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Nucleosynthesis in neutrino-driven winds: I. The physical conditions

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Y.-Z. Qian (Caltech), S. E. Woosley (UCSC)

Astrophysics · Submitted 12 Nov 1996

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

The authors' main claim The derived entropy typically falls short, by a factor of two to three, of the value required to produce a strong r-process.

how it is stated · asserted 0.98 read the record →

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arXiv IDastro-ph/9611094 (version 1)
Pith ID6LROF3NO, Pith's permanent record of this paper and its review
CitationS. E. Woosley (UCSC), Y.-Z. Qian (Caltech). "Nucleosynthesis in neutrino-driven winds: I. The physical conditions." arXiv:astro-ph/9611094 (1996). https://pith.science/paper/6LROF3NO
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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-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,156 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.06 · states limitation 0.91 · human participants 0.01 · controlled comparison 0.05 · randomized assignment 0.01 · states quantitative result 0.95 · compares with prior results 0.86 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

During the first 20 seconds of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. Previous investigations have shown that this neutrino-driven wind could be the site where the r-process occurs. The nucleosynthesis is sensitive to four physical parameters characterizing the wind: its mass loss rate, the entropy per baryon, the electron fraction, and the dynamic time scale. Different authors, using numerical models for supernovae, have arrived at qualitatively different values for these key parameters. Here we derive their values analytically and test our analytic results by numerical calculations using an implicit hydrodynamic code. Employing our analytic and numerical methods, we also investigate how various factors can affect our results. The derived entropy typically falls short, by a factor of two to three, of the value required to produce a strong r-process. Various factors that might give a higher entropy or a more rapid expansion in the wind are discussed.

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 During the first 20 seconds of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. background 1.00 0.10 0.03 asserted 1.00
s1 Previous investigations have shown that this neutrino-driven wind could be the site where the r-process occurs. background 1.00 0.03 0.04 hedged possibility 0.98
s2 The nucleosynthesis is sensitive to four physical parameters characterizing the wind: its mass loss rate, the entropy per baryon, the electron fraction, and the dynamic time scale. background 0.97 0.13 0.05 asserted 1.00
s3 Different authors, using numerical models for supernovae, have arrived at qualitatively different values for these key parameters. gap 0.55 0.04 0.02 asserted 1.00
s4 Here we derive their values analytically and test our analytic results by numerical calculations using an implicit hydrodynamic code. method 0.60 0.96 0.04 asserted 0.98
s5 Employing our analytic and numerical methods, we also investigate how various factors can affect our results. contribution 0.80 0.91 0.03 asserted 0.86
s6 The derived entropy typically falls short, by a factor of two to three, of the value required to produce a strong r-process. result 0.99 0.93 0.70 asserted 0.98
s7 Various factors that might give a higher entropy or a more rapid expansion in the wind are discussed. contribution 0.45 0.45 0.05 speculative 0.75

What kind of paper the classifier reports this is: theoretical result 0.96 · evidence from simulation or computation 0.59.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
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

During the first 20 seconds of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. Previous investigations have shown that this neutrino-driven wind could be the site where the r-process occurs. The nucleosynthesis is sensitive to four physical parameters characterizing the wind: its mass loss rate, the entropy per baryon, the electron fraction, and the dynamic time scale. Different authors, using numerical models for supernovae, have arrived at qualitatively different values for these key parameters. Here we derive their values analytically and test our analytic results by numerical calculations using an implicit hydrodynamic code. Employing our analytic and numerical methods, we also investigate how various factors can affect our results. The derived entropy typically falls short, by a factor of two to three, of the value required to produce a strong r-process. Various factors that might give a higher entropy or a more rapid expansion in the wind are discussed.

Human review

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References
How later papers used it

129 later papers cite it

Evidence: substantial. 123 of the citing papers share no author with it, and 25 of those carry a confident label from Pith's citation classifier.

Pith read 24 of the 267 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 8 of 19 papers with this label
Uses its data or values 1 of 2 papers with this label
How the literature uses it

40 arXiv papers cite this in 62 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 · 44 sentences without a confident label

Uses its method or tool 3 papers
Cites it as background 12 papers
  • The existence of this outflow at the late stages of the explosion is investigated in the seminal 1986 work by Duncan, Shapiro and Wasserman [ref] and has been elaborated on in [ref] .

    Near-critical supernova outflows and their neutrino signatures · Introduction · 0.86

  • An immediate consequence of flavor conversion, e.g. due to neutrino self-interactions, is that the change in the abundances and mean energies of $ν_e$ and $$ neutrinos would lead to a modified value of the equilibrium electron fraction corresponding to neutrino absorption, $$ [ref] , as well as the timescale over which $Y_e$ approaches $$ in outflows exposed to neutrino irradiation [ref] .

    Fast Neutrino Conversion in Hydrodynamic Simulations of Neutrino-Cooled Accretion Disks · Introduction · 0.84

  • For many years since [ref] the high entropy wind has been considered as the most promising (realistic?) environment, expelled from newly formed (hot) neutron stars in core-collapse supernovae, which continue to release neutrinos after the supernova shock wave is launched.

    Massive Stars and their Supernovae · Explosive Burning off Stability · 0.95

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