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Pre-Supernova Outbursts via Wave Heating in Massive Stars I: Red Supergiants

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Jim Fuller

Solar and Stellar Astrophysics · Submitted 27 Apr 2017

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

The authors' main claim In our models, wave heating is unlikely to lead to luminous type IIn SNe, but it may contribute to flash-ionized SNe and some of the diversity seen in II-P/II-L SNe.

how it is stated · hedged possibility 1.00 read the record →

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arXiv ID1704.08696 (version 2)
Pith ID2WQEDIV6, Pith's permanent record of this paper and its review
CitationJim Fuller. "Pre-Supernova Outbursts via Wave Heating in Massive Stars I: Red Supergiants." arXiv:1704.08696 (2017). https://pith.science/paper/2WQEDIV6
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The compiled record

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, 5,282 input tokens.

What the abstract itself states, as probabilities: claims first 0.10 · states limitation 0.91 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.73 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

Early observations of supernovae (SNe) indicate that enhanced mass loss and pre-SN outbursts may occur in progenitors of many types of SNe. We investigate the role of energy transport via waves driven by vigorous convection during late-stage nuclear burning of otherwise typical $15 \, M_\odot$ red supergiant SNe progenitors. Using MESA stellar evolution models including 1D hydrodynamics, we find that waves carry $\sim \! 10^7 \, L_\odot$ of power from the core to the envelope during core neon/oxygen burning in the final years before core collapse. The waves damp via shocks and radiative diffusion at the base of the hydrogen envelope, which heats up fast enough to launch a pressure wave into the overlying envelope that steepens into a weak shock near the stellar surface, causing a mild stellar outburst and ejecting a small ($\lesssim 1 \, M_\odot$) amount of mass at low speed ($\lesssim \! 50 \, {\rm km}/{\rm s}$) roughly one year before the SN. The wave heating inflates the stellar envelope but does not completely unbind it, producing a non-hydrostatic pre-SN envelope density structure different from prior expectations. In our models, wave heating is unlikely to lead to luminous type IIn SNe, but it may contribute to flash-ionized SNe and some of the diversity seen in II-P/II-L SNe.

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 Early observations of supernovae (SNe) indicate that enhanced mass loss and pre-SN outbursts may occur in progenitors of many types of SNe. background 1.00 0.04 0.03 hedged possibility 1.00
s1 We investigate the role of energy transport via waves driven by vigorous convection during late-stage nuclear burning of otherwise typical $15 \, M_\odot$ red supergiant SNe progenitors. contribution 1.00 0.70 0.05 unclear 0.49
s2 Using MESA stellar evolution models including 1D hydrodynamics, we find that waves carry $\sim \! 10^7 \, L_\odot$ of power from the core to the envelope during core neon/oxygen burning in the final years before core collapse. result 0.96 0.97 0.20 asserted 1.00
s3 The waves damp via shocks and radiative diffusion at the base of the hydrogen envelope, which heats up fast enough to launch a pressure wave into the overlying envelope that steepens into a weak shock near the stellar surface, causing a mild stellar outburst and ejecting a small ($\lesssim 1 \, M_\odot$) amount of mass at low speed ($\lesssim \! 50 \, {\rm km}/{\rm s}$) roughly one year before the SN. result 1.00 0.91 0.52 asserted 1.00
s4 The wave heating inflates the stellar envelope but does not completely unbind it, producing a non-hydrostatic pre-SN envelope density structure different from prior expectations. result 0.91 0.90 0.23 asserted 1.00
s5 In our models, wave heating is unlikely to lead to luminous type IIn SNe, but it may contribute to flash-ionized SNe and some of the diversity seen in II-P/II-L SNe. interpretation 0.99 0.81 0.27 hedged possibility 1.00

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • 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

Early observations of supernovae (SNe) indicate that enhanced mass loss and pre-SN outbursts may occur in progenitors of many types of SNe. We investigate the role of energy transport via waves driven by vigorous convection during late-stage nuclear burning of otherwise typical $15 \, M_\odot$ red supergiant SNe progenitors. Using MESA stellar evolution models including 1D hydrodynamics, we find that waves carry $\sim \! 10^7 \, L_\odot$ of power from the core to the envelope during core neon/oxygen burning in the final years before core collapse. The waves damp via shocks and radiative diffusion at the base of the hydrogen envelope, which heats up fast enough to launch a pressure wave into the overlying envelope that steepens into a weak shock near the stellar surface, causing a mild stellar outburst and ejecting a small ($\lesssim 1 \, M_\odot$) amount of mass at low speed ($\lesssim \! 50 \, {\rm km}/{\rm s}$) roughly one year before the SN. The wave heating inflates the stellar envelope but does not completely unbind it, producing a non-hydrostatic pre-SN envelope density structure different from prior expectations. In our models, wave heating is unlikely to lead to luminous type IIn SNe, but it may contribute to flash-ionized SNe and some of the diversity seen in II-P/II-L SNe.

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References
How later papers used it

113 later papers cite it

Evidence: substantial. 102 of the citing papers share no author with it, and 13 of those carry a confident label from Pith's citation classifier.

Pith read 17 of the 171 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Uses its method or tool 1 of 5 papers with this label · 1 by the same authors

By the same authors

How the literature uses it

11 arXiv papers cite this in 12 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 9 sentences without a confident label

Cites it as background 3 papers
  • 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

  • Such systems are relatively rare, and a range of theoretical models have been proposed to explain the phenomenon (e.g., [ref] , [ref] , [ref] , [ref] , [ref] ).

    The Physics of Flash (Supernova) Spectroscopy · Introduction · 1.00

  • There are also (sometimes overlapping) scenarios that have been discussed, involving binary mergers, stellar collisions, violent common envelope events, accretion events onto a companion (perhaps including compact object companions, although this has not been discussed much for $η$ Car), violent pulsations, extreme magnetic activity, pulsational pair instability eruptions, unsteady or explosive nuclear burning, and wave driving associated with late nuclear burning phases approaching core collapse [ref] .

    Exceptionally fast ejecta seen in light echoes of Eta Carinae's Great Eruption · INTRODUCTION · 0.99

What it cites · 10 sentences without a confident label

Compares with 1 paper
Cites as support 2 papers
Cites as background 1 paper

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