Pith. sign in

REVIEW 4 major objections 6 minor 79 references

High Power Accretion in Massive Binary Systems and the Impact of Metallicity

T0 review · 4 major / 6 minor · reviewed 2026-08-04 · deepseek-v4-flash

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

Pith's one-line read Higher metallicity makes accreting companion stars brighten more, not less.

desk verdict Useful and reproducible MESA grid, but the metallicity trend is a 20-year snapshot, not a settled general law. read the letter →

arxiv 2509.10002 v1 pith:BLEWKBBQ submitted 2025-09-12 astro-ph.SR astro-ph.HE

Bhawna Mukhija , Amit Kashi This is my paper
classification astro-ph.SRastro-ph.HE
keywords massivestarsaccretionbinarysystemsmetallicitystellarevolutionenvelopeinflationluminositygianteruptions
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper simulates 20 and 30 solar-mass companion stars accreting at high rates during a giant eruption of their binary partner, across three metallicities (Galactic, LMC, SMC). It claims that for the same accretion rate and stellar mass, higher-metallicity stars show the largest accretion-driven luminosity increase, despite having larger radii. The paper attributes this to opacity: higher metallicity traps the released accretion energy more efficiently, boosting luminosity beyond what the radius alone predicts. It also finds that the transition from a hot, thermally stable accretor to a cool, inflated star occurs at a lower accretion rate for higher metallicity. A sympathetic reader would care because this metallicity dependence shifts the expected luminosity and evolutionary outcome of accretion events in massive binaries, with implications for interpreting eruptions and merger precursors.

What carries the argument

The accretion luminosity formula L_acc = G m Mdot / R, where m is stellar mass and R is radius, predicts that a larger radius suppresses luminosity increase, making the observed reversal the paper's central puzzle. The resolving mechanism is metallicity-dependent opacity: higher Z increases line blanketing and opacity in the outer layers, trapping energy released by accretion and delaying its escape, which produces a higher luminosity increase despite the larger radius. This opacity effect also lowers the Eddington accretion rate, causing the star to leave thermal equilibrium and inflate at a lower accretion rate when Z is higher.

What would settle it

A numerical simulation of the same accretion grid that includes jet-driven mass loss or a wind during accretion should show that the luminosity increase either shrinks or the metallicity ordering flips; alternatively, a observed giant-eruption binary in the LMC with a known accretor mass and accretion rate that shows a larger ΔlogL than a Galactic counterpart at the same rate would contradict the paper's claim.

Watch

Extended reading notes

Core claim

The central claim is that metallicity reverses the naive expectation for accretion luminosity in massive stars. For 20 and 30 solar-mass post-main-sequence stars accreting at rates from 10^-5 to 10^-2 solar masses per year, higher metallicity yields a larger increase in luminosity (ΔlogL) even though the star has a larger initial radius. For example, at 10^-2 solar masses per year the 20 solar-mass star's luminosity rises by ΔlogL ≈ 0.904 at Galactic metallicity, versus 0.855 at LMC and 0.863 at SMC. The paper explains this through metallicity-dependent opacity: higher opacity traps accretion energy in the outer layers, increasing radiative output despite the larger radius. Additionally, the

Load-bearing premise

The models assume zero mass loss and zero jets during the accretion phase, and ignore rotation, so the envelope inflates purely from mass accumulation; if real companions shed mass or launch jets, the inflation thresholds and luminosity ordering would not hold.

Editorial extensions

If this is right

  • If correct, the luminosity jump during a giant eruption accreted onto a companion will be systematically higher in Galactic environments than in the LMC or SMC, affecting how such events are identified and their distances estimated.
  • The threshold accretion rate for envelope inflation and possible common-envelope formation is metallicity-dependent, with higher metallicity binaries entering inflated states at lower mass-transfer rates.
  • Population synthesis models that assume a single thermal-timescale accretion threshold should incorporate a metallicity-dependent threshold to correctly predict which binaries merge or form common envelopes.
  • The finding connects accretion luminosity to composition, implying that observed transient luminosities may carry a metallicity fingerprint even when the accretor mass and rate are identical.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The paper's no-jets, no-mass-loss assumption is the main caveat; if the companion launches jets as proposed in other studies, the outer layers may be removed before inflation, and the metallicity ordering of luminosity increase could weaken or reverse.
  • A testable extension is to compute the same grid with rotation or with the accreted material's entropy treated self-consistently, since both can alter the envelope response and thereby shift the thresholds.
  • If high-Z accretors reach cooler inflated states at lower accretion rates, then in low-metallicity environments (e.g., early universe) the same binary configuration would require a higher accretion rate to trigger a common envelope, potentially changing merger rates of massive stellar remnants.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 6 minor

Summary. The paper simulates the response of 20 and 30 M_sun post-main-sequence stars to constant, high-rate accretion (10^-5 to 10^-2 M_sun/yr) at Galactic, LMC, and SMC metallicities, using MESA r23.05.1. A grid of 234 models is run for 20 years, with endpoint luminosity, radius, and temperature changes tabulated (Tables 3-4) and a Zenodo release (10.5281/zenodo.15682592). The main claims are: (1) at a given accretion rate, higher-metallicity stars show larger luminosity increases (up to DeltaLogL ~ 0.9 for 20 M_sun at Galactic Z and 10^-2 M_sun/yr) despite their larger radii, contrary to the naive expectation from L_acc = GM Mdot/R; and (2) the minimum accretion rate for the transition from a hot, near-equilibrium state to a cool inflated envelope decreases with metallicity (for 20 M_sun: ~3.44e-3 Galactic, ~5.08e-3 LMC, ~6.17e-3 SMC). The proposed mechanism is opacity trapping of accreted energy in the outer layers. The models neglect rotation, winds, and jets during accretion and assume the accreted material has the same composition and entropy as the surface layers.

