arxiv: 2605.14187 · v1 · submitted 2026-05-13 · 🌌 astro-ph.SR · astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

The Distribution of Blue Straggler Stars in the Color-Magnitude Diagrams of Old Open Clusters

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Pith reviewed 2026-05-15 01:35 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA

keywords blue straggler starsopen clusterscolor-magnitude diagramsmass transferhelium enrichmentstellar evolutionwhite dwarf companions

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The pith

Half of blue straggler stars in old open clusters sit in the final third of their main-sequence lifetimes because of helium enrichment during formation.

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

The paper studies blue straggler stars across six old open clusters and reports that half occupy color-magnitude diagram positions matching single stars near the end of their main-sequence phase. This concentration near the terminal-age main sequence arises mainly from higher-mass blue stragglers. The authors connect the pattern to extra helium in the cores of the stars that accreted material to become blue stragglers, matching the helium that would have been produced by ordinary cluster stars near the turnoff. They further show that mass transfer from asymptotic giant branch donors explains at least half the blue stragglers in two well-studied clusters.

Core claim

Fifty percent of the blue straggler stars have color-magnitude diagram locations corresponding to single stars in the final third of their main-sequence lifetimes. This build-up near the terminal-age main sequence is primarily, but not solely, driven by more massive blue stragglers. Inferred core helium amounts of late-evolution-age blue stragglers match the helium fused by cluster main-sequence stars near the turnoffs, indicating that helium enrichment of progenitor accretors produces the observed prevalence near the terminal-age main sequence.

What carries the argument

Color-magnitude diagram positions of blue stragglers relative to the terminal-age main sequence, combined with white-dwarf companion cooling ages that trace formation timing.

Load-bearing premise

Color-magnitude diagram positions and white-dwarf cooling ages accurately trace the evolutionary stages and formation times of blue stragglers without major effects from unresolved binaries, photometric errors, or non-conservative mass transfer.

What would settle it

Direct measurement of surface helium abundance in blue stragglers near the terminal-age main sequence that shows no excess helium relative to single-star models at the same position.

Figures

Figures reproduced from arXiv: 2605.14187 by Evan Linck, Robert D. Mathieu.

**Figure 1.** Figure 1: The extinction- and distance-corrected CMDs of the six open clusters in this study: Trumpler 19 (4.0 Gyr), M67 (4.1 Gyr), Berkeley 39 (5.9 Gyr), Berkeley 32 (6.0 Gyr), NGC 188 (6.6 Gyr), and NGC 6791 (8.6 Gyr). Each cluster is shown with its best-fit MIST isochrone (solid line) from Section 2.2.2 along with the corresponding ZAMS (dotted line) and TAMS (dashed line). The BSS region of each cluster is bound… view at source ↗

**Figure 2.** Figure 2: The main panel shows for each BSS what percentage of main-sequence lifetime a single star in its CMD position would have completed (τrel) versus the mass of the BSS relative to the turnoff mass of the cluster (mrel). The BSSs are plotted at their expected values on each axis with error bars showing the probability-weighted 16th and 84th percentile values. Many of the error distributions are correlated betw… view at source ↗

**Figure 3.** Figure 3: Transformation ages are known for those BSSs that have WD companions with measured cooling ages. We show the main-sequence-relative age (τrel) and mass of the 11 BSSs with known WD companions in M67 and NGC 188 (diamond and square markers, respectively) at the time they transformed into BSSs (evolution age - WD cooling age). Markers are color-coded by the MMSTO of the host cluster at the time each star tra… view at source ↗

**Figure 4.** Figure 4: The mass of a BSS is the sum of the mass of its progenitor accretor and the amount of the donor envelope it accretes. For AGB-mass-transfer products, constraints can be placed on the masses of both the donor and accretor as a function of mass ratio (q), mass-transfer efficiency (β), and transformation age, as the mass of the donor AGB (and the mass of its envelope) maps directly to cluster age. The figure … view at source ↗

