pith. sign in

arxiv: 2606.22927 · v1 · pith:EBIDM6LHnew · submitted 2026-06-22 · 🌌 astro-ph.SR

Influence of mass transfer stability on the formation of post-common-envelope binaries

Yanxu Shi , Hongwei Ge , Zhenwei Li , Diogo Belloni , Rizhong Zheng , Dengkai Jiang , Hailiang Chen , A. Santos-Garcia
show 4 more authors
Santiago Torres Gil Alberto Rebassa-Mansergas Xuefei Chen Zhanwen Han
This is my paper

Pith reviewed 2026-06-26 07:28 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords post-common-envelope binariesmass transfer stabilitycommon envelope evolutionbinary population synthesiswhite dwarf main sequence binariesmagnetic brakingbinary stellar evolution
0
0 comments X

The pith

Enhanced mass transfer stability reduces the predicted number of post-common-envelope binaries with solar-type companions.

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

Standard binary population synthesis overpredicts post-common-envelope binaries that contain solar-type main-sequence stars. This work updates the Binary Star Evolution code with a physically motivated stability criterion for mass transfer and a self-consistent envelope binding energy. The updated models show that greater stability during mass transfer acts as an extra filter that removes many potential systems with solar-type companions. Magnetic braking and observational selection effects contribute but do not suffice on their own. Inefficient common-envelope evolution with efficiency parameter 0.25 produces the closest match to the compiled sample of observed systems.

Core claim

The enhanced mass transfer stability is an additional mechanism responsible for the observed dearth of post-common-envelope binaries with solar-type main sequence companions; neither magnetic braking nor selection effects alone can fully account for this deficit, and a combination of all three processes is most likely required. Models with inefficient common envelope evolution (α_CE=0.25) provide the best overall match to the observed population.

What carries the argument

Physically motivated mass transfer stability criterion in the Binary Star Evolution code, which decides whether mass transfer remains stable or triggers common-envelope evolution and thereby filters the predicted population.

If this is right

  • The observed population is best reproduced only when mass transfer stability, magnetic braking, and selection effects operate together.
  • Low common-envelope efficiency (α_CE = 0.25) yields the closest agreement with the compiled white-dwarf plus main-sequence sample.
  • Systems with M-dwarf companions remain largely unaffected by the change in stability criterion.
  • Traditional polytropic stability criteria systematically overproduce solar-type post-common-envelope binaries.

Where Pith is reading between the lines

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

  • The same stability criterion could alter predicted rates for other common-envelope outcomes such as double white dwarfs or Type Ia supernova progenitors.
  • Detailed stellar-structure calculations could test whether the adopted stability boundary shifts with metallicity or rotation.
  • Future Gaia or LSST samples of post-common-envelope binaries with precise masses and periods offer a direct test of the combined three-mechanism explanation.

Load-bearing premise

The mass transfer stability criterion used in the code accurately reflects the conditions under which real stars avoid common-envelope evolution.

What would settle it

A volume-complete survey that finds a substantially higher fraction of post-common-envelope binaries with solar-type companions than the updated models predict would falsify the claim that stability provides the missing reduction.

Figures

Figures reproduced from arXiv: 2606.22927 by Alberto Rebassa-Mansergas, A. Santos-Garcia, Dengkai Jiang, Diogo Belloni, Hailiang Chen, Hongwei Ge, Rizhong Zheng, Santiago Torres Gil, Xuefei Chen, Yanxu Shi, Zhanwen Han, Zhenwei Li.

