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arxiv: 2606.12242 · v1 · pith:ZU7ZWU3Onew · submitted 2026-06-10 · 🌌 astro-ph.SR

Shaping the horizontal branch: The role of envelope mass in the evolution of stripped core-helium-burning stars

Eduardo Arancibia-Rojas , M\'onica Zorotovic , Maja Vu\v{c}kovi\'c , Alexey Bobrick , Alex Dur\'an-Reyes This is my paper

Pith reviewed 2026-06-27 08:12 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords horizontal branchstripped starsenvelope masscore helium burningblue hook starsasymptotic giant branchstellar evolutionMESA
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The pith

The residual hydrogen envelope mass after stripping on the first giant branch sets the horizontal branch position of core-helium-burning stars and the maximum mass that still avoids later thermally pulsing asymptotic giant branch evolution.

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

Stars that lose their hydrogen envelopes on the first giant branch become core-helium-burning stars whose location on the horizontal branch depends on how much envelope remains. Models varying the envelope mass from near zero up to several tenths of a solar mass show that effective temperature drops as more envelope is left. The maximum envelope mass that still prevents later evolution through the thermally pulsing asymptotic giant branch increases with progenitor mass, from about 0.05 solar masses at low mass to 0.30 at intermediate mass. Early stripping on low-mass stars produces a late hot flash that accounts for the hottest observed blue hook stars. Partial stripping on intermediate-mass stars can create extended pre-horizontal-branch phases seen in some binary systems.

Core claim

We computed evolutionary sequences for stripped stars with initial masses below about 6 solar masses at two metallicities, removing the envelope at the minimum and maximum core masses for helium ignition and varying the remaining envelope mass. As envelope mass rises, stars sit at cooler temperatures on the horizontal branch. The upper limit on envelope mass to skip the thermally pulsing asymptotic giant branch is 0.05 solar masses for low-mass progenitors and 0.30 solar masses for intermediate-mass ones. Early envelope loss in low-mass cases triggers a late hot flash that reproduces the properties of the hottest blue hook stars, while intermediate-mass cases with partial stripping match ext

What carries the argument

Residual hydrogen-envelope mass after stripping on the first giant branch, which controls effective temperature on the horizontal branch and the path of subsequent evolution.

If this is right

  • Effective temperature along the horizontal branch decreases with increasing residual envelope mass.
  • Maximum residual envelope mass to avoid the thermally pulsing asymptotic giant branch is approximately 0.05 solar masses for low-mass progenitors and 0.30 solar masses for intermediate-mass progenitors.
  • Early envelope removal in low-mass progenitors induces a late hot flash that explains the hottest blue hook stars.
  • Partial envelope stripping in intermediate-mass systems produces extended pre-horizontal-branch configurations observed in binaries with Be companions.
  • Post-stripping evolutionary tracks are made available for use in binary population synthesis.

Where Pith is reading between the lines

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

  • These envelope mass thresholds may help predict the fraction of horizontal branch stars versus asymptotic giant branch stars in stellar populations.
  • The models could be tested against observed horizontal branch morphologies in globular clusters at different metallicities.
  • The late hot flash mechanism might apply to other stripping scenarios such as those in close binaries.
  • Extending the grid to higher masses or different stripping timings could reveal additional pathways for blue hook star formation.

Load-bearing premise

Envelope removal is assumed to occur on the first giant branch at the two extreme core masses that allow helium ignition.

What would settle it

A direct count of whether stars with measured envelope masses above 0.30 solar masses for intermediate-mass progenitors proceed to the thermally pulsing asymptotic giant branch or remain on the horizontal branch.

Figures

Figures reproduced from arXiv: 2606.12242 by Alex Dur\'an-Reyes, Alexey Bobrick, Eduardo Arancibia-Rojas, Maja Vu\v{c}kovi\'c, M\'onica Zorotovic.