Significance. If it holds, claim (1) overturns the simple radius-scaling expectation and identifies opacity as the controlling factor for the luminosity response to accretion; claim (2) provides a sharp, falsifiable prediction linking metallicity to the threshold for envelope inflation, with consequences for interpreting giant-eruption transients and for binary population synthesis. The study's strengths are the systematic parameter grid, fully tabulated results, and the publicly archived MESA inlists/data. The transition-rate ordering (Galactic < LMC < SMC) is consistent across both stellar masses and is the paper's most robust result. The DeltaLogL differences across metallicities are smaller and in one case (SMC vs LMC at 10^-2 for 20 M_sun) reversed, and the physical mechanism is asserted only qualitatively. All claims are also tied to a single 20-yr endpoint, far shorter than the envelope thermal timescale.

major comments (4)
  1. [§2.1, §3.1, Tables 3-4] The paper's central claim rests on the endpoints of a fixed 20-year accretion episode. The timestep justification in §2.1 compares to the dynamical timescale (tdyn ~ 5x10^3 s), but the relevant relaxation timescale for the envelope response that sets logR and logDeltaL is the thermal (Kelvin-Helmholtz) time, ~10^3-10^4 yr for these stars. Thus the reported DeltaLogL values and transition thresholds are transient values, and no duration-convergence test is presented. A longer (or shorter) episode could change the ranking; indeed at 10^-2 the 20 M_sun SMC model (0.863) already exceeds LMC (0.855). I request a duration-convergence test (e.g., selected runs to 10^2-10^3 yr) or an explicit, consistently applied scoping of all claims to 'the end of a 20-yr event.'
  2. [§3.2, Eq. (1)] The explanation that higher metallicity raises opacity, traps accreted energy, and thereby increases DeltaLogL despite a larger radius is qualitative. No quantitative diagnostic is shown: no opacity or radiative-diffusion timescale profiles across Z, and no control run (e.g., artificially flattened opacity) isolating the trapping effect. Since the inter-metallicity differences in Table 3 can be as small as ~0.01 dex, this is not a self-evident mechanism. Please add a quantitative measure of the trapping timescale for each metallicity and show that it correlates with the computed DeltaLogL, or soften the causal claim in §3.2 and the Abstract.
  3. [§3.3, Table 3] The stated trend 'higher metallicity -> greater variations in accretion luminosity' is not monotonic in Table 3 for the 20 M_sun star at the highest accretion rate: DeltaLogL = 0.904 (Galactic), 0.855 (LMC), 0.863 (SMC), so SMC exceeds LMC by 0.008 dex. This inversion is not discussed. The transition-rate ordering (Galactic < LMC < SMC) is well supported and is the paper's strongest claim; the DeltaLogL ordering needs either a numerical-convergence check or a caveat in the Abstract.
  4. [§2.2] The models assume zero wind mass loss, zero jets, and zero rotation during accretion. The paper cites Bear & Soker (2024) and Scolnic et al. (2025), who argue that jet-driven mass loss can remove high-entropy outer layers and prevent envelope inflation; under that mechanism the reported DeltaL values and threshold rates, including their metallicity ordering, would not apply to real binaries. This is disclosed as a simplification, but the Discussion (Sec. 4) does not address how the jet/mass-loss scenario would alter the metallicity dependence. Please add an explicit statement of the applicability regime and a qualitative discussion of the jet case.
minor comments (6)
  1. [§3.3 (both 20 and 30 M_sun paragraphs)] The sentence 'the star at SMC metallicity becomes cooler and inflates only for the accretion rates 10^-2, and it remains a hotter star for the accretion rates 4x10^-3, 6x10^-3, and 10^-2' contains a contradiction: the final '10^-2' should be '10^-4' (or removed).
  2. [Tables 3-4] Several entries are garbled ('0.0.960', '01.023', '22.176' for 30 M_sun Galactic at 9x10^-3). The caption states Mdot in 10^-3 M_sun/yr while the first rows are 10^-2 and 10^-1; please clarify that tabulated values are to be multiplied by 10^-3.
  3. [§2.1, Fig. 2] The text says 234 accretion points are simulated; Fig. 2 says 'all 239 runs.' 39 rates x 3 metallicities x 2 masses = 234; the '239' appears to be a typo.
  4. [§3.1] The 'four distinct jumps' are successive refinements of a single transition rate (e.g., 3.43-3.44e-3 for Galactic 20 M_sun). Consider describing this as one transition bracketed first at 10^-3-10^-2 and then localized by grid refinement.
  5. [§2.2] The phrase 'opacity table of type II OPAL which allows for time-dependent variation in the metal abundance' is imprecise; type II tables allow a separate composition for opacity (e.g., time-independent metal scaling), not a time-dependent abundance. Please rephrase.
  6. [§2.1, Eq. (1)] A quantitative comparison between the MESA-computed DeltaL at the quoted rates and L_acc = GM Mdot/R would be valuable; the current text leaves the relationship implicit.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the metallicity comparison is new MESA simulation output, and the self-citations are contextual, not load-bearing.

