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Solar models with new low-metal abundances

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Wuming Yang

Solar and Stellar Astrophysics · Submitted 5 Mar 2016

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

The authors' main claim The magnetic model called AGSM keeps the agreement of the AGSR and improves the prediction of the surface helium abundance.

how it is stated · asserted 1.00 read the record →

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arXiv ID1603.01666 (version 1)
Pith IDCEOBQJ2K, Pith's permanent record of this paper and its review
CitationWuming Yang. "Solar models with new low-metal abundances." arXiv:1603.01666 (2016). https://pith.science/paper/CEOBQJ2K
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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, 8,288 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.76 · human participants 0.02 · controlled comparison 0.38 · randomized assignment 0.01 · states quantitative result 0.96 · compares with prior results 0.96 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

In the last decade, the photospheric abundances of the Sun had been revised several times by many observers. The standard solar models (SSM) constructed with the new low-metal abundances disagree with helioseismic results and detected neutrino fluxes. The solar model problem has been puzzled some stellar physicists for more than ten years. Rotation, enhanced diffusion, convection overshoot, and magnetic fields are used to reconcile the new abundances with helioseismology. The \textbf{too} low-helium \textbf{subsurface abundance} in enhanced diffusion models can be improved by the mixing caused by rotation and magnetic fields. The problem of the depth of the convective zone in rotating models can be resolved by convection overshoot. Consequently the Asplund-Grevesse-Sauval rotation model including overshooting (AGSR) reproduces the seismically inferred sound-speed and density profiles, and the convection zone depth as well as the Grevesse and Sauval (GS98) model computed before. But this model fails to reproduce the surface helium abundance which is 0.2393 ($2.6$ $\sigma$ away from the seismic value) and neutrino fluxes. The magnetic model called AGSM keeps the agreement of the AGSR and improves the prediction of the surface helium abundance. The observed separation ratios $r_{02}$ and $r_{13}$ are reasonably reproduced by AGSM. Moreover, neutrino fluxes calculated by this model are not far from the detected neutrino fluxes and the predictions of previous works.

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 In the last decade, the photospheric abundances of the Sun had been revised several times by many observers. background 1.00 0.04 0.02 asserted 1.00
s1 The standard solar models (SSM) constructed with the new low-metal abundances disagree with helioseismic results and detected neutrino fluxes. background 0.90 0.11 0.07 asserted 1.00
s2 The solar model problem has been puzzled some stellar physicists for more than ten years. background 0.97 0.05 0.03 asserted 1.00
s3 Rotation, enhanced diffusion, convection overshoot, and magnetic fields are used to reconcile the new abundances with helioseismology. method 0.50 0.13 0.07 asserted 1.00
s4 The \textbf{too} low-helium \textbf{subsurface abundance} in enhanced diffusion models can be improved by the mixing caused by rotation and magnetic fields. method 0.31 0.19 0.07 asserted 0.88
s5 The problem of the depth of the convective zone in rotating models can be resolved by convection overshoot. method 0.42 0.24 0.07 asserted 1.00
s6 Consequently the Asplund-Grevesse-Sauval rotation model including overshooting (AGSR) reproduces the seismically inferred sound-speed and density profiles, and the convection zone depth as well as the Grevesse and Sauval (GS98) model computed before. result 0.91 0.66 0.26 asserted 1.00
s7 But this model fails to reproduce the surface helium abundance which is 0.2393 ($2.6$ $\sigma$ away from the seismic value) and neutrino fluxes. limitation 0.69 0.66 0.12 asserted 1.00
s8 The magnetic model called AGSM keeps the agreement of the AGSR and improves the prediction of the surface helium abundance. result 0.64 0.69 0.25 asserted 1.00
s9 The observed separation ratios $r_{02}$ and $r_{13}$ are reasonably reproduced by AGSM. result 1.00 0.75 0.13 asserted 0.81
s10 Moreover, neutrino fluxes calculated by this model are not far from the detected neutrino fluxes and the predictions of previous works. result 0.99 0.76 0.17 asserted 0.82

What kind of paper the classifier reports this is: simulation study 0.85 · evidence from simulation or computation 0.95.

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

In the last decade, the photospheric abundances of the Sun had been revised several times by many observers. The standard solar models (SSM) constructed with the new low-metal abundances disagree with helioseismic results and detected neutrino fluxes. The solar model problem has been puzzled some stellar physicists for more than ten years. Rotation, enhanced diffusion, convection overshoot, and magnetic fields are used to reconcile the new abundances with helioseismology. The \textbf{too} low-helium \textbf{subsurface abundance} in enhanced diffusion models can be improved by the mixing caused by rotation and magnetic fields. The problem of the depth of the convective zone in rotating models can be resolved by convection overshoot. Consequently the Asplund-Grevesse-Sauval rotation model including overshooting (AGSR) reproduces the seismically inferred sound-speed and density profiles, and the convection zone depth as well as the Grevesse and Sauval (GS98) model computed before. But this model fails to reproduce the surface helium abundance which is 0.2393 ($2.6$ $\sigma$ away from the seismic value) and neutrino fluxes. The magnetic model called AGSM keeps the agreement of the AGSR and improves the prediction of the surface helium abundance. The observed separation ratios $r_{02}$ and $r_{13}$ are reasonably reproduced by AGSM. Moreover, neutrino fluxes calculated by this model are not far from the detected neutrino fluxes and the predictions of previous works.

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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

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