Figure 1
Figure 1. Figure 1: shows the evolutionary tracks in the HR diagram for a star with an initial mass of 1.5 M⊙, stripped of its envelope at [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 3
Figure 3. Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: same as in [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as in [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Top panel: critical envelope mass required to reach the TPAGB phase, as a function of MZAMS. Black circles show the initial residual envelope mass set by the relax_mass process. Red plus signs and blue crosses show the envelope mass at the beginning and end of the sub￾sequent subdwarf phase, respectively. Bottom panel: He-core mass at the tip of the FGB phase (black circles) and the enclosed mass of the st… view at source ↗
Figure 7
Figure 7. Figure 7: Evolution in the Menv–MHe,core plane for the first models that reach the TPAGB phase for different ZAMS masses (labelled at the beginning of each track). Progenitors with degenerate (left panel) and non-degenerate (right panel) ignition are shown separately. Black circles indicate Menv and MHe,core immediately after stripping, while red plus signs and blue crosses mark the beginning and end of the subdwarf… view at source ↗
Figure 8
Figure 8. Figure 8: Location of our models during the hot subdwarf phase (as defined in Sect. 2) in the HR (top) and Kiel (bottom) diagrams. Left and right panels separate low-mass progenitors (MZAMS ≤ 1.9 M⊙), with degenerate He cores, from higher-mass ones (MZAMS ≥ 2.0 M⊙), that ignite He under non-degenerate or mildly degenerate conditions. Different symbols denote different ZAMS masses. Colours indicate the instantaneous … view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of post-stripping evolutionary tracks in the HR diagram for MZAMS = 1.5 M⊙ (left) and MZAMS = 3.0 M⊙ (right) in the tip FGB (blue) and early (black) removal scenarios. All models shown were left with a residual envelope of 0.01 M⊙. The symbol coding is the same as in [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Evolution of physical parameters after stripping in the early-removal scenario for MZAMS = 1.5 M⊙ (left) and MZAMS = 3.0 M⊙ (right) models with Menv = 0.01 M⊙. The panels show the same quantities as in [PITH_FULL_IMAGE:figures/full_fig_p008_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Same as in [PITH_FULL_IMAGE:figures/full_fig_p009_11.png] view at source ↗
Figure 12
Figure 12. Figure 12 [PITH_FULL_IMAGE:figures/full_fig_p009_12.png] view at source ↗
read the original abstract

The location of a star along the horizontal branch (HB) during core-helium burning is primarily determined by the amount of mass lost by its progenitor. We investigate the formation and properties of stripped core-helium-burning stars, focusing on how the residual hydrogen-envelope mass ($M_{\mathrm{env}}$) and the timing of envelope removal shape their properties. We used the MESA stellar evolution code to model stars that lose their hydrogen envelopes on the first giant branch. We explored two limiting cases for the timing of stripping, corresponding to the minimum and maximum core masses for helium ignition, for progenitors with initial masses below $\sim$6 $M_{\odot}$ at two metallicities ($Z=0.02$ and $Z=0.004$), while systematically varying $M_{\mathrm{env}}$. As expected, the effective temperature along the HB decreases as $M_{\mathrm{env}}$ increases. We determined the maximum $M_{\mathrm{env}}$ required to avoid subsequent evolution through the thermally pulsing asymptotic giant branch, which ranges from $\sim0.05$ $M_{\odot}$, for low-mass progenitors to $\sim0.30$ $M_{\odot}$ for intermediate-mass progenitors. In low-mass progenitors, early envelope removal triggers a late hot flash, naturally explaining the hottest blue hook stars. In intermediate-mass systems, partial envelope stripping can produce extended pre-HB configurations consistent with puffed-up stripped stars observed in binaries with Be companions. Our post-stripping evolutionary tracks are publicly available for use in binary evolution and population synthesis studies.

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

1 major / 0 minor

Summary. The paper uses MESA to model stars that lose their hydrogen envelopes on the first giant branch, exploring two limiting cases for the timing of stripping (minimum and maximum core masses for helium ignition) for progenitors below ~6 Msun at Z=0.02 and Z=0.004 while varying residual envelope mass M_env. It reports that effective temperature on the HB decreases with increasing M_env, determines the maximum M_env to avoid TP-AGB evolution (~0.05 Msun for low-mass to ~0.30 Msun for intermediate-mass progenitors), and notes that early stripping in low-mass stars triggers a late hot flash while partial stripping in intermediate-mass systems can produce extended pre-HB phases. Post-stripping tracks are made public.