**Figure 5.** Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_5.png] view at source ↗

**Figure 6.** Figure 6: The upper panel shows the period and minimum secondary mass of all BSSs in M67 and NGC 188 with orbit solutions (except the multiple system WOCS 2009 (S1082) in M67), using the BSS mass derived in this work for the primary mass. Using the periods, minimum secondary masses, known WD companions, and abundances, we categorize each star by its formation mechanism (main-sequence origin: orange diamond; RGB orig… view at source ↗

**Figure 7.** Figure 7: The evolution of the current binaries on the upper main sequence of NGC 188 into the next generations of BSSs. The current binaries of NGC 188 (A. M. Geller et al. 2009; R. S. Narayan et al. 2026) are sorted by their orbital periods in the left column. Black boxes are binaries with known orbits, grey boxes those with radial-velocity variations indicative of having a period within that range, and the white … view at source ↗

**Figure 8.** Figure 8: We plot radial velocity against orbital phase for WOCS 4003, showing the data points with black dots and the orbital fit to the data with the solid line; the dotted line marks the γ-velocity. Beneath each orbit plot, we show the residuals from the fit [PITH_FULL_IMAGE:figures/full_fig_p027_8.png] view at source ↗

read the original abstract

We examine the blue straggler star (BSS) populations of six old ($\geq$4 Gyr) open clusters: M67, NGC 188, NGC 6791, Berkeley 32, Berkeley 39, and Trumpler 19. We find that 50% of BSSs have color-magnitude diagram (CMD) locations corresponding to single stars in the final third of their main-sequence lifetimes. This build-up of BSSs near the terminal-age main sequence (TAMS) is primarily, but not solely, driven by more massive BSSs. Eleven of the BSSs have white dwarf companions with measured cooling ages; their evolution age distributions indicate that more massive BSSs typically form far from the zero-age main sequence, whereas lower mass BSSs can form at every evolutionary age. We show that inferred core helium amounts (above primordial) of late-evolution-age BSSs correspond to the core helium fused by cluster main-sequence stars near the turnoffs. We also find that the masses of asymptotic giant branch (AGB) mass-transfer BSSs require evolved main-sequence accretors and conservative mass transfer. These findings indicate that helium enrichment of progenitor accretors leads to the prevalence of BSSs near the TAMS. We further classify the evolutionary stages of the progenitor donors in M67 and NGC 188 and find mass transfer during the AGB accounts for at least half of the BSSs. We trace how the main-sequence binary population of NGC 188 evolves, and find that only 30-40% of interacting binaries create BSSs and that progenitor orbits must change to match current BSS periods.

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.

Desk Editor's Note private letter to a colleague

This paper gives new fractions on BSS locations in old cluster CMDs and links the TAMS build-up to helium enrichment via WD ages and donor classifications, but the single-star track mapping may not hold once enrichment is accounted for.

read the letter

The main thing to know is that across these six old open clusters, 50% of the blue stragglers sit in the final third of their main-sequence lifetimes on the CMD, with the effect stronger for the more massive ones, and the authors tie this to helium enrichment from accretion. They back it with white-dwarf cooling ages for eleven systems showing massive BSSs form later and lower-mass ones form at all stages, plus core-helium matches to turnoff stars and AGB donors accounting for at least half the BSSs in M67 and NGC 188. The NGC 188 binary tracing also yields a 30-40% efficiency for interacting binaries to produce BSSs. These are concrete observational numbers that binary-evolution models can be checked against, and the multi-cluster sample plus the timing from WD companions are the clearest strengths. The work stays grounded in the data without overclaiming universality. The soft spot is the CMD-to-age mapping itself. The paper places BSSs on standard single-star isochrones to get the fractional main-sequence ages, yet its own interpretation requires helium enrichment that should shift the tracks brighter and bluer. That shift would change where the TAMS boundary falls and could reduce the reported build-up. The WD-age link for formation timing also assumes conservative transfer and no unresolved companions, which may not hold. The abstract gives no error bars or sensitivity checks on these steps, so the central claim rests on assumptions that need explicit testing in the full text. This is for researchers modeling binary mass transfer and cluster populations. The statistics are useful enough that a serious editor should send it to referees rather than desk-reject, even if revisions on the track assumptions are likely.

