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Stellar evolution with rotation VI: The Eddington and Omega-limits, the rotational mass loss for OB and LBV stars

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Andre Maeder, Georges Meynet

Astrophysics · Submitted 28 Jun 2000

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The expression for the global mass loss-rates is a function of both $\Omega$ and $\Gamma$, and this may give raise to extreme mass loss-rates ($\Omega \Gamma $-limit).

how it is stated · hedged possibility 0.97 read the record →

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arXiv IDastro-ph/0006405 (version 1)
Pith IDVNGPJSJN, Pith's permanent record of this paper and its review
CitationAndre Maeder, Georges Meynet. "Stellar evolution with rotation VI: The Eddington and Omega-limits, the rotational mass loss for OB and LBV stars." arXiv:astro-ph/0006405 (2000). https://pith.science/paper/VNGPJSJN
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,394 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.16 · human participants 0.01 · controlled comparison 0.06 · randomized assignment 0.01 · states quantitative result 0.97 · compares with prior results 0.73 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

Several properties of massive stars with large effects of rotation and radiation are studied. We show that there are 2 roots for the equation giving the rotational velocities at break-up: 1) The usual solution, which is shown to apply when the Eddington ratio $\Gamma$ of the star is smaller than formally 0.639. 2) Above this value of $\Gamma$, there is a second root, inferior to the first one, for the break-up velocity. This second solution tends to zero, when $\Gamma$ tends towards 1. This second root results from the interplay of radiation and rotation, and in particular from the reduction by rotation of the effective mass in the local Eddington factor. The analysis made here should hopefully clarify a recent debate between Langer (\cite{La97,La98}) and Glatzel (\cite{Gla98}). The expression for the global mass loss-rates is a function of both $\Omega$ and $\Gamma$, and this may give raise to extreme mass loss-rates ($\Omega \Gamma $-limit). In particular, for O-type stars, LBV stars, supergiants and Wolf-Rayet stars, even slow rotation may dramatically enhance the mass loss rates. Numerical examples in the range of 9 to 120 M$_{\odot}$ at various $T_\mathrm{eff}$ are given.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Several properties of massive stars with large effects of rotation and radiation are studied. contribution 0.78 0.79 0.04 asserted 0.87
s1 We show that there are 2 roots for the equation giving the rotational velocities at break-up: 1) The usual solution, which is shown to apply when the Eddington ratio $\Gamma$ of the star is smaller than formally 0.639. 2) Above this value of $\Gamma$, there is a second root, inferior to the first one, for the break-up velocity. result 0.99 0.93 0.38 asserted 1.00
s2 This second solution tends to zero, when $\Gamma$ tends towards 1. result 0.99 0.82 0.09 asserted 1.00
s3 This second root results from the interplay of radiation and rotation, and in particular from the reduction by rotation of the effective mass in the local Eddington factor. interpretation 0.94 0.79 0.11 asserted 1.00
s4 The analysis made here should hopefully clarify a recent debate between Langer (\cite{La97,La98}) and Glatzel (\cite{Gla98}). background 0.38 0.27 0.03 hedged possibility 0.89
s5 The expression for the global mass loss-rates is a function of both $\Omega$ and $\Gamma$, and this may give raise to extreme mass loss-rates ($\Omega \Gamma $-limit). result 0.88 0.81 0.28 hedged possibility 0.97
s6 In particular, for O-type stars, LBV stars, supergiants and Wolf-Rayet stars, even slow rotation may dramatically enhance the mass loss rates. result 0.71 0.74 0.20 asserted 0.77
s7 Numerical examples in the range of 9 to 120 M$_{\odot}$ at various $T_\mathrm{eff}$ are given. method 0.68 0.90 0.03 asserted 0.97

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.89.

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not examined
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  • references and citing sentences
  • relations to other papers
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  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

Several properties of massive stars with large effects of rotation and radiation are studied. We show that there are 2 roots for the equation giving the rotational velocities at break-up: 1) The usual solution, which is shown to apply when the Eddington ratio $\Gamma$ of the star is smaller than formally 0.639. 2) Above this value of $\Gamma$, there is a second root, inferior to the first one, for the break-up velocity. This second solution tends to zero, when $\Gamma$ tends towards 1. This second root results from the interplay of radiation and rotation, and in particular from the reduction by rotation of the effective mass in the local Eddington factor. The analysis made here should hopefully clarify a recent debate between Langer (\cite{La97,La98}) and Glatzel (\cite{Gla98}). The expression for the global mass loss-rates is a function of both $\Omega$ and $\Gamma$, and this may give raise to extreme mass loss-rates ($\Omega \Gamma $-limit). In particular, for O-type stars, LBV stars, supergiants and Wolf-Rayet stars, even slow rotation may dramatically enhance the mass loss rates. Numerical examples in the range of 9 to 120 M$_{\odot}$ at various $T_\mathrm{eff}$ are given.

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