Significance. If the numerical results hold, the work supplies publicly available evolutionary tracks useful for binary population synthesis and offers a natural explanation for the hottest blue hook stars via late hot flashes in low-mass stripped stars. The systematic parameter variation over progenitor mass and metallicity strengthens the mapping from M_env to HB location and TP-AGB avoidance.

major comments (1)
  1. [Abstract and methods description] Abstract and methods description: the reported maximum M_env thresholds (0.05–0.30 Msun) are obtained exclusively from instantaneous envelope removal at the two limiting core masses for He ignition. No sequences with finite-rate removal (e.g., over 10^4–10^6 yr) or continuous mass-loss histories are described; because core growth and thermal relaxation during stripping depend on the adopted timescale, the critical M_env values could shift by an amount comparable to the quoted range itself.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for identifying this methodological point. We address the comment below.

read point-by-point responses

  1. Referee: [Abstract and methods description] Abstract and methods description: the reported maximum M_env thresholds (0.05–0.30 Msun) are obtained exclusively from instantaneous envelope removal at the two limiting core masses for He ignition. No sequences with finite-rate removal (e.g., over 10^4–10^6 yr) or continuous mass-loss histories are described; because core growth and thermal relaxation during stripping depend on the adopted timescale, the critical M_env values could shift by an amount comparable to the quoted range itself.

    Authors: We thank the referee for this observation. Our calculations deliberately employ instantaneous envelope removal at the two limiting core masses for helium ignition precisely to bracket the range of possible stripping outcomes while isolating the dependence on residual envelope mass M_env. These two cases correspond to the earliest and latest plausible moments of envelope loss on the first giant branch. We acknowledge that a finite-duration mass-loss episode would permit some core growth and thermal readjustment during the stripping phase itself, and that the precise critical M_env values separating HB from TP-AGB evolution could therefore differ from the instantaneous limits we report. In the revised manuscript we will (i) state explicitly in the methods section that envelope removal is modeled as instantaneous, (ii) add a brief discussion of how continuous mass-loss histories would be expected to produce results intermediate between our two limiting cases, and (iii) note this modeling choice as a limitation when interpreting the quoted M_env thresholds. We believe these additions will clarify the scope of the reported thresholds without altering the main conclusions of the work. revision: yes

Circularity Check

0 steps flagged

No circularity: numerical forward modeling with M_env varied as explicit input

full rationale

The paper runs MESA simulations that take initial mass, metallicity, stripping timing (two fixed RGB core-mass limits), and residual M_env as independent inputs, then reports the resulting HB properties and the M_env threshold that avoids TP-AGB evolution. These thresholds are direct simulation outputs, not quantities obtained by fitting to data and then relabeled as predictions, nor derived from self-citations whose content reduces to the present work. No self-definitional loops, ansatz smuggling, or renaming of known results appear in the derivation chain. The work is self-contained against external stellar-evolution benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The work rests on standard MESA stellar evolution assumptions and the choice to explore two limiting stripping times on the first giant branch; no new entities are introduced and M_env is treated as a free exploration parameter rather than a fitted constant.

free parameters (1)
  • M_env
    Systematically varied across runs to map its effect on HB temperature and later evolution; not fitted to data but chosen as the central control variable.
axioms (2)
  • domain assumption MESA code accurately captures core helium burning, envelope stripping, and subsequent evolution for stars below 6 solar masses at the stated metallicities.
    All results derive from MESA runs; no independent verification of the code's behavior for these stripped configurations is provided in the abstract.
  • domain assumption Envelope removal occurs on the first giant branch in the two limiting core-mass cases for helium ignition.
    Explicitly stated as the modeling setup in the abstract.

pith-pipeline@v0.9.1-grok · 5844 in / 1507 out tokens · 19619 ms · 2026-06-27T08:12:41.971342+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

125 extracted references · 114 canonical work pages · 45 internal anchors

  1. [1]