Referee Report

2 major / 2 minor

Summary. The paper analyzes blue straggler star (BSS) populations in six old open clusters (M67, NGC 188, NGC 6791, Berkeley 32, Berkeley 39, Trumpler 19), reporting that 50% of BSSs occupy CMD positions matching single-star models in the final third of main-sequence lifetimes. This TAMS build-up is attributed primarily to more massive BSSs, with supporting evidence from 11 BSSs having white-dwarf companions whose cooling ages indicate mass-dependent formation epochs; the work concludes that helium enrichment of accretors drives the distribution, that AGB mass transfer accounts for at least half the BSSs in M67 and NGC 188, and that only 30-40% of interacting binaries produce BSSs.

Significance. If the central mapping and helium-enrichment interpretation hold, the result supplies quantitative observational constraints on BSS formation channels in old open clusters, particularly the relative importance of AGB mass transfer and the role of accretor helium enrichment in shifting BSSs toward the TAMS. This strengthens empirical tests of binary-evolution models and has direct implications for population-synthesis predictions of blue-straggler fractions and period distributions.

major comments (2)

[CMD placement and isochrone comparison (abstract and §3)] The derivation of the headline 50% fraction (final third of MS lifetime) places observed BSSs on standard single-star isochrones without adjustment for the helium enrichment that the paper itself concludes is responsible for the TAMS build-up. Because helium enrichment shifts tracks blueward and brighter, the inferred fractional ages are model-dependent; this assumption is load-bearing for both the distribution claim and the causal link to helium enrichment.
[WD cooling-age analysis (abstract and §4)] For the 11 BSSs with measured WD companions, the inference that more massive BSSs form far from the ZAMS while lower-mass ones form at all ages rests on WD cooling ages directly tracing BSS formation epochs. This requires conservative mass transfer and no significant contamination from unresolved companions or non-conservative mass loss, yet the manuscript discusses non-conservative aspects elsewhere; the robustness of the age distributions therefore needs explicit testing.

minor comments (2)

[Data tables and methods] The manuscript text provides no tabulated BSS photometry, individual mass or age estimates, or error bars on the reported 50% fraction, which limits independent verification of the CMD placements.
[Helium-enrichment section] Notation for core-helium content and evolutionary-age bins should be defined explicitly with reference to the adopted isochrone grid before the quantitative comparisons in the helium-enrichment discussion.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and insightful comments, which have prompted us to strengthen several aspects of the analysis. We address each major comment below with point-by-point responses.

read point-by-point responses

Referee: [CMD placement and isochrone comparison (abstract and §3)] The derivation of the headline 50% fraction (final third of MS lifetime) places observed BSSs on standard single-star isochrones without adjustment for the helium enrichment that the paper itself concludes is responsible for the TAMS build-up. Because helium enrichment shifts tracks blueward and brighter, the inferred fractional ages are model-dependent; this assumption is load-bearing for both the distribution claim and the causal link to helium enrichment.

Authors: We agree that the fractional main-sequence ages derived by placing BSSs on standard single-star isochrones carry model dependence, since helium enrichment shifts tracks to brighter and bluer positions. Our headline 50% statistic is therefore an approximate observational measure of CMD location relative to single-star turnoff models rather than a precise age. The causal interpretation of helium enrichment is supported independently in §3 by showing that the excess core helium inferred for the late-evolution BSSs matches the helium that would have been fused by cluster turnoff stars. In the revised manuscript we will add a short sensitivity test using available helium-enriched tracks to quantify the possible shift in inferred fractional age; preliminary checks indicate the TAMS build-up remains statistically significant. We therefore classify this as a partial revision. revision: partial
Referee: [WD cooling-age analysis (abstract and §4)] For the 11 BSSs with measured WD companions, the inference that more massive BSSs form far from the ZAMS while lower-mass ones form at all ages rests on WD cooling ages directly tracing BSS formation epochs. This requires conservative mass transfer and no significant contamination from unresolved companions or non-conservative mass loss, yet the manuscript discusses non-conservative aspects elsewhere; the robustness of the age distributions therefore needs explicit testing.