Figure 1
Figure 1. Figure 1: The effect of critical mass ratio and CE descrip￾tion on the binary evolution and the formation of WD+MS PCEBs. Over the past two decades, significant advances in our understanding of CE evolution have been made through observational surveys of PCEBs (M. Zorotovic et al. 2011; A. Nebot G´omez-Mor´an et al. 2011; S. Toonen & G. Nelemans 2013; J. Camacho et al. 2014; R. Cojo￾caru et al. 2017; N. Yamaguchi et… view at source ↗
Figure 2
Figure 2. Figure 2: Critical mass ratio adopted in our simulations, plotted on the stellar mass-radius diagram. Black and white dashed lines represent the radii of ZAMS stars and the minimum radii of RGB at different masses, respectively. Note that not all regions shown are physically valid, as the AGB boundary is not plotted here. white dwarfs. We therefore adopt corrected white dwarf masses for these affected systems in thi… view at source ↗
Figure 3
Figure 3. Figure 3: Initial primary versus initial secondary mass dis￾tribution of PCEB progenitors. Points are color-coded by the final WD type: red for He WDs, blue for carbon-oxygen (C/O) WDs, and green for oxygen-neon (O/Ne) WDs. Dark points in the foreground correspond to the Ge et al. qc pre￾scription (model a), and are overlaid on top of lighter points representing the polytropic qc prescription (model d). The grey das… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of observed (pink dots) and simulated PCEBs in the MWD − MMS plane. The point color encodes the local number density of simulated PCEBs, normalized independently to the maximum density in each panel for visual clarity. Peak-normalized marginal histograms are shown at the top (MWD) and right (MMS), where grey lines represent the observed distributions, red represents the simulated MWD distribut… view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of observed (pink dots) and simulated PCEBs in the MMS − Porb plane. The color intensity scale is identical to [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of observed (pink dots) and simulated PCEBs in the MWD − Porb plane. The color intensity scale is identical to Figures 4 and 5. tional torque are the largest convective cells; when the difference between Ω and Ωeq is too large, these cells can [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of observed (pink dots) and simulated PCEBs using the CARB MB prescription, plotted in the MWD − MMS, MMS − Porb, and MWD − Porb planes. The color scheme is identical to [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Our compiled PCEB sample and long-period WD+MS binaries from (E. Kruse & E. Agol 2014; H. Kawahara et al. 2018; N. Yamaguchi et al. 2024a) plotted in the MWD − Porb plane (adapted from N. Yamaguchi et al. 2024a and S. G. Parsons et al. 2023). The point color encodes the mass of the MS companion in each system. We mark the position of the well-known PCEB IK Peg for reference. The dashed line and grey region… view at source ↗
Figure 9
Figure 9. Figure 9: Distribution of observed (pink dots, classic PCEBs and long-period WD+MS binaries) and simulated PCEBs adopting half of internal energy contribution, plotted in the MWD − MMS, MMS − Porb, and MWD − Porb planes. The αCE is set to 0.25. The color scheme is identical to [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Distribution of observed (pink dots) and simu￾lated PCEBs in the MWD −MMS plane. We exclude systems discovered via UV excess from this plot, as they are sub￾ject to totally different selection effects. The color scheme is identical to [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
read the original abstract

Post-common-envelope binaries are the natural laboratories for constraining the physics of common envelope evolution, which is one of the most uncertain phases in binary stellar evolution. Traditional binary population synthesis models, adopting mass transfer stability criteria based on polytropic stellar models, systematically overpredict the number of post-common-envelope binaries with solar-type main-sequence companions. In this work, we present an updated binary population synthesis model using the rapid binary evolution code \textit{Binary Star Evolution}, incorporating a physically motivated mass transfer stability criterion and a self-consistent envelope binding energy prescription. We compile a comprehensive sample of classic white dwarf + main sequence post-common-envelope binaries with well-measured parameters, hosting both M-dwarf and A/F/G/K- stars. We find that the enhanced mass transfer stability is an additional mechanism responsible for the observed dearth of post-common-envelope binaries with solar-type main sequence companions; neither magnetic braking nor selection effects alone can fully account for this deficit, and a combination of all three processes is most likely required. Models with inefficient common envelope evolution ($\alpha_{\rm CE}=0.25$) provide the best overall match to the observed population. These results highlight the critical role of MT stability in shaping the observed post-common-envelope binaries population and provide new constraints on common envelope evolution.

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 / 1 minor

Summary. The paper claims that an updated BSE population synthesis model incorporating a physically motivated mass transfer stability criterion (replacing the polytropic one) and a self-consistent envelope binding energy prescription shows that enhanced MT stability is an additional mechanism (beyond magnetic braking and selection effects) responsible for the observed dearth of post-common-envelope binaries with solar-type main-sequence companions; models with α_CE=0.25 provide the best overall match to a compiled sample of WD+MS PCEBs.

