009005

    work page doi:10.1046/j.1365-8711.2001.04022.x 2001

  59. [59]

    Binary interaction dominates the evolution of massive stars

    Sana, H. and de Mink, S. E. and de Koter, A. and Langer, N. and Evans, C. J. and Gieles, M. and Gosset, E. and Izzard, R. G. and Bouquin, J. -B. Le and Schneider, F. R. N. Binary interaction dominates the evolution of massive stars. Science. 2012. doi:10.1126/science.1223344. arXiv:1207.6397

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1223344 2012

  60. [60]

    Tidal Spin-up of Black Hole Progenitor Stars

    Ma, Linhao and Fuller, Jim. Tidal Spin-up of Black Hole Progenitor Stars. Astrophys. J. 2023. doi:10.3847/1538-4357/acdb74. arXiv:2305.08356

    work page doi:10.3847/1538-4357/acdb74 2023

  61. [61]

    Most Black Holes are Born Very Slowly Rotating

    Fuller, Jim and Ma, Linhao. Most Black Holes are Born Very Slowly Rotating. Astrophys. J. Lett. 2019. doi:10.3847/2041-8213/ab339b. arXiv:1907.03714

    work page doi:10.3847/2041-8213/ab339b 2019

  62. [62]

    Presupernova Evolution of Rotating Massive Stars I: Numerical Method and Evolution of the Internal Stellar Structure

    Heger, A. and Langer, N. and Woosley, S. E. Presupernova evolution of rotating massive stars. 1. Numerical method and evolution of the internal stellar structure. Astrophys. J. 2000. doi:10.1086/308158. arXiv:astro-ph/9904132

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308158 2000

  63. [63]

    Spruit, H. C. Differential rotation and magnetic fields in stellar interiors. Astron. Astrophys. 1999. arXiv:astro-ph/9907138

    Pith/arXiv arXiv 1999

  64. [64]

    Supernova Fallback as Origin of Neutron Star Spins and Spin-kick Alignment

    Janka, Hans-Thomas and Wongwathanarat, Annop and Kramer, Michael. Supernova Fallback as Origin of Neutron Star Spins and Spin-kick Alignment. Astrophys. J. 2022. doi:10.3847/1538-4357/ac403c. arXiv:2104.07493

    work page doi:10.3847/1538-4357/ac403c 2022

  65. [65]

    Inferences about supernova physics from gravitational-wave measurements: GW151226 spin misalignment as an indicator of strong black-hole natal kicks

    O'Shaughnessy, Richard and Gerosa, Davide and Wysocki, Daniel. Inferences about supernova physics from gravitational-wave measurements: GW151226 spin misalignment as an indicator of strong black-hole natal kicks. Phys. Rev. Lett. 2017. doi:10.1103/PhysRevLett.119.011101. arXiv:1704.03879

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.119.011101 2017

  66. [66]

    Spin-Orbit Misalignment in Close Binaries with Two Compact Objects

    Kalogera, Vassiliki. Spin orbit misalignment in close binaries with two compact objects. Astrophys. J. 2000. doi:10.1086/309400. arXiv:astro-ph/9911417

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/309400 2000

  67. [67]

    Revising the Spin and Kick Connection in Isolated Binary Black Holes

    Baibhav, Vishal and Kalogera, Vicky. Revising the Spin and Kick Connection in Isolated Binary Black Holes. 2024. arXiv:2412.03461

    arXiv 2024

  68. [68]

    GW150914: Spin based constraints on the merger time of the progenitor system

    Kushnir, Doron and Zaldarriaga, Matias and Kollmeier, Juna A. and Waldman, Roni. GW150914: Spin based constraints on the merger time of the progenitor system. Mon. Not. R. Astron. Soc. 2016. doi:10.1093/mnras/stw1684. arXiv:1605.03839

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1684 2016

  69. [69]

    An upper limit on the spins of merging binary black holes formed through isolated binary evolution

    Marchant, Pablo and Podsiadlowski, Philipp and Mandel, Ilya. An upper limit on the spins of merging binary black holes formed through isolated binary evolution. Astron. Astrophys. 2024. doi:10.1051/0004-6361/202348190. arXiv:2311.14041

    work page doi:10.1051/0004-6361/202348190 2024

  70. [70]

    uller, Bernhard , title =

    Mandel, Ilya and M\"uller, Bernhard , title = ". Mon. Not. R. Astron. Soc. 2020. doi:10.1093/mnras/staa3043. arXiv:2006.08360

    work page doi:10.1093/mnras/staa3043 2020

  71. [71]

    uller, Bernhard , title =

    Kapil, Veome and Mandel, Ilya and Berti, Emanuele and M\"uller, Bernhard , title = ". Mon. Not. R. Astron. Soc. 2023. doi:10.1093/mnras/stad019. arXiv:2209.09252

    work page doi:10.1093/mnras/stad019 2023

  72. [72]

    and Stevenson, Simon and Thrane, Eric

    Broekgaarden, Floor S. and Stevenson, Simon and Thrane, Eric. Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes. Astrophys. J. 2022. doi:10.3847/1538-4357/ac8879. arXiv:2205.01693

    work page doi:10.3847/1538-4357/ac8879 2022

  73. [73]

    Astrophys

    Double white dwarfs as progenitors of R Coronae Borealis stars and type I supernovae. Astrophys. J. , keywords =. doi:10.1086/161701 , adsurl =

    work page doi:10.1086/161701

  74. [74]

    Astrophys

    Common Envelope Evolution and Double Cores of Planetary Nebulae. Astrophys. J. , keywords =. doi:10.1086/168974 , adsurl =

    work page doi:10.1086/168974

  75. [75]

    On the Binding Energy Parameter $\lambda$ of Common Envelope Evolution

    Xu, Xiao-Jie and Li, Xiang-Dong. On the Binding Energy Parameter of Common Envelope Evolution. Astrophys. J. 2010. doi:10.1088/0004-637X/716/1/114. arXiv:1004.4957

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/716/1/114 2010

  76. [76]

    Chemically homogeneous evolution: a rapid population synthesis approach

    Riley, Jeff and Mandel, Ilya and Marchant, Pablo and Butler, Ellen and Nathaniel, Kaila and Neijssel, Coenraad and Shortt, Spencer and Vigna-Gomez, Alejandro. Chemically homogeneous evolution: a rapid population synthesis approach. Mon. Not. R. Astron. Soc. 2021. doi:10.1093/mnras/stab1291. arXiv:2010.00002

    work page doi:10.1093/mnras/stab1291 2021

  77. [77]

    de Mink, S. E. and Cantiello, M. and Langer, N. and Pols, O. R. Chemically homogeneous evolution in massive binaries. AIP Conf. Proc. 2010. doi:10.1063/1.3536387. arXiv:1010.2177

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1063/1.3536387 2010

  78. [78]

    Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries

    Mandel, Ilya and de Mink, Selma E. Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries. Mon. Not. R. Astron. Soc. 2016. doi:10.1093/mnras/stw379. arXiv:1601.00007

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw379 2016

  79. [79]

    Abbott, B. P. and others. GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs. Phys. Rev. X. 2019. doi:10.1103/PhysRevX.9.031040. arXiv:1811.12907

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevx.9.031040 2019

  80. [80]

    GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run

    Abbott, R. and others. GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run. Phys. Rev. X. 2021. doi:10.1103/PhysRevX.11.021053. arXiv:2010.14527

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevx.11.021053 2021

Showing first 80 references.