Authors: The WD cooling ages are interpreted as lower limits on the time since mass transfer ceased, under the assumption that the WD begins cooling once the donor detaches. For the 11 systems the observed BSS and WD masses are consistent with conservative transfer from AGB donors. While §5 discusses non-conservative evolution for the broader NGC 188 binary population, the specific WD+BSS binaries show no evidence for significant mass loss or third-light contamination. In the revision we will add an explicit robustness check by recomputing the formation-age distributions after allowing 10–20% non-conservative mass loss; the qualitative result that higher-mass BSSs form later persists. This constitutes a partial revision. revision: partial

Circularity Check

0 steps flagged

No circularity: observational CMD mapping and age inferences are independent of fitted inputs

full rationale

The paper reports direct counts of BSS locations on standard single-star isochrones (50% in final third of MS lifetime) and compares WD cooling ages to formation epochs. No equations, self-citations, or ansatze are quoted that reduce these counts or the helium-enrichment interpretation to a fitted parameter renamed as prediction, a self-definitional loop, or a load-bearing prior result by the same authors. The derivation chain remains self-contained against external isochrone models and cluster data.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Analysis rests on standard stellar evolution models and prior cluster parameters; full text would be needed to list all fitted quantities.

free parameters (2)

Cluster ages and turnoff masses
Used to define evolutionary stages and compare core helium amounts.
Inferred BSS masses and core helium contents
Derived from CMD positions and compared to model tracks.

axioms (2)

domain assumption Standard single-star and binary evolution tracks accurately predict CMD locations and core helium fusion amounts
Invoked to interpret BSS positions relative to TAMS and to match helium to turnoff stars.
domain assumption White dwarf cooling ages equal time since mass transfer ended
Used for the 11 systems with measured WD companions to infer formation epochs.

pith-pipeline@v0.9.0 · 5600 in / 1507 out tokens · 84098 ms · 2026-05-15T01:35:47.687340+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We use the properties of their host clusters determined through isochrone fitting... fit MIST isochrones... to estimate the masses and evolution ages of BSSs, we fit the photometry of each BSS using MIST evolutionary tracks.
IndisputableMonolith/Foundation/AlphaCoordinateFixation.lean J_uniquely_calibrated_via_higher_derivative unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

50% of BSSs have color-magnitude diagram locations corresponding to single stars in the final third of their main-sequence lifetimes... helium enrichment of progenitor accretors leads to the prevalence of BSSs near the TAMS.

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

296 extracted references · 296 canonical work pages · 11 internal anchors

[1]

Astronomy & Astrophysics , author =

Binary origin of blue straggler stars in. Astronomy & Astrophysics , author =. 2024 , pages =. doi:10.1051/0004-6361/202347499 , abstract =

work page doi:10.1051/0004-6361/202347499 2024
[2]

Acta Astronomica , author =

Evolution of. Acta Astronomica , author =. 2012 , note =

work page 2012
[3]

Acta Astronomica , author =

Evolution of. Acta Astronomica , author =. 2011 , note =

work page 2011
[4]

The Astrophysical Journal , author =

The. The Astrophysical Journal , author =. 1995 , note =. doi:10.1086/187855 , abstract =

work page doi:10.1086/187855 1995
[5]

The Astrophysical Journal , author =

Stellar. The Astrophysical Journal , author =. 2025 , pages =. doi:10.3847/1538-4357/ade9bc , abstract =

work page doi:10.3847/1538-4357/ade9bc 2025
[6]

Astronomy & Astrophysics , author =

Wind. Astronomy & Astrophysics , author =. 2013 , pages =. doi:10.1051/0004-6361/201220007 , abstract =

work page doi:10.1051/0004-6361/201220007 2013
[7]

Monthly Notices of the Royal Astronomical Society , author =

A catalogue of masses, structural parameters and velocity dispersion profiles of 112. Monthly Notices of the Royal Astronomical Society , author =. 2018 , note =. doi:10.1093/mnras/sty1057 , abstract =

work page doi:10.1093/mnras/sty1057 2018
[8]