Significance. If the new stability criterion is shown to be accurate, the work would strengthen the case that mass transfer stability shapes the PCEB population and provide useful constraints on common-envelope efficiency. The compilation of an observational sample with both M-dwarf and A/F/G/K companions is a positive contribution.

major comments (2)
  1. [Abstract and §2] Abstract and model description: the claim that the new criterion explains part of the dearth relies on the assumption that it correctly identifies the stable-MT/CE boundary for ~1 M⊙ donors, but the manuscript supplies no validation against detailed stellar models or hydrodynamical calculations; without this, the population synthesis result could be an artifact of the criterion rather than a physical explanation.
  2. [Results (comparison to observations)] Results section comparing models to the compiled sample: α_CE=0.25 is selected because it yields the best overall match; this makes the central assertion that the combination of the stability criterion plus this specific efficiency reproduces the data circular rather than an independent prediction.
minor comments (1)
  1. [Abstract] The abstract would benefit from including at least one quantitative metric (e.g., a goodness-of-fit value or ratio of predicted-to-observed numbers) rather than stating only that the model provides the 'best overall match'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. We address each major comment below. Revisions have been made to clarify the physical basis of the stability criterion, add discussion of its limitations, and distinguish the independent role of the new criterion from the choice of α_CE. These changes strengthen the manuscript without altering its core conclusions.

read point-by-point responses

  1. Referee: [Abstract and §2] Abstract and model description: the claim that the new criterion explains part of the dearth relies on the assumption that it correctly identifies the stable-MT/CE boundary for ~1 M⊙ donors, but the manuscript supplies no validation against detailed stellar models or hydrodynamical calculations; without this, the population synthesis result could be an artifact of the criterion rather than a physical explanation.

    Authors: We agree that direct validation against detailed stellar models or hydrodynamical simulations for the ~1 M⊙ regime is not presented in the current manuscript. The criterion is physically motivated by the response of the stellar structure to mass loss (as described in §2), but we acknowledge this leaves open the possibility of systematic bias. In the revised manuscript we have added a dedicated paragraph in §2 that (i) summarizes the derivation from the adiabatic response and (ii) cites existing comparisons in the literature between similar stability criteria and both 1D stellar models and limited hydrodynamical work. We also explicitly state the assumption and its uncertainty so that readers can assess the robustness of the population-synthesis results. revision: partial

  2. Referee: [Results (comparison to observations)] Results section comparing models to the compiled sample: α_CE=0.25 is selected because it yields the best overall match; this makes the central assertion that the combination of the stability criterion plus this specific efficiency reproduces the data circular rather than an independent prediction.

    Authors: The stability criterion itself is independent of α_CE; it is fixed by the donor response and is applied before any common-envelope phase is invoked. The main result—that enhanced stability reduces the predicted number of solar-type PCEBs—is present for all tested values of α_CE. We select α_CE=0.25 only as the value that simultaneously reproduces the observed period and mass-ratio distributions once the new stability boundary is adopted. In the revised text we have rephrased the abstract and §4 to emphasize that the stability effect operates across the α_CE range and that the low-efficiency value is a secondary constraint, not a prerequisite for the stability conclusion. This removes any appearance of circularity. revision: partial

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper implements an updated mass transfer stability criterion in the BSE code, compiles an observed PCEB sample, and compares population synthesis outputs for different α_CE values against that external sample. The statement that α_CE=0.25 provides the best match is the direct result of running the models and inspecting the match to data, not a self-referential definition or a fitted input relabeled as a prediction. The central claim that enhanced MT stability contributes to the observed dearth rests on the new criterion's effect on the synthesized population and is independent of the α_CE tuning step. No load-bearing derivation step reduces to its own inputs by construction; the work is a standard parameter study benchmarked against observations.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the accuracy of the new mass-transfer stability criterion (whose derivation is not shown), the assumption that the compiled observational sample is unbiased, and the choice of alpha_CE fitted to the same data used for validation.

free parameters (1)
  • alpha_CE = 0.25
    Value selected because models with alpha_CE=0.25 provide the best overall match to the observed PCEB population.
axioms (2)
  • domain assumption Polytropic stellar models yield inaccurate mass-transfer stability criteria for solar-type stars in binaries.
    Invoked to explain why traditional models overpredict the number of PCEBs with solar-type companions.
  • domain assumption The updated mass-transfer stability criterion implemented in BSE is physically motivated and more accurate than polytropic prescriptions.
    Central modeling choice whose validity is required for the conclusion that stability is an additional mechanism.

pith-pipeline@v0.9.1-grok · 5798 in / 1716 out tokens · 34701 ms · 2026-06-26T07:28:57.450333+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

85 extracted references · 24 linked inside Pith

  1. [1]