full rationale

The central claim—that at fixed Mdot higher-Z companions show larger log DeltaL and transition from hot to cool at lower accretion rates—is produced by evolving 20 and 30 Msun MESA models at Z=0.02, 0.008, 0.004 with accretion rates 1e-5 to 1e-2 Msun/yr. Eq. (1) (Lacc=GmMdot/R) is the standard energy-injection formula used by MESA; the reported result runs opposite to the naive inverse-radius expectation (at the final state the Galactic star has the largest radius, which per Eq. 1 would give the smallest DeltaL), so the output is not a restatement of the input formula. No parameter is fitted to the target result, and the threshold accretion rates are read from the MESA final profiles rather than imposed. The paper cites Mukhija & Kashi (2025) for the previous accretion grid and for the qualitative hot/cool dichotomy, and Kashi & Soker (2010b) for the order-of-magnitude luminosity context, but these citations are not used to derive or force the metallicity ordering; the inlists are available on Zenodo for independent reproduction. The omitted mass loss/jets/rotation and the fixed 20-yr accretion window are acknowledged modeling limitations (Sec. 2.2 and Sec. 4), not circular steps: they affect realism and time-convergence of the reported DeltaL values, but they do not make the simulation output equivalent to its inputs by definition. Therefore no circularity step can be exhibited.

Assumptions & free parameters 6 free parameters · 6 assumptions · 0 invented entities

The central claim rests on a suite of standard MESA microphysics choices and explicit physical assumptions. None of these are fitted to the target result; they are chosen from the cited literature. The absence of mass loss/jets and the fixed accretion duration are the most consequential premises.

free parameters (6)
  • mixing_length_parameter = 1.5
    Chosen from literature (Henyey et al. 1965); affects envelope structure and radius, which drives the accretion luminosity response.
  • semiconvection_efficiency = 0.01
    Langer et al. 1985; affects mixing and core evolution, indirectly the post-MS structure.
  • overshoot_parameters = f1=0.005, f0=0.001
    Herwig 2000; determines core size and post-MS starting point.
  • wind_scaling_factor = 0.5
    Zhao & Fuller 2020; reduces mass loss, affects the mass at accretion start.
  • accretion_duration = 20 yr
    Chosen by hand; a longer or shorter burst would change how much the star relaxes.
  • accreted_entropy_ratio = 1:1 with surface entropy
    Assumed equal to surface entropy (following Paxton et al. 2015); controls the thermal response of the envelope.
assumptions (6)
  • domain assumption MESA r23.05.1 correctly solves the 1D stellar structure equations for these accretion timescales.
    The whole paper rests on the code's fidelity for rapid accretion onto massive stars.
  • domain assumption The accretion luminosity formula L_acc = G m Mdot / R (Eq. 1) captures the immediate energy release.
    Taken from Lau et al. 2024; used to interpret the simulation output.
  • domain assumption The accreted material has the same chemical composition as the stellar surface.
    Stated in Section 2.2 and revisited in Section 4; donor surface may differ.
  • domain assumption No mass loss or jet-driven outflow occurs during accretion.
    Stated in Section 2.2; excludes the Bear & Soker (2024) and Scolnic et al. (2025) mechanism that could prevent inflation.
  • domain assumption The accretion rate is constant over the 20-year period.
    Stated in Section 2.1; real giant eruption accretion rates vary with orbital phase.
  • domain assumption The star is non-rotating and accreted angular momentum is ignored.
    Stated in Section 2.2; rotation would spin the star to critical and cause mixing.

how reviews work

0 comments
Cite this review

Pith. "Pith review of High Power Accretion in Massive Binary Systems and the Impact of Metallicity." pith.science (2026). https://pith.science/paper/BLEWKBBQ

@misc{pith2026250910002,
  author       = {Pith},
  title        = {Pith review of: High Power Accretion in Massive Binary Systems and the Impact of Metallicity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BLEWKBBQ}},
  note         = {Machine review of arXiv:2509.10002}
}
abstract

During a giant eruption of a very massive star in the binary system, the companion star can accrete a large amount of mass that can change its properties and potentially its subsequent evolution. The effect depends on the companion mass, metallicity, the amount of mass it accreted, orbital parameters and other parameters. We simulate individual companion stars assuming they undergo such accretion events. We study the envelope properties of 20 $\rm M_\odot$ and 30 $\rm M_\odot$ single massive stars at different matallicities ($Z= 0.02$, $Z=0.008$ and $Z=0.004$) during accretion at different rates, from $\rm 10^{-5}$ to $\rm 10^{-2}~M_\odot\,yr^{-1}$. For the lower accretion rates we simulate, the stars remains hot, while at higher accretion rates, it becomes cooler and inflates. This behavior is observed in both stars but occurs at different accretion rates. Higher metallicity stars exhibit greater variations in accretion luminosity for the same accretion rate and stellar mass compared to lower metallicity stars. While higher metallicity stars typically have larger stellar envelopes, suggesting smaller variations in luminosity at Galactic metallicity compared to the LMC and SMC, our results show the opposite.

Figures

Figures reproduced from arXiv: 2509.10002 by the authors.