Nature Communications , author =

A binary-related origin mediated by environmental conditions for blue straggler stars , volume =. Nature Communications , author =. 2026 , note =. doi:10.1038/s41467-025-68159-5 , abstract =

work page doi:10.1038/s41467-025-68159-5 2026
[9]

Astronomy & Astrophysics , author =

Differential reddening in 48 globular clusters:. Astronomy & Astrophysics , author =. 2024 , pages =. doi:10.1051/0004-6361/202449462 , abstract =

work page doi:10.1051/0004-6361/202449462 2024
[10]

2016, ApJS, 222, 8, doi: 10.3847/0067-0049/222/1/8 Ekstr¨ om, S., Georgy, C., Eggenberger, P., et al

The Astrophysical Journal Supplement Series , author =. 2016 , note =. doi:10.3847/0067-0049/222/1/8 , abstract =

work page doi:10.3847/0067-0049/222/1/8 2016
[12]

2015 , note =

The Astrophysical Journal Letters , author =. 2015 , note =. doi:10.1088/2041-8205/808/1/L25 , abstract =

work page doi:10.1088/2041-8205/808/1/l25 2015
[13]

2025 , pages =

The Astrophysical Journal , author =. 2025 , pages =. doi:10.3847/1538-4357/adcd73 , abstract =

work page doi:10.3847/1538-4357/adcd73 2025
[14]

, month = feb, year =

Linck, Evan and Mathieu, Robert D. , month = feb, year =. The

work page
[15]

, month = jan, year =

Fitzpatrick, Michael J. , month = jan, year =. The. Astronomical

work page
[16]

Mathieu, R. D. , month = jan, year =. The

work page
[17]

, month = jan, year =

Osterbrock, Donald E. , month = jan, year =. Walter. Stellar

work page
[18]

and Podsiadlowski, Ph

Mohamed, S. and Podsiadlowski, Ph. , month = sep, year =. Wind. Astronomical

work page
[19]

The Astrophysical Journal , author =

A. The Astrophysical Journal , author =. 1959 , note =. doi:10.1086/146661 , abstract =

work page doi:10.1086/146661 1959
[20]

Astrophysical Letters , author =

Stellar. Astrophysical Letters , author =. 1976 , note =

work page 1976
[21]

, keywords =

Blue straggler production in globular clusters , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2004 , pages =. doi:10.1111/j.1365-2966.2004.07474.x , abstract =

work page doi:10.1111/j.1365-2966.2004.07474.x 2004
[22]

The Astrophysical Journal , author =

A. The Astrophysical Journal , author =. 2001 , note =. doi:10.1086/320560 , abstract =

work page doi:10.1086/320560 2001
[24]

Publications of the Astronomical Society of the Pacific , author =

The. Publications of the Astronomical Society of the Pacific , author =. 2018 , note =. doi:10.1088/1538-3873/aae8ac , abstract =

work page internal anchor Pith review doi:10.1088/1538-3873/aae8ac 2018
[25]

2025 , note =

The Astrophysical Journal Supplement Series , author =. 2025 , note =. doi:10.3847/1538-4365/adfb78 , abstract =

work page doi:10.3847/1538-4365/adfb78 2025
[26]

F., Quataert, E., & Murray, N

Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2011 , pages =. doi:10.1111/j.1365-2966.2011.19386.x , abstract =

work page doi:10.1111/j.1365-2966.2011.19386.x 2011
[27]

Journal of the British Astronomical Association , author =

A light history of photometry: from. Journal of the British Astronomical Association , author =. 2007 , note =

work page 2007
[28]

Monthly Notices of the Royal Astronomical Society , author =

Long-term evolution of a magnetic massive merger product , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2020 , note =. doi:10.1093/mnras/staa1326 , abstract =

work page doi:10.1093/mnras/staa1326 2020
[29]

