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Wave-Driven Mass Loss in the Last Year of Stellar Evolution: Setting the Stage for the Most Luminous Core-Collapse Supernovae
Solar and Stellar Astrophysics · Submitted 22 Feb 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This wave-driven mass loss can explain the existence of extremely large stellar mass loss rates just prior to core-collapse, which are inferred via circumstellar interaction in some core-collapse supernovae (e.g., SNe 2006gy and PTF 09uj, and even Type IIn supernovae more generally).
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The abstract, sentence by sentence
During the late stages of stellar evolution in massive stars (C fusion and later), the fusion luminosity in the core of the star exceeds the star's Eddington luminosity. This can drive vigorous convective motions which in turn excite internal gravity waves. The local wave energy flux excited by convection is itself well above Eddington during the last few years in the life of the star. We suggest that an interesting fraction of the energy in gravity waves can, in some cases, convert into sound waves as the gravity waves propagate (tunnel) towards the stellar surface. The subsequent dissipation of the sound waves can unbind up to several $M_\odot$ of the stellar envelope. This wave-driven mass loss can explain the existence of extremely large stellar mass loss rates just prior to core-collapse, which are inferred via circumstellar interaction in some core-collapse supernovae (e.g., SNe 2006gy and PTF 09uj, and even Type IIn supernovae more generally). An outstanding question is understanding what stellar parameters (mass, rotation, metallicity, age) are the most susceptible to wave-driven mass loss. This depends on the precise internal structure of massive stars and the power-spectrum of internal gravity waves excited by stellar convection.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | During the late stages of stellar evolution in massive stars (C fusion and later), the fusion luminosity in the core of the star exceeds the star's Eddington luminosity. | background 0.93 | 0.13 | 0.05 | asserted 1.00 |
| s1 | This can drive vigorous convective motions which in turn excite internal gravity waves. | background 0.81 | 0.13 | 0.03 | asserted 0.67 |
| s2 | The local wave energy flux excited by convection is itself well above Eddington during the last few years in the life of the star. | result 0.73 | 0.38 | 0.06 | asserted 1.00 |
| s3 | We suggest that an interesting fraction of the energy in gravity waves can, in some cases, convert into sound waves as the gravity waves propagate (tunnel) towards the stellar surface. | contribution 0.76 | 0.30 | 0.08 | hedged possibility 0.66 |
| s4 | The subsequent dissipation of the sound waves can unbind up to several $M_\odot$ of the stellar envelope. | result 0.78 | 0.42 | 0.27 | hedged possibility 0.92 |
| s5 | This wave-driven mass loss can explain the existence of extremely large stellar mass loss rates just prior to core-collapse, which are inferred via circumstellar interaction in some core-collapse supernovae (e.g., SNe 2006gy and PTF 09uj, and even Type IIn supernovae more generally). | interpretation 0.97 | 0.21 | 0.66 | hedged possibility 0.69 |
| s6 | An outstanding question is understanding what stellar parameters (mass, rotation, metallicity, age) are the most susceptible to wave-driven mass loss. | gap 0.72 | 0.08 | 0.04 | unclear 0.49 |
| s7 | This depends on the precise internal structure of massive stars and the power-spectrum of internal gravity waves excited by stellar convection. | gap 0.40 | 0.08 | 0.03 | asserted 0.94 |
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The paper
Original abstract
During the late stages of stellar evolution in massive stars (C fusion and later), the fusion luminosity in the core of the star exceeds the star's Eddington luminosity. This can drive vigorous convective motions which in turn excite internal gravity waves. The local wave energy flux excited by convection is itself well above Eddington during the last few years in the life of the star. We suggest that an interesting fraction of the energy in gravity waves can, in some cases, convert into sound waves as the gravity waves propagate (tunnel) towards the stellar surface. The subsequent dissipation of the sound waves can unbind up to several $M_\odot$ of the stellar envelope. This wave-driven mass loss can explain the existence of extremely large stellar mass loss rates just prior to core-collapse, which are inferred via circumstellar interaction in some core-collapse supernovae (e.g., SNe 2006gy and PTF 09uj, and even Type IIn supernovae more generally). An outstanding question is understanding what stellar parameters (mass, rotation, metallicity, age) are the most susceptible to wave-driven mass loss. This depends on the precise internal structure of massive stars and the power-spectrum of internal gravity waves excited by stellar convection.
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References
How the literature uses it
19 arXiv papers cite this in 21 sentences
Papers citing it · 13 sentences without a confident label
Contests it 1 paper
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[ref] proposed mass loss driven by gravity waves generated in the late burning phases; however, at this point the model does not explain what are the properties of the small fraction of massive stars that end as SN IIn events.
Common Envelope Evolution Leading to Supernovae with Dense Interaction · DISCUSSION · contest 0.74
Cites it as support 1 paper
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This scenario is physically motivated by assuming that the star undergoes a period of enhanced wind mass-loss a few decades before core-collapse, as seen in numerous simulations of massive stars [ref] .
From mass-loss histories to lightcurves: a generalised framework for interaction-powered transients · Recovering variable wind mass-loss histories · 0.96
Cites it as background 6 papers
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Many channels of complex CSM structure formation have been proposed, such as pulsational instabilities [ref] , turbulent convection induced unsteady nuclear burning [ref] , wave-driven mass loss [ref] , and binary interactions.
Same explosion, many faces: numerical modeling reveals viewing angle as a driver of diversity for core-collapse SNe in binary systems · Introduction · 0.85
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From the perspective of a single-stellar evolution, several processes have been proposed, including wave-driven mass loss triggered by super-Eddington core luminosities [ref] , pulsations of red supergiant SN progenitors [ref] , and unstable silicon burning leading to violent flashes in the stellar core [ref] .
Diversity of stripped-envelope supernova light curves from interaction with binary-driven circumstellar material · Introduction · 0.93
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Mechanisms by which WR stars experience such a huge mass loss just before the explosion have not yet been clarified, although there are some suggestions [ref] .
A Dip after the Early Emission of Super-Luminous Supernovae: A Signature of Shock Breakout within Dense Circumstellar Media · Dense Circumstellar Medium around SN 2006oz · 0.84
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