Figure 1
Figure 1. The evolutionary tracks of 20 and 30 M⊙ stars at Galactic, LMC, and SMC metallicities, spanning from the ZAMS to the helium-core burning phase. Points A, A’, and A” mark the initiation of accretion for the 20 M⊙, while points B, B’, and B” represent the initiation of accretion for the 30 M⊙ star. metallicity (Z=0.02), A’ to LMC metallicity (Z=0.008), and A" to SMC metallicity (Z=0.004). These points highlight how th… view at source ↗
Figure 2
Figure 2. Panels (a) and (b) show the increased luminosity ( [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. The variation in luminosity L (row 1), radii R (row 2), and temperature Teff (row 3) of the 20 M⊙ star at Galactic (column 1), LMC (column 2) and SMC (column 3) metallicities during the mass accretion process, respectively. At Galactic for M˙ acc = 10−4 M⊙ yr−1 the star remains on the blue side of the H-R diagram and becomes hotter, while for 4 × 10−3 , 6 × 10−3 , and 10−2 M⊙ yr−1 accretion rates star becomes a cool… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Same as Figure 3, but for the 30 M [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

79 extracted references · 5 canonical work pages

  1. [1]

    , author Harrison , F.A

    author Bachetti , M. , author Harrison , F.A. , author Walton , D.J. , author Grefenstette , B.W. , author Chakrabarty , D. , author F \"u rst , F. , author Barret , D. , author Beloborodov , A. , author Boggs , S.E. , author Christensen , F.E. , author Craig , W.W. , author Fabian , A.C. , author Hailey , C.J. , author Hornschemeier , A. , author Kaspi ,...

    arXiv 2014

  2. [2]

    , author El Eid , M.F

    author Baraffe , I. , author El Eid , M.F. , year 1991 . title Evolution of massive stars with variable initial compositions . journal volume 245 , pages 548--560

    1991

  3. [3]

    On the response of massive main sequence stars to mass accretion and outflow at high rates

    author Bear , E. , author Soker , N. , year 2024 . title On the response of massive main sequence stars to mass accretion and outflow at high rates . journal arXiv e-prints , pages arXiv:2407.03182 :10.48550/arXiv.2407.03182, http://arxiv.org/abs/2407.03182 arXiv:2407.03182

    work page Pith review arXiv doi:10.48550/arxiv.2407.03182 2024

  4. [4]

    , author Soderberg , A.M

    author Berger , E. , author Soderberg , A.M. , author Chevalier , R.A. , author Fransson , C. , author Foley , R.J. , author Leonard , D.C. , author Debes , J.H. , author Diamond-Stanic , A.M. , author Dupree , A.K. , author Ivans , I.I. , author Simmerer , J. , author Thompson , I.B. , author Tremonti , C.A. , year 2009 . title An Intermediate Luminosity...

    arXiv 2009

  5. [5]

    , author de Mink , S.E

    author Brott , I. , author de Mink , S.E. , author Cantiello , M. , author Langer , N. , author de Koter , A. , author Evans , C.J. , author Hunter , I. , author Trundle , C. , author Vink , J.S. , year 2011 . title Rotating massive main-sequence stars. I. Grids of evolutionary models and isochrones . journal volume 530 , pages A115 . :10.1051/0004-6361/2...

    arXiv 2011

  6. [6]

    , author Truran , J.W

    author Brunish , W.M. , author Truran , J.W. , year 1982 . title The evolution of massive stars. II. The influence of initial composition and mass loss. journal volume 49 , pages 447--468 . :10.1086/190806

    work page doi:10.1086/190806 1982

  7. [7]

    , author Langer , N

    author de Mink , S.E. , author Langer , N. , author Izzard , R.G. , author Sana , H. , author de Koter , A. , year 2013 . title The Rotation Rates of Massive Stars: The Role of Binary Interaction through Tides, Mass Transfer, and Mergers . journal volume 764 , pages 166 . :10.1088/0004-637X/764/2/166, http://arxiv.org/abs/1211.3742 arXiv:1211.3742

    arXiv 2013

  8. [8]

    , author Ekstr \"o m , S

    author Georgy , C. , author Ekstr \"o m , S. , author Eggenberger , P. , author Meynet , G. , author Haemmerl \'e , L. , author Maeder , A. , author Granada , A. , author Groh , J.H. , author Hirschi , R. , author Mowlavi , N. , author Yusof , N. , author Charbonnel , C. , author Decressin , T. , author Barblan , F. , year 2013 . title Grids of stellar mo...

    arXiv 2013

Show all 79 references
  1. [9]

    , author Ekstr \"o m , S

    author Groh , J.H. , author Ekstr \"o m , S. , author Georgy , C. , author Meynet , G. , author Choplin , A. , author Eggenberger , P. , author Hirschi , R. , author Maeder , A. , author Murphy , L.J. , author Boian , I. , author Farrell , E.J. , year 2019 . title Grids of ste...

    2019 arXiv

  2. [10]

    , author Langer , N

    author Heger , A. , author Langer , N. , author Woosley , S.E. , year 2000 . title Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure . journal volume 528 , pages 368--396 . :10.1086/308158, http://arxiv.org/ab...

    2000 arXiv

  3. [11]

    , author Woosley , S.E

    author Heger , A. , author Woosley , S.E. , author Spruit , H.C. , year 2005 . title Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields . journal volume 626 , pages 350--363 . :10.1086/429868, http://arxiv.org/abs/astro-ph/0409422 arXiv:a...