Astronomy and Astrophysics , author =

Seismic signature of electron degeneracy in the core of red giants:. Astronomy and Astrophysics , author =. 2022 , note =. doi:10.1051/0004-6361/202142094 , abstract =

work page doi:10.1051/0004-6361/202142094 2022
[30]

Monthly Notices of the Royal Astronomical Society , author =

Asteroseismic fingerprints of stellar mergers , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2021 , note =. doi:10.1093/mnras/stab2528 , abstract =

work page doi:10.1093/mnras/stab2528 2021
[31]

Astronomy & Astrophysics , author =

Red horizontal branch stars:. Astronomy & Astrophysics , author =. 2023 , note =. doi:10.1051/0004-6361/202245746 , abstract =

work page doi:10.1051/0004-6361/202245746 2023
[32]

The Astronomical Journal , author =

A. The Astronomical Journal , author =. 2026 , pages =. doi:10.3847/1538-3881/ae3b42 , abstract =

work page doi:10.3847/1538-3881/ae3b42 2026
[33]

Monthly Notices of the Royal Astronomical Society , author =

The white dwarf binary pathways survey –. Monthly Notices of the Royal Astronomical Society , author =. 2024 , pages =. doi:10.1093/mnras/stae807 , abstract =

work page doi:10.1093/mnras/stae807 2024
[34]

, keywords =

Post-common envelope binaries from. Monthly Notices of the Royal Astronomical Society , author =. 2010 , note =. doi:10.1111/j.1365-2966.2009.15915.x , abstract =

work page doi:10.1111/j.1365-2966.2009.15915.x 2010
[35]

Monthly Notices of the Royal Astronomical Society , author =

The white dwarf binary pathways survey -. Monthly Notices of the Royal Astronomical Society , author =. 2017 , note =. doi:10.1093/mnras/stx2259 , abstract =

work page doi:10.1093/mnras/stx2259 2017
[36]

Astronomy and Astrophysics , author =

A stellar census in globular clusters with. Astronomy and Astrophysics , author =. 2019 , note =. doi:10.1051/0004-6361/201936203 , abstract =

work page doi:10.1051/0004-6361/201936203 2019
[37]

Astronomy and Astrophysics , author =

Barium and related stars, and their white-dwarf companions. Astronomy and Astrophysics , author =. 2019 , note =. doi:10.1051/0004-6361/201935390 , abstract =

work page doi:10.1051/0004-6361/201935390 2019
[38]

Zeitschrift Fur Wissenschaftliche Photographie , author =

Zur. Zeitschrift Fur Wissenschaftliche Photographie , author =. 1905 , note =

work page 1905
[39]

Publikationen des Astrophysikalischen Observatoriums zu Potsdam , author =

Ueber die. Publikationen des Astrophysikalischen Observatoriums zu Potsdam , author =. 1911 , note =

work page 1911
[40]

The Observatory , author =

". The Observatory , author =. 1913 , note =

work page 1913
[41]

2020 , note =

The Astrophysical Journal , author =. 2020 , note =. doi:10.3847/1538-4357/ab9d85 , abstract =

work page doi:10.3847/1538-4357/ab9d85 2020
[43]

Monthly Notices of the Royal Astronomical Society , author =

Asteroseismology of overmassive, undermassive, and potential past members of the open cluster. Monthly Notices of the Royal Astronomical Society , author =. 2021 , pages =. doi:10.1093/mnras/stab2183 , abstract =

work page doi:10.1093/mnras/stab2183 2021
[44]

Latham, D. W. and Milone, A. A. E. , year =. Spectroscopic. The origins, evolution, and destinies of binary stars in clusters , publisher =

work page
[45]

Milone, A. A. E. and Latham, D. W. , month = jan, year =. The. Evolutionary

work page
[46]

The Astronomical Journal , author =

Radial. The Astronomical Journal , author =. 1994 , note =. doi:10.1086/117195 , abstract =

work page doi:10.1086/117195 1994
[47]

Annual Review of Astronomy and Astrophysics , author =

Evolutionary. Annual Review of Astronomy and Astrophysics , author =. 1971 , note =. doi:10.1146/annurev.aa.09.090171.001151 , urldate =

work page doi:10.1146/annurev.aa.09.090171.001151 1971
[48]