    , year = 1954, month = jan, volume = 119, pages =

    On the Indentification of Radio Sources. , year = 1954, month = jan, volume = 119, pages =

    1954

  2. [2]

    Lithium and mass loss in massive AGB stars in the Large Magellanic Clouds

    Lithium and mass loss in massive AGB stars in the Large Magellanic Cloud. , keywords =. doi:10.48550/arXiv.astro-ph/0101374 , archivePrefix =. astro-ph/0101374 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0101374

  3. [3]

    The Origin of Hot Subluminous Horizontal-Branch Stars in Omega Centauri and NGC 2808

    The Origin of Hot Subluminous Horizontal-Branch Stars in Centauri and NGC 2808. Omega Centauri, A Unique Window into Astrophysics , year = 2002, editor =. doi:10.48550/arXiv.astro-ph/0203063 , archivePrefix =. astro-ph/0203063 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0203063 2002

  4. [4]

    , keywords =

    Mass Loss in Globular Cluster Red Giants: an Evolutionary Investigation. , keywords =. doi:10.1086/172547 , adsurl =

    work page doi:10.1086/172547

  5. [5]

    Stellar evolution of low and intermediate-mass stars. I. Mass loss on the AGB and its consequences for stellar evolution. , keywords =

  6. [6]

    , keywords =

    RR Lyrae from binary evolution: abundant, young, and metal-rich. , keywords =. doi:10.1093/mnras/stad3996 , archivePrefix =. 2208.04332 , primaryClass =

    work page doi:10.1093/mnras/stad3996

  7. [7]

    , keywords =

    Alone but not lonely: Observational evidence that binary interaction is always required to form hot subdwarf stars. , keywords =. doi:10.1051/0004-6361/202038473 , archivePrefix =. 2008.07522 , primaryClass =

    work page doi:10.1051/0004-6361/202038473 2008

  8. [8]

    Horizontal-branch morphology and multiple stellar populations in the anomalous globular cluster M22

    Horizontal Branch Morphology and Multiple Stellar Populations in the Anomalous Globular Cluster M 22. , keywords =. doi:10.1088/0004-637X/768/1/27 , archivePrefix =. 1302.5870 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/768/1/27

  9. [9]

    , year = 1976, month = mar, volume =

    Gaps in the blue horizontal branch. , year = 1976, month = mar, volume =. doi:10.1086/154228 , adsurl =

    work page doi:10.1086/154228 1976

  10. [10]

    Multiple Populations on the Horizontal Branch. I. Observations in the (log g, log T eff)--Diagram. , keywords =. doi:10.1086/166648 , adsurl =

    work page doi:10.1086/166648

  11. [11]

    , keywords =

    A stripped-companion origin for Be stars: clues from the putative black holes HR 6819 and LB-1. , keywords =. doi:10.1093/mnras/stab285 , archivePrefix =. 2006.11974 , primaryClass =

    work page doi:10.1093/mnras/stab285 2006

  12. [12]

    , keywords =

    Evolutionary nature of puffed-up stripped star binaries and their occurrence in stellar populations. , keywords =. doi:10.1051/0004-6361/202349065 , archivePrefix =. 2312.12658 , primaryClass =

    work page doi:10.1051/0004-6361/202349065

  13. [13]

    , keywords =

    A self-synthesized origin for heavy metals in hot subdwarf stars. , keywords =. doi:10.1051/0004-6361/202348157 , archivePrefix =. 2311.04700 , primaryClass =

    work page doi:10.1051/0004-6361/202348157

  14. [14]

    Bimodality and Gaps on Globular Cluster Horizontal Branches. II. The Cases of NGC 6229, NGC 1851, and NGC 2808. , keywords =. doi:10.1086/305200 , archivePrefix =. astro-ph/9708096 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/305200

  15. [15]

    The sdA problem I: Physical Properties

    The sdA problem - I. Physical properties. , keywords =. doi:10.1093/mnras/sty011 , archivePrefix =. 1801.00495 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty011

  16. [16]

    Are sdAs helium core stars?