    Progress in Particle and Nuclear Physics , keywords =

    Binary stars in the new millennium. Progress in Particle and Nuclear Physics , keywords =. doi:10.1016/j.ppnp.2023.104083 , archivePrefix =. 2311.11454 , primaryClass =

    doi:10.1016/j.ppnp.2023.104083 2023

  2. [2]

    IX: Constraining the common-envelope efficiency

    Post-common-envelope binaries from SDSS. IX: Constraining the common-envelope efficiency. , keywords =. doi:10.1051/0004-6361/200913658 , archivePrefix =. 1006.1621 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/200913658

  3. [3]

    Post common envelope binaries from SDSS. XI. The white dwarf mass distributions of CVs and pre-CVs. , keywords =. doi:10.1051/0004-6361/201116626 , archivePrefix =. 1108.4600 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201116626

  4. [4]

    Post common envelope binaries from SDSS. XII. The orbital period distribution. , keywords =. doi:10.1051/0004-6361/201117514 , archivePrefix =. 1109.6662 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201117514

  5. [5]

    Post common envelope binaries from SDSS. VIII. Evidence for disrupted magnetic braking. , keywords =. doi:10.1051/0004-6361/201013990 , adsurl =

    doi:10.1051/0004-6361/201013990

  6. [6]

    , keywords =

    The Companion Mass Distribution of Post Common Envelope Hot Subdwarf Binaries: Evidence for Boosted and Disrupted Magnetic Braking?. , keywords =. doi:10.1088/1538-3873/ad94a2 , archivePrefix =. 2408.15334 , primaryClass =

    doi:10.1088/1538-3873/ad94a2

  7. [7]

    , keywords =

    Evidence for saturated and disrupted magnetic braking from samples of detached close binaries with M and K dwarfs. , keywords =. doi:10.1051/0004-6361/202347931 , archivePrefix =. 2311.04309 , primaryClass =

    doi:10.1051/0004-6361/202347931

  8. [8]

    Thresholds for Rapid Mass Transfer in Binary System. I. Polytropic Models. , keywords =. doi:10.1086/165412 , adsurl =

    doi:10.1086/165412

  9. [9]

    , keywords =

    Evolution of binary stars and the effect of tides on binary populations. , keywords =. doi:10.1046/j.1365-8711.2002.05038.x , archivePrefix =. astro-ph/0201220 , primaryClass =

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

  10. [10]

    , keywords =

    A comprehensive population synthesis study of post-common envelope binaries. , keywords =. doi:10.1111/j.1365-2966.2009.16138.x , archivePrefix =. 0903.4152 , primaryClass =

    doi:10.1111/j.1365-2966.2009.16138.x 2009

  11. [11]

    , keywords =

    The effect of common-envelope evolution on the visible population of post-common-envelope binaries. , keywords =. doi:10.1051/0004-6361/201321753 , archivePrefix =. 1309.0327 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321753

  12. [12]

    , keywords =

    Monte Carlo simulations of post-common-envelope white dwarf + main sequence binaries: The effects of including recombination energy. , keywords =. doi:10.1051/0004-6361/201323039 , archivePrefix =. 1407.3301 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201323039

  13. [13]

    , keywords =

    Monte Carlo Population Synthesis of Post-common-envelope White Dwarf Binaries and Type Ia supernova Rate. , keywords =. doi:10.3847/0004-637X/826/1/53 , archivePrefix =. 1605.03646 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/0004-637x/826/1/53

  14. [14]

    Three close white dwarf binaries with G-type secondary stars

    The White Dwarf Binary Pathways Survey - IV. Three close white dwarf binaries with G-type secondary stars. , keywords =. doi:10.1093/mnras/staa3815 , archivePrefix =. 2012.04683 , primaryClass =

    doi:10.1093/mnras/staa3815 2012

  15. [15]

    Two close post-common envelope binaries with TESS light curves

    The white dwarf binary pathways survey - VI. Two close post-common envelope binaries with TESS light curves. , keywords =. doi:10.1093/mnras/stac604 , archivePrefix =. 2203.01745 , primaryClass =

    doi:10.1093/mnras/stac604

  16. [16]

    A post-common envelope binary with a massive white dwarf and an active G-type secondary star

    The white dwarf binary pathways survey - VIII. A post-common envelope binary with a massive white dwarf and an active G-type secondary star. , keywords =. doi:10.1093/mnras/stac2837 , archivePrefix =. 2209.15591 , primaryClass =

    doi:10.1093/mnras/stac2837

  17. [17]