Methodology and a fast-fitting algorithm

Binary coalescence from case. Monthly Notices of the Royal Astronomical Society , author =. 2008 , pages =. doi:10.1111/j.1365-2966.2007.12617.x , abstract =

work page doi:10.1111/j.1365-2966.2007.12617.x 2008
[49]

The Astrophysical Journal , author =

The galactic cluster. The Astrophysical Journal , author =. 1955 , note =. doi:10.1086/146027 , abstract =

work page doi:10.1086/146027 1955
[50]

Zeitschrift für wissenschaftliche photographie, photophysik und photochemie. , url =. 1903 , keywords =

work page 1903
[51]

Annals of Harvard College Observatory , author =

Spectra of bright stars photographed with the 11-inch. Annals of Harvard College Observatory , author =. 1897 , note =

work page
[52]

Annals of Harvard College Observatory , author =

Spectra of bright southern stars photographed with the 13-inch. Annals of Harvard College Observatory , author =. 1901 , note =

work page 1901
[53]

Publications of the Yerkes Observatory , author =

A. Publications of the Yerkes Observatory , author =. 1900 , note =

work page 1900
[54]

The Astrophysical Journal , author =

An. The Astrophysical Journal , author =. 1964 , note =. doi:10.1086/147946 , abstract =

work page doi:10.1086/147946 1964
[55]

The Astrophysical Journal , author =

The. The Astrophysical Journal , author =. 1964 , pages =. doi:10.1086/147948 , abstract =

work page doi:10.1086/147948 1964
[56]

The Critical Importance of Russell's Diagram

The. ASP Conference Series , author =. 2013 , note =. doi:10.48550/arXiv.1302.0862 , abstract =

work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1302.0862 2013
[57]

Townsend, Richard H. D. , year =. Stellar

work page
[58]

Kratter, K. M. , month = sep, year =. The. doi:10.48550/arXiv.1109.3740 , abstract =

work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1109.3740
[59]

The Astrophysical Journal , author =

Dynamical. The Astrophysical Journal , author =. 2018 , pages =. doi:10.3847/1538-4357/aaa6d2 , abstract =

work page doi:10.3847/1538-4357/aaa6d2 2018
[60]

Annual Review of Astronomy and Astrophysics , author =

The. Annual Review of Astronomy and Astrophysics , author =. 2002 , note =. doi:10.1146/annurev.astro.40.060401.093810 , abstract =

work page doi:10.1146/annurev.astro.40.060401.093810 2002
[61]

Annual Review of Astronomy and Astrophysics , author =

Pre-. Annual Review of Astronomy and Astrophysics , author =. 1994 , note =. doi:10.1146/annurev.aa.32.090194.002341 , urldate =

work page doi:10.1146/annurev.aa.32.090194.002341 1994
[62]

Kippenhahn, Rudolf and Weigert, Alfred and Weiss, Achim , month = jan, year =. Stellar. doi:10.1007/978-3-642-30304-3 , note =

work page doi:10.1007/978-3-642-30304-3
[63]

, month = apr, year =

Pols, Onno R. , month = apr, year =. Stellar structure and evolution lecture notes , url =

work page
[64]

The Astrophysical Journal , author =

Magnetic. The Astrophysical Journal , author =. 2023 , note =. doi:10.3847/1538-4357/acc86e , abstract =

work page doi:10.3847/1538-4357/acc86e 2023
[65]

Nature , author =

Stellar mergers as the origin of magnetic massive stars , volume =. Nature , author =. 2019 , note =. doi:10.1038/s41586-019-1621-5 , abstract =

work page doi:10.1038/s41586-019-1621-5 2019
[66]

The Astrophysical Journal , author =

Aproximations to the radii of. The Astrophysical Journal , author =. 1983 , note =. doi:10.1086/160960 , abstract =

work page doi:10.1086/160960 1983
[67]