    Are sdAs helium core stars?. Open Astronomy , keywords =. doi:10.1515/astro-2017-0433 , archivePrefix =. 1710.09882 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1515/astro-2017-0433 2017

  17. [17]

    New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12

    New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12. , keywords =. doi:10.1093/mnras/stv2526 , archivePrefix =. 1510.08409 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2526

  18. [18]

    The Nature of Faint Blue Stars in the Halo. II. , year = 1974, month = nov, volume =. doi:10.1086/190315 , adsurl =

    work page doi:10.1086/190315 1974

  19. [19]

    IAU Colloq

    Quantitative spectroscopy of HBB stars and sdB stars. IAU Colloq. 95: Second Conference on Faint Blue Stars , year = 1987, editor =

    1987

  20. [20]

    Ultraviolet Radiation from Evolved Stellar Populations. I. Models. , keywords =. doi:10.1086/173511 , archivePrefix =. astro-ph/9311022 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/173511

  21. [21]

    , keywords =

    Synthetic Colors and the Chemical Evolution of Elliptical Galaxies. , keywords =. doi:10.1086/168330 , adsurl =

    work page doi:10.1086/168330

  22. [22]

    , keywords =

    Analysis of the Hot Stellar Population of the Globular Cluster Centauri. , keywords =. doi:10.1086/305288 , adsurl =

    work page doi:10.1086/305288

  23. [23]

    , year = 2016, month = sep, volume =

    Red Clump Stars. , year = 2016, month = sep, volume =. doi:10.1146/annurev-astro-081915-023354 , adsurl =

    work page doi:10.1146/annurev-astro-081915-023354 2016

  24. [24]

    HST Observations of New Horizontal Branch Structures in the Globular Cluster omega Centauri

    Hubble Space Telescope Observations of New Horizontal Branch Structures in the Globular Cluster omega Centauri. , keywords =. doi:10.1086/308375 , archivePrefix =. astro-ph/9909371 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308375

  25. [25]

    , keywords =

    The elusive chase for the first RR Lyr star in a binary system: the case of KIC 2831097. , keywords =. doi:10.1051/0004-6361/202556279 , archivePrefix =. 2509.20473 , primaryClass =

    work page doi:10.1051/0004-6361/202556279

  26. [26]

    VFTS 291: a stripped star from a recent mass transfer phase

    The B-type Binaries Characterisation Programme - II. VFTS 291: a stripped star from a recent mass transfer phase. , keywords =. doi:10.1093/mnras/stad2533 , archivePrefix =. 2307.07766 , primaryClass =

    work page doi:10.1093/mnras/stad2533

  27. [27]

    , keywords =

    HR6819: a puffed-up stripped star system challenging stable mass transfer theory. , keywords =. doi:10.1051/0004-6361/202556556 , archivePrefix =. 2509.21521 , primaryClass =

    work page doi:10.1051/0004-6361/202556556

  28. [28]

    , keywords =

    The binary fraction of extreme horizontal branch stars. , keywords =. doi:10.1111/j.1365-2966.2001.04714.x , archivePrefix =. astro-ph/0103342 , primaryClass =

    work page doi:10.1111/j.1365-2966.2001.04714.x 2001

  29. [29]

    , keywords =

    The binary fraction of blue horizontal branch stars. , keywords =. doi:10.1051/0004-6361/202555002 , archivePrefix =. 2508.02790 , primaryClass =

    work page doi:10.1051/0004-6361/202555002

  30. [30]

    New RR Lyrae variables in binary systems

    New RR Lyrae variables in binary systems. , keywords =. doi:10.1093/mnrasl/slv024 , archivePrefix =. 1502.01318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slv024

  31. [31]

    Studies of RR Lyrae Variables in Binary Systems. I. Evidence of a Trimodal Companion Mass Distribution. , keywords =. doi:10.3847/1538-4357/abff4b , archivePrefix =. 2105.03750 , primaryClass =

    work page doi:10.3847/1538-4357/abff4b

  32. [32]

    , keywords =

    A Radial-velocity Search for Binary RR Lyrae Variables. , keywords =. doi:10.3847/1538-3881/ac09f2 , archivePrefix =. 2106.05208 , primaryClass =

    work page doi:10.3847/1538-3881/ac09f2

  33. [33]