    , keywords =

    Wide post-common envelope binaries containing ultramassive white dwarfs: evidence for efficient envelope ejection in massive asymptotic giant branch stars. , keywords =. doi:10.1093/mnras/stad4005 , archivePrefix =. 2309.15905 , primaryClass =

    doi:10.1093/mnras/stad4005

  18. [18]

    , keywords =

    Wide Post-common Envelope Binaries from Gaia: Orbit Validation and Formation Models. , keywords =. doi:10.1088/1538-3873/ad6809 , archivePrefix =. 2405.06020 , primaryClass =

    doi:10.1088/1538-3873/ad6809

  19. [19]

    , keywords =

    A Not-so-compact Companion: Massive, Oversized White Dwarf in a Post-common-envelope Eclipsing Binary. , keywords =. doi:10.3847/1538-3881/ae3b42 , archivePrefix =. 2601.14378 , primaryClass =

    doi:10.3847/1538-3881/ae3b42

  20. [20]

    Formation of long-period post-common envelope binaries. I. No extra energy is needed to explain oxygen-neon white dwarfs paired with AFGK-type main-sequence stars. , keywords =. doi:10.1051/0004-6361/202449235 , archivePrefix =. 2401.07692 , primaryClass =

    doi:10.1051/0004-6361/202449235

  21. [21]

    Formation of long-period post-common-envelope binaries. II. Explaining the self-lensing binary KOI 3278. , keywords =. doi:10.1051/0004-6361/202449320 , archivePrefix =. 2401.17510 , primaryClass =

    doi:10.1051/0004-6361/202449320

  22. [22]

    Adiabatic Mass Loss in Binary Stars. I. Computational Method. , keywords =. doi:10.1088/0004-637X/717/2/724 , archivePrefix =. 1005.3099 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/717/2/724

  23. [23]

    Adiabatic Mass Loss in Binary Stars. II. From Zero-age Main Sequence to the Base of the Giant Branch. , keywords =. doi:10.1088/0004-637X/812/1/40 , archivePrefix =. 1507.04843 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/812/1/40

  24. [24]

    Adiabatic Mass Loss in Binary Stars. III. From the Base of the Red Giant Branch to the Tip of the Asymptotic Giant Branch. , keywords =. doi:10.3847/1538-4357/aba7b7 , archivePrefix =. 2007.09848 , primaryClass =

    doi:10.3847/1538-4357/aba7b7 2007

  25. [25]

    , keywords =

    Criteria for Dynamical Timescale Mass Transfer of Metal-poor Intermediate-mass Stars. , keywords =. doi:10.3847/1538-4357/acb7e9 , archivePrefix =. 2302.00183 , primaryClass =

    doi:10.3847/1538-4357/acb7e9

  26. [26]

    , keywords =

    On the Binding Energy Parameter of Common Envelope Evolution. , keywords =. doi:10.1088/0004-637X/716/1/114 , archivePrefix =. 1004.4957 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/716/1/114

  27. [27]

    , year = 2010, month = oct, volume =

    ERRATUM: ``On the Binding Energy Parameter of Common Envelope Evolution'' <A href=``/abs/2010ApJ...716..114X''>(2010, ApJ, 716, 114)</A>. , year = 2010, month = oct, volume =. doi:10.1088/0004-637X/722/2/1985 , adsurl =

    doi:10.1088/0004-637x/722/2/1985 2010

  28. [28]

    , keywords =

    Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. , keywords =. doi:10.1046/j.1365-8711.2000.03426.x , archivePrefix =. astro-ph/0001295 , primaryClass =

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

  29. [29]

    , keywords =

    The Initial Mass Function and Stellar Birthrate in the Solar Neighborhood. , keywords =. doi:10.1086/190629 , adsurl =

    doi:10.1086/190629

  30. [30]

    , keywords =

    The Distribution of Visual Binaries with Two Bright Components. , keywords =. doi:10.1086/168190 , adsurl =

    doi:10.1086/168190

  31. [31]

    Research in Astronomy and Astrophysics , keywords =

    Binary Population Synthesis. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/20/10/161 , archivePrefix =. 2009.08611 , primaryClass =

    doi:10.1088/1674-4527/20/10/161 2009

  32. [32]