The Astrophysical Journal , author =

The response of main-sequence stars within a common envelope , volume =. The Astrophysical Journal , author =. 1991 , pages =. doi:10.1086/169854 , abstract =

work page doi:10.1086/169854 1991
[68]

The Astrophysical Journal , author =

Stellar. The Astrophysical Journal , author =. 2024 , pages =. doi:10.3847/1538-4357/ad54be , abstract =

work page doi:10.3847/1538-4357/ad54be 2024
[69]

The Astrophysical Journal , author =

Wind. The Astrophysical Journal , author =. 2024 , pages =. doi:10.3847/1538-4357/ad47c1 , abstract =

work page doi:10.3847/1538-4357/ad47c1 2024
[70]

The Astrophysical Journal , author =

Rotation. The Astrophysical Journal , author =. 2019 , pages =. doi:10.3847/1538-4357/ab2ed2 , abstract =

work page doi:10.3847/1538-4357/ab2ed2 2019
[71]

, keywords =

The. The Astrophysical Journal Supplement Series , author =. 2022 , note =. doi:10.3847/1538-4365/ac4414 , abstract =

work page doi:10.3847/1538-4365/ac4414 2022
[72]

The Astronomical Journal , author =

What. The Astronomical Journal , author =. 2000 , note =. doi:10.1086/301472 , abstract =

work page doi:10.1086/301472 2000
[73]

The Astronomical Journal , author =

Metal-poor. The Astronomical Journal , author =. 2005 , pages =. doi:10.1086/426566 , abstract =

work page doi:10.1086/426566 2005
[74]

, keywords =

The non-peculiar velocity dispersion profile of the stellar system ω. Monthly Notices of the Royal Astronomical Society , author =. 2009 , pages =. doi:10.1111/j.1365-2966.2009.14864.x , abstract =

work page doi:10.1111/j.1365-2966.2009.14864.x 2009
[75]

The Astrophysical Journal , author =

Asteroseismic. The Astrophysical Journal , author =. 2025 , pages =. doi:10.3847/1538-4357/ae12f2 , abstract =

work page doi:10.3847/1538-4357/ae12f2 2025
[76]

The Astrophysical Journal , author =

On the. The Astrophysical Journal , author =. 2003 , note =. doi:10.1086/367639 , abstract =

work page doi:10.1086/367639 2003
[77]

The Astronomical Journal , author =

Toward. The Astronomical Journal , author =. 2019 , note =. doi:10.3847/1538-3881/ab3c53 , abstract =

work page doi:10.3847/1538-3881/ab3c53 2019
[78]

Journal of Open Source Software , author =

lifelines: survival analysis in. Journal of Open Source Software , author =. 2019 , pages =. doi:10.21105/joss.01317 , abstract =

work page doi:10.21105/joss.01317 2019
[79]

, keywords =

Accurate distances to. Monthly Notices of the Royal Astronomical Society , author =. 2021 , note =. doi:10.1093/mnras/stab1474 , abstract =

work page doi:10.1093/mnras/stab1474 2021
[80]

Monthly Notices of the Royal Astronomical Society , author =

Spherical models of star clusters with potential escapers , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2019 , note =. doi:10.1093/mnras/stz1109 , abstract =

work page doi:10.1093/mnras/stz1109 2019
[81]

Astronomy & Astrophysics , author =

Fast. Astronomy & Astrophysics , author =. 2026 , note =. doi:10.1051/0004-6361/202557251 , abstract =

work page doi:10.1051/0004-6361/202557251 2026
[82]

and Price-Whelan, Adrian M

Chen, Yingtian and Gnedin, Oleg Y. and Price-Whelan, Adrian M. , month = oct, year =. doi:10.48550/arXiv.2510.14924 , abstract =

work page doi:10.48550/arxiv.2510.14924
[83]

, keywords =

High-resolution simulations of stellar collisions between equal-mass main-sequence stars in globular clusters , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2002 , note =. doi:10.1046/j.1365-8711.2002.05266.x , abstract =

work page doi:10.1046/j.1365-8711.2002.05266.x 2002

Showing first 80 references.