    The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. VII. Implications from the Nearly Universal Nature of Horizontal Branch Discontinuities. , keywords =. doi:10.3847/0004-637X/822/1/44 , archivePrefix =. 1603.07651 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/822/1/44

  34. [34]

    The atmosphere of subluminous B stars. II. Analysis of 10 helium poor subdwarfs and the birthrate of sdB stars. , keywords =

  35. [35]

    The Origin of Extreme Horizontal Branch Stars

    The Origin of Extreme Horizontal Branch Stars. , keywords =. doi:10.1086/177515 , archivePrefix =. astro-ph/9511017 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/177515

  36. [36]

    First full evolutionary computation of the He-flash induced mixing in Population II stars

    First Full Evolutionary Computation of the Helium Flash-induced Mixing in Population II Stars. , keywords =. doi:10.1086/346200 , archivePrefix =. astro-ph/0211498 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/346200

  37. [37]

    Helium Mixing in Globular Cluster Stars

    Helium Mixing in Globular Cluster Stars. The Third Conference on Faint Blue Stars , year = 1997, editor =. doi:10.48550/arXiv.astro-ph/9708164 , archivePrefix =. astro-ph/9708164 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9708164 1997

  38. [38]

    Spectroscopic Analyses of the "Blue Hook" Stars in omega Centauri: A Test of the Late Hot Flasher Scenario

    Spectroscopic analyses of the ``blue hook'' stars in omega Centauri: A test of the late hot flasher scenario. , keywords =. doi:10.1051/0004-6361:20021248 , archivePrefix =. astro-ph/0209028 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20021248

  39. [39]

    Spectroscopic Analyses of the Blue Hook Stars in NGC 2808: A More Stringent Test of the Late Hot Flasher Scenario

    Spectroscopic analyses of the blue hook stars in NGC 2808: A more stringent test of the late hot flasher scenario. , keywords =. doi:10.1051/0004-6361:20034505 , archivePrefix =. astro-ph/0311215 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20034505

  40. [40]

    The Blue Hook Populations of Massive Globular Clusters

    The Blue Hook Populations of Massive Globular Clusters. , keywords =. doi:10.1088/0004-637X/718/2/1332 , archivePrefix =. 1006.1591 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/718/2/1332

  41. [41]

    , keywords =

    Effects of Helium Mixing on the Evolution of Globular Cluster Stars. , keywords =. doi:10.1086/310414 , adsurl =

    work page doi:10.1086/310414

  42. [42]

    , keywords =

    The mass range of hot subdwarf B stars from MESA simulations. , keywords =. doi:10.1093/mnras/stad3891 , archivePrefix =. 2312.09920 , primaryClass =

    work page doi:10.1093/mnras/stad3891

  43. [43]

    , keywords =

    Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure. , keywords =. doi:10.3847/1538-4365/acae8d , archivePrefix =. 2208.03651 , primaryClass =

    work page doi:10.3847/1538-4365/acae8d

  44. [44]

    Explaining the orbital period-mass ratio relation in wide hot subdwarf binaries

    Observed binary populations reflect the Galactic history. Explaining the orbital period-mass ratio relation in wide hot subdwarf binaries. , keywords =. doi:10.1051/0004-6361/201937195 , archivePrefix =. 2003.05665 , primaryClass =

    work page doi:10.1051/0004-6361/201937195 2003

  45. [45]

    The effects of diffusion in hot subdwarf progenitors from the common envelope channel

    The effects of diffusion in hot subdwarf progenitors from the common envelope channel. , keywords =. doi:10.1093/mnras/sty158 , archivePrefix =. 1802.00436 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty158

  46. [46]

    Formation and evolution of hybrid He-CO white dwarfs and their properties

    Formation and evolution of hybrid He-CO white dwarfs and their properties. , keywords =. doi:10.1093/mnras/sty2723 , archivePrefix =. 1803.04444 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2723

  47. [47]

    , keywords =

    The formation of bipolar planetary nebulae and close white dwarf binaries. , keywords =. doi:10.1093/mnras/272.4.800 , adsurl =

    work page doi:10.1093/mnras/272.4.800

  48. [48]