    , keywords =

    Origin of apparent period variations in eclipsing post-common-envelope binaries. , keywords =. doi:10.1051/0004-6361/201220321 , archivePrefix =. 1211.5356 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201220321

  33. [33]

    , keywords =

    How many cataclysmic variables are crossing the period gap? A test for the disruption of magnetic braking. , keywords =. doi:10.1111/j.1365-2966.2008.13675.x , archivePrefix =. 0805.4700 , primaryClass =

    doi:10.1111/j.1365-2966.2008.13675.x 2008

  34. [34]

    , keywords =

    The Thermal Equilibrium Mass-loss Model and Its Applications in Binary Evolution. , keywords =. doi:10.3847/1538-4365/ab98f6 , archivePrefix =. 2006.00774 , primaryClass =

    doi:10.3847/1538-4365/ab98f6 2006

  35. [35]

    , keywords =

    Influence of a mass transfer stability criterion on double white dwarf populations. , keywords =. doi:10.1051/0004-6361/202243893 , archivePrefix =. 2211.01861 , primaryClass =

    doi:10.1051/0004-6361/202243893

  36. [36]

    , keywords =

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

    doi:10.1086/161701

  37. [37]

    , keywords =

    The Common Envelope Phase in the Evolution of Binary Stars. , keywords =. doi:10.1086/166419 , adsurl =

    doi:10.1086/166419

  38. [38]

    , keywords =

    The Common Envelope Evolution Outcome-A Case Study on Hot Subdwarf B Stars. , keywords =. doi:10.3847/1538-4357/ac75d3 , archivePrefix =. 2205.14256 , primaryClass =

    doi:10.3847/1538-4357/ac75d3

  39. [39]

    The Common Envelope Evolution Outcome. II. Short-orbital-period Hot Subdwarf B Binaries Reveal a Clear Picture. , keywords =. doi:10.3847/1538-4357/ad158e , archivePrefix =. 2311.17304 , primaryClass =

    doi:10.3847/1538-4357/ad158e

  40. [40]

    , keywords =

    Rapid Stellar and Binary Population Synthesis with COMPAS. , keywords =. doi:10.3847/1538-4365/ac416c , archivePrefix =. 2109.10352 , primaryClass =

    doi:10.3847/1538-4365/ac416c

  41. [41]

    Three long period white dwarf plus subgiant binaries

    The white dwarf binary pathways survey - IX. Three long period white dwarf plus subgiant binaries. , keywords =. doi:10.1093/mnras/stac3368 , archivePrefix =. 2211.08440 , primaryClass =

    doi:10.1093/mnras/stac3368

  42. [42]

    , keywords =

    The relation between white dwarf mass and orbital period in wide binary radio pulsars. , keywords =. doi:10.1093/mnras/273.3.731 , adsurl =

    doi:10.1093/mnras/273.3.731

  43. [43]

    , keywords =

    Photometric follow-up of 43 new eclipsing white dwarf plus main-sequence binaries from the ZTF survey. , keywords =. doi:10.1093/mnras/stad612 , archivePrefix =. 2302.11392 , primaryClass =

    doi:10.1093/mnras/stad612

  44. [44]

    Long orbital period systems and the energy budget of common envelope evolution

    Post-common envelope binaries from SDSS - XVI. Long orbital period systems and the energy budget of common envelope evolution. , keywords =. doi:10.1111/j.1365-2966.2012.20880.x , archivePrefix =. 1203.1208 , primaryClass =

    doi:10.1111/j.1365-2966.2012.20880.x 2012

  45. [45]

    , keywords =

    A Catalog of Potential Post-Common Envelope Binaries. , keywords =. doi:10.3847/1538-4357/ac13ac , archivePrefix =. 2107.05221 , primaryClass =

    doi:10.3847/1538-4357/ac13ac

  46. [46]

    , keywords =

    A post-common-envelope binary with double-peaked Balmer emission lines from TMTS. , keywords =. doi:10.1051/0004-6361/202553732 , archivePrefix =. 2504.18202 , primaryClass =

    doi:10.1051/0004-6361/202553732

  47. [47]

    Four eclipsing white dwarf main-sequence binaries

    Post-common-envelope binaries from SDSS - V. Four eclipsing white dwarf main-sequence binaries. , keywords =. doi:10.1111/j.1365-2966.2008.14378.x , archivePrefix =. 0812.2510 , primaryClass =

    doi:10.1111/j.1365-2966.2008.14378.x 2008

  48. [48]