    2005 arXiv

  4. [12]

    , author Vardya , M.S

    author Henyey , L. , author Vardya , M.S. , author Bodenheimer , P. , year 1965 . title Studies in Stellar Evolution. III. The Calculation of Model Envelopes. journal volume 142 , pages 841 . :10.1086/148357

    1965 doi

  5. [13]

    , year 2000

    author Herwig , F. , year 2000 . title The evolution of AGB stars with convective overshoot . journal volume 360 , pages 952--968 . :10.48550/arXiv.astro-ph/0007139, http://arxiv.org/abs/astro-ph/0007139 arXiv:astro-ph/0007139

    2000 doi arXiv

  6. [14]

    , author Taam , R.E

    author Hjellming , M.S. , author Taam , R.E. , year 1991 . title The Response of Main-Sequence Stars within a Common Envelope . journal volume 370 , pages 709 . :10.1086/169854

    1991 doi

  7. [15]

    , year 1971

    author Hunt , R. , year 1971 . title A fluid dynamical study of the accretion process . journal volume 154 , pages 141 . :10.1093/mnras/154.2.141

    1971 doi

  8. [16]

    , author Tout , C.A

    author Hurley , J.R. , author Tout , C.A. , author Pols , O.R. , year 2002 . title Evolution of binary stars and the effect of tides on binary populations . journal volume 329 , pages 897--928 . :10.1046/j.1365-8711.2002.05038.x, http://arxiv.org/abs/astro-ph/0201220 arXiv:ast...

    2002

  9. [17]

    , author Rogers , F.J

    author Iglesias , C.A. , author Rogers , F.J. , year 1996 . title Updated Opal Opacities . journal volume 464 , pages 943 . :10.1086/177381

    1996 doi

  10. [18]

    , author Ueno , M

    author Ishii , M. , author Ueno , M. , author Kato , M. , year 1999 . title Core-Halo Structure of a Chemically Homogeneous Massive Star and Bending of the Zero-Age Main Sequence . journal volume 51 , pages 417--424 . :10.1093/pasj/51.4.417, http://arxiv.org/abs/astro-ph/99071...

    1999 arXiv

  11. [19]

    , author Justham , S

    author Ivanova , N. , author Justham , S. , author Chen , X. , author De Marco , O. , author Fryer , C.L. , author Gaburov , E. , author Ge , H. , author Glebbeek , E. , author Han , Z. , author Li , X.D. , author Lu , G. , author Marsh , T. , author Podsiadlowski , P. , autho...

    2013 arXiv

  12. [20]

    , year 2010

    author Kashi , A. , year 2010 . title An indication for the binarity of P Cygni from its 17th century eruption . journal volume 405 , pages 1924--1929 . :10.1111/j.1365-2966.2010.16582.x, http://arxiv.org/abs/0912.3998 arXiv:0912.3998

    2010

  13. [21]

    , author Frankowski , A

    author Kashi , A. , author Frankowski , A. , author Soker , N. , year 2010 . title NGC 300 OT2008-1 as a Scaled-down Version of the Eta Carinae Great Eruption . journal volume 709 , pages L11--L15 . :10.1088/2041-8205/709/1/L11, http://arxiv.org/abs/0909.1909 arXiv:0909.1909

    2010 arXiv

  14. [22]

    , author Michaelis , A

    author Kashi , A. , author Michaelis , A. , author Kaminetsky , Y. , year 2022 . title Accretion in massive colliding-wind binaries and the effect of the wind momentum ratio . journal volume 516 , pages 3193--3205 . :10.1093/mnras/stac1912, http://arxiv.org/abs/2207.01990 arXi...

    2022 arXiv

  15. [23]

    , author Soker , N

    author Kashi , A. , author Soker , N. , year 2010 a. title Common Powering Mechanism of Intermediate Luminosity Optical Transients and Luminous Blue Variables . journal arXiv e-prints , pages arXiv:1011.1222 :10.48550/arXiv.1011.1222, http://arxiv.org/abs/1011.1222 arXiv:1011.1222

    2010 doi arXiv

  16. [24]

    , author Soker , N

    author Kashi , A. , author Soker , N. , year 2010 b. title Periastron Passage Triggering of the 19th Century Eruptions of Eta Carinae . journal volume 723 , pages 602--611 . :10.1088/0004-637X/723/1/602, http://arxiv.org/abs/0912.1439 arXiv:0912.1439

    2010 arXiv

  17. [25]

    , author Soker , N

    author Kashi , A. , author Soker , N. , year 2016 . title Operation of the jet feedback mechanism (JFM) in intermediate luminosity optical transients (ILOTs) . journal Research in Astronomy and Astrophysics volume 16 , pages 99 . :10.1088/1674-4527/16/6/099, http://arxiv.org/a...

    2016 arXiv

  18. [26]

    , author Soker , N

    author Kashi , A. , author Soker , N. , author Moskovitz , N. , year 2013 . title Powering the second 2012 outburst of SN 2009ip by repeating binary interaction . journal volume 436 , pages 2484--2491 . :10.1093/mnras/stt1742, http://arxiv.org/abs/1307.7681 arXiv:1307.7681

    2013 arXiv

  19. [27]

    , author Meyer-Hofmeister , E

    author Kippenhahn , R. , author Meyer-Hofmeister , E. , year 1977 . title On the radii of accreting main sequence stars. journal volume 54 , pages 539--542

    1977

  20. [28]

    , author Ruschenplatt , G

    author Kippenhahn , R. , author Ruschenplatt , G. , author Thomas , H.C. , year 1980 . title The time scale of thermohaline mixing in stars . journal volume 91 , pages 175--180

    1980

  21. [29]

    , author Weigert , A

    author Kippenhahn , R. , author Weigert , A. , author Weiss , A. , year 2013 . title Stellar Structure and Evolution . :10.1007/978-3-642-30304-3

    2013 doi

  22. [30]

    , author El Eid , M.F

    author Langer , N. , author El Eid , M.F. , author Fricke , K.J. , year 1985 . title Evolution of massive stars with semiconvective diffusion . journal volume 145 , pages 179--191

    1985

  23. [31]

    , author Yoon , S.C

    author Langer , N. , author Yoon , S.C. , author Petrovic , J. , author Heger , A. , year 2003 . title Binary evolution models with rotation . journal arXiv e-prints , pages astro--ph/0302232 :10.48550/arXiv.astro-ph/0302232, http://arxiv.org/abs/astro-ph/0302232 arXiv:astro-p...