    , keywords =

    A critical test of stellar evolution and convective core `overshooting' by means of zeta Aurigae systems. , keywords =. doi:10.1093/mnras/285.4.696 , adsurl =

    work page doi:10.1093/mnras/285.4.696

  49. [49]

    , keywords =

    Further critical tests of stellar evolution by means of double-lined eclipsing binaries. , keywords =. doi:10.1093/mnras/289.4.869 , adsurl =

    work page doi:10.1093/mnras/289.4.869

  50. [50]

    , year = 1971, month = jan, volume =

    The evolution of low mass stars. , year = 1971, month = jan, volume =. doi:10.1093/mnras/151.3.351 , adsurl =

    work page doi:10.1093/mnras/151.3.351 1971

  51. [51]

    , year = 1972, month = jan, volume =

    Composition changes during stellar evolution. , year = 1972, month = jan, volume =. doi:10.1093/mnras/156.3.361 , adsurl =

    work page doi:10.1093/mnras/156.3.361 1972

  52. [52]

    , year = 1973, month = jan, volume =

    A numerical treatment of double shell source stars. , year = 1973, month = jan, volume =. doi:10.1093/mnras/163.3.279 , adsurl =

    work page doi:10.1093/mnras/163.3.279 1973

  53. [53]

    2002 , Bdsk-Url-1 =

    The origin of subdwarf B stars - I. The formation channels. , keywords =. doi:10.1046/j.1365-8711.2002.05752.x , archivePrefix =. astro-ph/0206130 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05752.x 2002

  54. [54]

    , keywords =

    Measurements of general relativistic effects in the binary pulsar PSR1913 + 16. , keywords =. doi:10.1038/277437a0 , adsurl =

    work page doi:10.1038/277437a0

  55. [55]

    2013, ApJS, 208, 4, doi: 10.1088/0067-0049/208/1/4

    Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars. , keywords =. doi:10.1088/0067-0049/208/1/4 , archivePrefix =. 1301.0319 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/208/1/4

  56. [56]

    2015, ApJS, 220, 15, doi: 10.1088/0067-0049/220/1/15

    Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions. , keywords =. doi:10.1088/0067-0049/220/1/15 , archivePrefix =. 1506.03146 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/220/1/15

  57. [57]

    B., et al

    Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions. , keywords =. doi:10.3847/1538-4365/aaa5a8 , archivePrefix =. 1710.08424 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aaa5a8

  58. [58]

    Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation

    Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation. , keywords =. doi:10.3847/1538-4365/ab2241 , archivePrefix =. 1903.01426 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab2241 1903

  59. [59]

    , keywords =

    Stellar evolution models for Z = 0.0001 to 0.03. , keywords =. doi:10.1046/j.1365-8711.1998.01658.x , adsurl =

    work page doi:10.1046/j.1365-8711.1998.01658.x 1998

  60. [60]

    The shape of convective core overshooting from gravity-mode period spacings

    The shape of convective core overshooting from gravity-mode period spacings. , keywords =. doi:10.1051/0004-6361/201732317 , archivePrefix =. 1802.02051 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732317

  61. [61]

    , keywords =

    New Grids of Stellar Models from 0.8-SOLAR-MASS to 120-SOLAR-MASSES at Z=0.020 and Z=0.001. , keywords =

  62. [62]

    Subdwarf B stars from the common envelope ejection channel

    Subdwarf B stars from the common envelope ejection channel. , keywords =. doi:10.1051/0004-6361/201629622 , archivePrefix =. 1608.08739 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629622

  63. [63]

    Stellar wind models of subluminous hot stars

    Stellar wind models of subluminous hot stars. , keywords =. doi:10.1051/0004-6361/201628433 , archivePrefix =. 1607.04445 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628433

  64. [64]

    doi:10.1046/j.1365-8711.2000.03050.x , eprint =

    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 =

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

  65. [65]

    , year = 2009, month = sep, volume =

    Hot Subdwarf Stars. , year = 2009, month = sep, volume =. doi:10.1146/annurev-astro-082708-101836 , adsurl =

    work page doi:10.1146/annurev-astro-082708-101836 2009

  66. [66]