    , keywords =

    Two dynamically discovered compact object candidate binary systems from LAMOST low-resolution survey. , keywords =. doi:10.1093/mnras/stae1590 , archivePrefix =. 2406.17340 , primaryClass =

    doi:10.1093/mnras/stae1590

  49. [49]

    , keywords =

    Discovery of a pre-cataclysmic binary with unusual chromaticity of the eclipsed white dwarf by the GPX survey. , keywords =. doi:10.1093/mnras/staa547 , archivePrefix =. 2002.08031 , primaryClass =

    doi:10.1093/mnras/staa547 2002

  50. [50]

    , keywords =

    LAMOST J101356.33+272410.7: A Detached White Dwarf─Main-sequence Binary with a Massive White Dwarf within the Period Gap. , keywords =. doi:10.3847/1538-4357/adc0fa , archivePrefix =. 2501.01171 , primaryClass =

    doi:10.3847/1538-4357/adc0fa

  51. [51]

    , keywords =

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

    doi:10.1093/pasj/psaf148

  52. [52]

    , keywords =

    Discovery of Three Self-lensing Binaries from Kepler. , keywords =. doi:10.3847/1538-3881/aaaaaf , archivePrefix =. 1801.07874 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-3881/aaaaaf

  53. [53]

    , keywords =

    A new technique for calculations of binary stellar evolution application to magnetic braking. , keywords =. doi:10.1086/161569 , adsurl =

    doi:10.1086/161569

  54. [54]

    , keywords =

    Evolved cataclysmic variables as progenitors of AM CVn stars. , keywords =. doi:10.1093/mnras/stad354 , archivePrefix =. 2301.12992 , primaryClass =

    doi:10.1093/mnras/stad354

  55. [55]

    , keywords =

    Reversing the verdict: Cataclysmic variables could be the dominant progenitors of AM CVn binaries after all. , keywords =. doi:10.1051/0004-6361/202347047 , archivePrefix =. 2305.19312 , primaryClass =

    doi:10.1051/0004-6361/202347047

  56. [56]

    , keywords =

    Revisiting the extremely long-period cataclysmic variables V479 Andromedae and V1082 Sagittarii. , keywords =. doi:10.1051/0004-6361/202556385 , archivePrefix =. 2508.21358 , primaryClass =

    doi:10.1051/0004-6361/202556385

  57. [57]

    , keywords =

    Evolving LMXBs: CARB Magnetic Braking. , keywords =. doi:10.3847/2041-8213/ab571c , archivePrefix =. 1911.05790 , primaryClass =

    doi:10.3847/2041-8213/ab571c 2041

  58. [58]

    , keywords =

    On Convective Turnover Times and Dynamos in Low-mass Stars. , keywords =. doi:10.3847/1538-4357/adde4d , archivePrefix =. 2410.20000 , primaryClass =

    doi:10.3847/1538-4357/adde4d

  59. [59]

    , keywords =

    Rotation Period Evolution in Low-mass Binary Stars: The Impact of Tidal Torques and Magnetic Braking. , keywords =. doi:10.3847/1538-4357/ab2ed2 , archivePrefix =. 1903.05686 , primaryClass =

    doi:10.3847/1538-4357/ab2ed2 1903

  60. [60]

    , keywords =

    Stellar Spin-down in Post-mass-transfer Binary Systems. , keywords =. doi:10.3847/1538-4357/ad54be , archivePrefix =. 2403.17279 , primaryClass =

    doi:10.3847/1538-4357/ad54be

  61. [61]

    Research in Astronomy and Astrophysics , keywords =

    The binding energy parameter for common envelope evolution. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/16/8/126 , archivePrefix =. 1605.03668 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/1674-4527/16/8/126

  62. [62]

    , keywords =

    A population synthesis study of the Gaia 100 pc unresolved white dwarf-main-sequence binary population. , keywords =. doi:10.1051/0004-6361/202452989 , archivePrefix =. 2502.11593 , primaryClass =

    doi:10.1051/0004-6361/202452989

  63. [63]

    The DR7 white dwarf-main-sequence binary catalogue

    Post-common envelope binaries from SDSS - XIV. The DR7 white dwarf-main-sequence binary catalogue. , keywords =. doi:10.1111/j.1365-2966.2011.19923.x , archivePrefix =. 1110.1000 , primaryClass =

    doi:10.1111/j.1365-2966.2011.19923.x 2011

  64. [64]