    2003 doi

  24. [32]

    , author Hirai , R

    author Lau , M.Y.M. , author Hirai , R. , author Mandel , I. , author Tout , C.A. , year 2024 . title Expansion of Accreting Main-sequence Stars during Rapid Mass Transfer . journal volume 966 , pages L7 . :10.3847/2041-8213/ad3d50, http://arxiv.org/abs/2401.09570 arXiv:2401.09570

    2024 arXiv

  25. [33]

    , author Sari , R

    author Linial , I. , author Sari , R. , year 2017 . title Mass-loss through the L2 Lagrange point - application to main-sequence EMRI . journal volume 469 , pages 2441--2454 . :10.1093/mnras/stx1041, http://arxiv.org/abs/1705.01435 arXiv:1705.01435

    2017 arXiv

  26. [34]

    , author Pappas , K.M.W

    author Marchant , P. , author Pappas , K.M.W. , author Gallegos-Garcia , M. , author Berry , C.P.L. , author Taam , R.E. , author Kalogera , V. , author Podsiadlowski , P. , year 2021 . title The role of mass transfer and common envelope evolution in the formation of merging b...

    2021 arXiv

  27. [35]

    , author Girardi , L

    author Marigo , P. , author Girardi , L. , author Chiosi , C. , author Wood , P.R. , year 2001 . title Zero-metallicity stars. I. Evolution at constant mass . journal volume 371 , pages 152--173 . :10.1051/0004-6361:20010309, http://arxiv.org/abs/astro-ph/0102253 arXiv:astro-p...

    2001 arXiv

  28. [36]

    , author Fragos , T

    author Misra , D. , author Fragos , T. , author Tauris , T.M. , author Zapartas , E. , author Aguilera-Dena , D.R. , year 2020 . title The origin of pulsating ultra-luminous X-ray sources: Low- and intermediate-mass X-ray binaries containing neutron star accretors . journal vo...

    2020 arXiv

  29. [37]

    , author Kashi , A

    author Mukhija , B. , author Kashi , A. , year 2024 . title Giant Eruptions in Massive Stars and their Effect on the Stellar Structure . journal volume 974 , pages 124 . :10.3847/1538-4357/ad7398, http://arxiv.org/abs/2408.01718 arXiv:2408.01718

    2024 arXiv

  30. [38]

    , author Kashi , A

    author Mukhija , B. , author Kashi , A. , year 2025 . title Accretion and Recovery in Giant Eruptions of Massive Stars . journal volume 986 , pages 188 . :10.3847/1538-4357/add3f1, http://arxiv.org/abs/2504.19884 arXiv:2504.19884

    2025 arXiv

  31. [39]

    , author Narayan , G

    author Muthukrishna , D. , author Narayan , G. , author Mandel , K.S. , author Biswas , R. , author Hlo z ek , R. , year 2019 . title RAPID: Early Classification of Explosive Transients Using Deep Learning . journal volume 131 , pages 118002 . :10.1088/1538-3873/ab1609, http:/...

    2019 arXiv

  32. [40]

    , author Ivanova , N

    author Nandez , J.L.A. , author Ivanova , N. , author Lombardi , J. C., J. , year 2014 . title V1309 Sco Understanding a Merger . journal volume 786 , pages 39 . :10.1088/0004-637X/786/1/39, http://arxiv.org/abs/1311.6522 arXiv:1311.6522

    2014 arXiv

  33. [41]

    , author Miyaji , S

    author Neo , S. , author Miyaji , S. , author Nomoto , K. , author Sugimoto , D. , year 1977 . title Effect of Rapid Mass Accretion onto the Main-Sequence Stars . journal volume 29 , pages 249--262

    1977

  34. [42]

    , editor Lamers , H

    editor Nota , A. , editor Lamers , H. (Eds.), year 1997 . title Luminous Blue Variables: Massive Stars in Transition . volume volume 120 of series Astronomical Society of the Pacific Conference Series

    1997

  35. [43]

    , author Rybicki , G.B

    author Owocki , S.P. , author Rybicki , G.B. , year 1984 . title Instabilities in line-driven stellar winds. I. Dependence on perturbation wavelength. journal volume 284 , pages 337--350 . :10.1086/162412

    1984 doi

  36. [44]

    , year 1981

    author Packet , W. , year 1981 . title On the spin-up of the mass accreting component in a close binary system . journal volume 102 , pages 17--19

    1981

  37. [45]

    , year 1971

    author Paczy \'n ski , B. , year 1971 . title Evolutionary Processes in Close Binary Systems . journal volume 9 , pages 183 . :10.1146/annurev.aa.09.090171.001151

    1971

  38. [46]

    , author Bildsten , L

    author Paxton , B. , author Bildsten , L. , author Dotter , A. , author Herwig , F. , author Lesaffre , P. , author Timmes , F. , year 2011 . title Modules for Experiments in Stellar Astrophysics (MESA) . journal volume 192 , pages 3 . :10.1088/0067-0049/192/1/3, http://arxiv....

    2011 arXiv

  39. [47]

    , author Cantiello , M

    author Paxton , B. , author Cantiello , M. , author Arras , P. , author Bildsten , L. , author Brown , E.F. , author Dotter , A. , author Mankovich , C. , author Montgomery , M.H. , author Stello , D. , author Timmes , F.X. , author Townsend , R. , year 2013 . title Modules fo...