    The role of an outer tertiary on formation channels

    Forming hot subluminous stars from hierarchical triples - I. The role of an outer tertiary on formation channels. , keywords =. doi:10.1093/mnras/stac2798 , archivePrefix =. 2209.11327 , primaryClass =

    work page doi:10.1093/mnras/stac2798

  67. [67]

    An atlas of stellar spectra, with an outline of spectral classification

  68. [68]

    , year = 1939, month = may, volume =

    Two New White Dwarfs; Notes on Proper Motion Stars. , year = 1939, month = may, volume =. doi:10.1086/144075 , adsurl =

    work page doi:10.1086/144075 1939

  69. [69]

    A Survey of Stellar Families: Multiplicity of Solar-Type Stars

    A Survey of Stellar Families: Multiplicity of Solar-type Stars. , keywords =. doi:10.1088/0067-0049/190/1/1 , archivePrefix =. 1007.0414 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/190/1/1

  70. [70]

    2001 , Bdsk-Url-1 =

    On the variation of the initial mass function. , keywords =. doi:10.1046/j.1365-8711.2001.04022.x , archivePrefix =. astro-ph/0009005 , primaryClass =

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

  71. [71]

    , keywords =

    Evolutionary modelling of subdwarf B stars using MESA with the predictive mixing and convective pre-mixing schemes. , keywords =. doi:10.1093/mnras/staa3751 , archivePrefix =. 2011.14621 , primaryClass =

    work page doi:10.1093/mnras/staa3751 2011

  72. [72]

    , keywords =

    White dwarf binaries suggest a common envelope efficiency 1/3. , keywords =. doi:10.1093/mnras/stac3313 , archivePrefix =. 2211.02036 , primaryClass =

    work page doi:10.1093/mnras/stac3313

  73. [73]

    , keywords =

    On the Number-Mass Distribution of Degenerate Dwarfs Produced by the Interacting Binaries and Evidence for Mergers of Low-Mass Helium Dwarfs. , keywords =. doi:10.1086/164813 , adsurl =

    work page doi:10.1086/164813

  74. [74]

    , keywords =

    On the evolution of close binaries with components of initial mass between 3 M and 12 M. , keywords =. doi:10.1086/191054 , adsurl =

    work page doi:10.1086/191054

  75. [75]

    Exploring stellar evolution models of sdB stars using MESA

    Exploring Stellar Evolution Models of sdB Stars using MESA. , keywords =. doi:10.1088/0004-637X/806/2/178 , archivePrefix =. 1410.8204 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/806/2/178

  76. [76]

    arXiv e-prints , keywords =

    Normal type Ia supernovae from disruptions of hybrid He-CO white-dwarfs by CO white-dwarfs. arXiv e-prints , keywords =. doi:10.48550/arXiv.1910.07532 , archivePrefix =. 1910.07532 , primaryClass =

    work page doi:10.48550/arxiv.1910.07532 1910

  77. [77]

    Evolution of Low-Mass Helium Stars in Semidetached Binaries

    Evolution of low-mass helium stars in semidetached binaries. Astronomy Letters , keywords =. doi:10.1134/S1063773708090053 , archivePrefix =. 0804.2780 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1134/s1063773708090053

  78. [78]

    , year = 1984, month = feb, volume = 277, pages =

    Double white dwarfs as progenitors of R Coronae Borealis stars and Type I supernovae. , year = 1984, month = feb, volume = 277, pages =. doi:10.1086/161701 , adsurl =

    work page doi:10.1086/161701 1984

  79. [79]

    , year = 1958, month = may, volume =

    Study of the Hydrogen and Helium II Lines in a High-Temperature Subdwarf. , year = 1958, month = may, volume =. doi:10.1086/146496 , adsurl =

    work page doi:10.1086/146496 1958

  80. [80]

    , year = 1947, month = jan, volume =

    A Search for Faint Blue Stars. , year = 1947, month = jan, volume =. doi:10.1086/144884 , adsurl =

    work page doi:10.1086/144884 1947

Showing first 80 references.