    Triage of the Gaia DR3 astrometric orbits. II. A census of white dwarfs. , keywords =. doi:10.1093/mnras/stae773 , archivePrefix =. 2309.15143 , primaryClass =

    doi:10.1093/mnras/stae773

  65. [65]

    , keywords =

    Stellar Multiplicity. , keywords =. doi:10.1146/annurev-astro-081710-102602 , archivePrefix =. 1303.3028 , primaryClass =

    Pith/arXiv arXiv doi:10.1146/annurev-astro-081710-102602

  66. [66]

    , keywords =

    Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars. , keywords =. doi:10.3847/1538-4365/aa6fb6 , archivePrefix =. 1606.05347 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4365/aa6fb6

  67. [67]

    Structure and Evolution of Close Binary Systems , year = 1976, editor =

    Common Envelope Binaries. Structure and Evolution of Close Binary Systems , year = 1976, editor =

    1976

  68. [68]

    , keywords =

    Common envelope evolution: where we stand and how we can move forward. , keywords =. doi:10.1007/s00159-013-0059-2 , archivePrefix =. 1209.4302 , primaryClass =

    Pith/arXiv arXiv doi:10.1007/s00159-013-0059-2

  69. [69]

    , keywords =

    A Global View of Post-interaction White Dwarf-main Sequence Binaries. , keywords =. doi:10.1088/1538-3873/ae453b , archivePrefix =. 2601.00439 , primaryClass =

    doi:10.1088/1538-3873/ae453b

  70. [70]

    , keywords =

    Tidal evolution in close binary systems. , keywords =

  71. [71]

    , keywords =

    Monte Carlo simulations of post-common-envelope white dwarf + main sequence binaries: comparison with the SDSS DR7 observed sample. , keywords =. doi:10.1051/0004-6361/201323052 , archivePrefix =. 1404.5464 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201323052

  72. [72]

    , keywords =

    The population of white dwarf-main sequence binaries in the SDSS DR 12. , keywords =. doi:10.1093/mnras/stx1326 , archivePrefix =. 1705.05888 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx1326

  73. [73]

    , keywords =

    Reconstructing post-common envelope white dwarf─main-sequence binary histories through inverse population synthesis techniques: A case study of ZTF eclipsing binaries. , keywords =. doi:10.1051/0004-6361/202554039 , archivePrefix =. 2505.01505 , primaryClass =

    doi:10.1051/0004-6361/202554039

  74. [74]

    , keywords =

    The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9-12. , keywords =. doi:10.1093/mnras/stw554 , archivePrefix =. 1603.01017 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw554

  75. [75]

    A sample of FGK stars with white dwarf companions

    The white dwarf binary pathways survey - I. A sample of FGK stars with white dwarf companions. , keywords =. doi:10.1093/mnras/stw2143 , archivePrefix =. 1604.01613 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw2143

  76. [76]

    Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

    The white dwarf binary pathways survey - II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4. , keywords =. doi:10.1093/mnras/stx2259 , archivePrefix =. 1708.09480 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx2259

  77. [77]

    The White Dwarf Binary Pathways Survey. V. The Gaia White Dwarf Plus AFGK Binary Sample and the Identification of 23 Close Binaries. , keywords =. doi:10.3847/1538-4357/abc017 , archivePrefix =. 2010.02885 , primaryClass =

    doi:10.3847/1538-4357/abc017 2010

  78. [78]

    , keywords =

    Searching for GEMS: Discovery of the Nearby Post-common-envelope Binary System TIC-460388167. , keywords =. doi:10.3847/1538-4357/ae6246 , archivePrefix =. 2604.07527 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ae6246

  79. [79]

    , keywords =

    Characterization of the eclipsing post-common-envelope binary TIC 60040774. , keywords =. doi:10.1093/mnras/stac2197 , archivePrefix =. 2208.02986 , primaryClass =

    doi:10.1093/mnras/stac2197

  80. [80]

    , year = 1994, month = sep, volume =

    A possible criterion for envelope ejection in asymptotic giant branch or first giant branch stars. , year = 1994, month = sep, volume =. doi:10.1093/mnras/270.1.121 , adsurl =

    doi:10.1093/mnras/270.1.121 1994

Showing first 80 references.