    2013 arXiv

  40. [48]

    , author Marchant , P

    author Paxton , B. , author Marchant , P. , author Schwab , J. , author Bauer , E.B. , author Bildsten , L. , author Cantiello , M. , author Dessart , L. , author Farmer , R. , author Hu , H. , author Langer , N. , author Townsend , R.H.D. , author Townsley , D.M. , author Tim...

    2015 arXiv

  41. [49]

    , author Schwab , J

    author Paxton , B. , author Schwab , J. , author Bauer , E.B. , author Bildsten , L. , author Blinnikov , S. , author Duffell , P. , author Farmer , R. , author Goldberg , J.A. , author Marchant , P. , author Sorokina , E. , author Thoul , A. , author Townsend , R.H.D. , autho...

    2018 arXiv

  42. [50]

    , author Smolec , R

    author Paxton , B. , author Smolec , R. , author Schwab , J. , author Gautschy , A. , author Bildsten , L. , author Cantiello , M. , author Dotter , A. , author Farmer , R. , author Goldberg , J.A. , author Jermyn , A.S. , author Kanbur , S.M. , author Marchant , P. , author T...

    2019 arXiv

  43. [51]

    , author Langer , N

    author Petrovic , J. , author Langer , N. , author van der Hucht , K.A. , year 2005 . title Constraining the mass transfer in massive binaries through progenitor evolution models of Wolf-Rayet+O binaries . journal volume 435 , pages 1013--1030 . :10.1051/0004-6361:20042368, ht...

    2005 arXiv

  44. [52]

    , author Walton , D.J

    author Pinto , C. , author Walton , D.J. , year 2023 . title Ultra-luminous X-ray sources: extreme accretion and feedback . journal arXiv e-prints , pages arXiv:2302.00006 :10.48550/arXiv.2302.00006, http://arxiv.org/abs/2302.00006 arXiv:2302.00006

    2023 doi arXiv

  45. [53]

    , author Cote , J

    author Pols , O.R. , author Cote , J. , author Waters , L.B.F.M. , author Heise , J. , year 1991 . title The formation of Be stars through close binary evolution. journal volume 241 , pages 419

    1991

  46. [54]

    , author Schroeder , K.P

    author Pols , O.R. , author Schroeder , K.P. , author Hurley , J.R. , author Tout , C.A. , author Eggleton , P.P. , year 2009 . title VizieR Online Data Catalog: Stellar evolution models for Z = 0.0001 to 0.03 (Pols+ 1998) . howpublished VizieR On-line Data Catalog: J/MNRAS/29...

    2009

  47. [55]

    , author Verbunt , F

    author Portegies Zwart , S.F. , author Verbunt , F. , year 1996 . title Population synthesis of high-mass binaries. journal volume 309 , pages 179--196

    1996

  48. [56]

    , year 1981

    author Pringle , J.E. , year 1981 . title Accretion discs in astrophysics . journal volume 19 , pages 137--162 . :10.1146/annurev.aa.19.090181.001033

    1981

  49. [57]

    , author Marchant , P

    author Qin , Y. , author Marchant , P. , author Fragos , T. , author Meynet , G. , author Kalogera , V. , year 2019 . title On the Origin of Black Hole Spin in High-mass X-Ray Binaries . journal volume 870 , pages L18 . :10.3847/2041-8213/aaf97b, http://arxiv.org/abs/1810.1301...

    2019 arXiv

  50. [58]

    , author Fern \'a ndez , R

    author Quataert , E. , author Fern \'a ndez , R. , author Kasen , D. , author Klion , H. , author Paxton , B. , year 2016 . title Super-Eddington stellar winds driven by near-surface energy deposition . journal volume 458 , pages 1214--1233 . :10.1093/mnras/stw365, http://arxi...

    2016 arXiv

  51. [59]

    , author G \"o tberg , Y

    author Renzo , M. , author G \"o tberg , Y. , year 2021 . title Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling Ophiuchi . journal volume 923 , pages 277 . :10.3847/1538-4357/ac29c5, http://arxiv.org/abs/2107.10933 arXiv:2107.10933

    2021 arXiv

  52. [60]

    , author Grassitelli , L

    author Sanyal , D. , author Grassitelli , L. , author Langer , N. , author Bestenlehner , J.M. , year 2015 . title Massive main-sequence stars evolving at the Eddington limit . journal volume 580 , pages A20 . :10.1051/0004-6361/201525945, http://arxiv.org/abs/1506.02997 arXiv...

    2015 arXiv

  53. [61]

    , author Langer , N

    author Sanyal , D. , author Langer , N. , author Sz \'e csi , D. , author -C Yoon , S. , author Grassitelli , L. , year 2017 . title Metallicity dependence of envelope inflation in massive stars . journal volume 597 , pages A71 . :10.1051/0004-6361/201629612, http://arxiv.org/...

    2017 arXiv

  54. [62]

    , author Langer , N

    author Schootemeijer , A. , author Langer , N. , author Grin , N.J. , author Wang , C. , year 2019 . title Constraining mixing in massive stars in the Small Magellanic Cloud . journal volume 625 , pages A132 . :10.1051/0004-6361/201935046, http://arxiv.org/abs/1903.10423 arXiv...

    2019 arXiv

  55. [63]

    , author Langer , N

    author Sch \"u rmann , C. , author Langer , N. , year 2024 . title Exploring the borderline between stable mass transfer and mergers in close binary evolution . journal arXiv e-prints , pages arXiv:2404.08615 :10.48550/arXiv.2404.08615, http://arxiv.org/abs/2404.08615 arXiv:2404.08615

    2024 doi arXiv

  56. [64]

    , author Bear , E

    author Scolnic , A. , author Bear , E. , author Soker , N. , year 2025 . title Enabling high mass accretion rates onto massive main sequence stars by outer envelope mass removal . journal Open Journal of Astrophysics

    2025

  57. [65]

    , author Langer , N

    author Sen , K. , author Langer , N. , author Marchant , P. , author Menon , A. , author de Mink , S.E. , author Schootemeijer , A. , author Sch \"u rmann , C. , author Mahy , L. , author Hastings , B. , author Nathaniel , K. , author Sana , H. , author Wang , C. , author Xu ,...

    2022

  58. [66]

    , author Li , X.D

    author Shao , Y. , author Li , X.D. , year 2014 . title On the Formation of Be Stars through Binary Interaction . journal volume 796 , pages 37 . :10.1088/0004-637X/796/1/37, http://arxiv.org/abs/1410.0100 arXiv:1410.0100

    2014 arXiv

  59. [67]

    , author Li , X.D

    author Shao , Y. , author Li , X.D. , year 2016 . title Nonconservative Mass Transfer in Massive Binaries and the Formation of Wolf-Rayet+O Binaries . journal volume 833 , pages 108 . :10.3847/1538-4357/833/1/108, http://arxiv.org/abs/1610.04307 arXiv:1610.04307

    2016 arXiv

  60. [68]

    , author Schreier , R

    author Shiber , S. , author Schreier , R. , author Soker , N. , year 2016 . title Binary interactions with high accretion rates onto main sequence stars . journal Research in Astronomy and Astrophysics volume 16 , pages 117 . :10.1088/1674-4527/16/7/117, http://arxiv.org/abs/1...

    2016 arXiv

  61. [69]

    , year 2001

    author Soker , N. , year 2001 . title The departure of Carinae from axisymmetry and the binary hypothesis . journal volume 325 , pages 584--588 . :10.1046/j.1365-8711.2001.04439.x, http://arxiv.org/abs/astro-ph/0103033 arXiv:astro-ph/0103033

    2001

  62. [70]

    , year 2017

    author Soker , N. , year 2017 . title Energizing the last phase of common-envelope removal . journal volume 471 , pages 4839--4843 . :10.1093/mnras/stx1978, http://arxiv.org/abs/1706.03720 arXiv:1706.03720

    2017 arXiv

  63. [71]

    , year 2020

    author Soker , N. , year 2020 . title Shaping Planetary Nebulae with Jets and the Grazing Envelope Evolution . journal Galaxies volume 8 , pages 26 . :10.3390/galaxies8010026, http://arxiv.org/abs/2002.04229 arXiv:2002.04229

    2020 arXiv

  64. [72]

    , year 2023

    author Soker , N. , year 2023 . title On the nature of the planet-powered transient event ZTF SLRN-2020 . journal volume 524 , pages L94--L97 . :10.1093/mnrasl/slad086, http://arxiv.org/abs/2305.04909 arXiv:2305.04909

    2023 arXiv

  65. [73]

    , author Pols , O.R

    author Temmink , K.D. , author Pols , O.R. , author Justham , S. , author Istrate , A.G. , author Toonen , S. , year 2023 . title Coping with loss. Stability of mass transfer from post-main-sequence donor stars . journal volume 669 , pages A45 . :10.1051/0004-6361/202244137, h...

    2023 arXiv

  66. [74]

    , author Nelemans , G

    author Toonen , S. , author Nelemans , G. , author Portegies Zwart , S. , year 2012 . title Supernova Type Ia progenitors from merging double white dwarfs. Using a new population synthesis model . journal volume 546 , pages A70 . :10.1051/0004-6361/201218966, http://arxiv.org/...

    2012 arXiv

  67. [75]

    , author Hajduk , M

    author Tylenda , R. , author Hajduk , M. , author Kami \'n ski , T. , author Udalski , A. , author Soszy \'n ski , I. , author Szyma \'n ski , M.K. , author Kubiak , M. , author Pietrzy \'n ski , G. , author Poleski , R. , author Wyrzykowski , . , author Ulaczyk , K. , year 20...

    2011 arXiv

  68. [76]

    , author de Mink , S.E

    author van Son , L.A.C. , author de Mink , S.E. , author Callister , T. , author Justham , S. , author Renzo , M. , author Wagg , T. , author Broekgaarden , F.S. , author Kummer , F. , author Pakmor , R. , author Mandel , I. , year 2022 . title The Redshift Evolution of the Bi...

    2022 arXiv

  69. [77]

    , author Neijssel , C.J

    author Vigna-G \'o mez , A. , author Neijssel , C.J. , author Stevenson , S. , author Barrett , J.W. , author Belczynski , K. , author Justham , S. , author de Mink , S.E. , author M \"u ller , B. , author Podsiadlowski , P. , author Renzo , M. , author Sz \'e csi , D. , autho...

    2018 arXiv

  70. [78]

    , author Fuller , J

    author Zhao , X. , author Fuller , J. , year 2020 . title Centrifugally driven mass-loss and outbursts of massive stars . journal volume 495 , pages 249--265 . :10.1093/mnras/staa1097, http://arxiv.org/abs/2004.07279 arXiv:2004.07279

    2020 arXiv

  71. [79]

    2015, , 579, A101

    Aladro, R., Martín, S., Riquelme, D., et al. 2015, , 579, A101

    2015

Pith tools

Reviewed August 4, 2026 · model on record in the stance chip above.