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A systematic numerical study of the tidal instability in a rotating triaxial ellipsoid

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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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David Cébron (IRPHE), Michael Le Bars (IRPHE), Justin Leontini, Pierre Maubert (IRPHE), Patrice Le Gal (IRPHE)

Classical Physics · Submitted 30 Sep 2010

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

The authors' main claim This tidal dissipation can be of major importance for some geophysical situations and we thus derive general scaling laws which are applied to typical planetary cores.

how it is stated · hedged possibility 0.56 read the record →

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arXiv ID1009.6093 (version 1)
Pith IDXLAKVBLD, Pith's permanent record of this paper and its review
CitationDavid C\'ebron (IRPHE), Justin Leontini, Michael Le Bars (IRPHE), Patrice Le Gal (IRPHE), Pierre Maubert (IRPHE). "A systematic numerical study of the tidal instability in a rotating triaxial ellipsoid." arXiv:1009.6093 (2010). https://pith.science/paper/XLAKVBLD
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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, 4,890 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.09 · states limitation 0.10 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.10 · compares with prior results 0.78 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

The full non-linear evolution of the tidal instability is studied numerically in an ellipsoidal fluid domain relevant for planetary cores applications. Our numerical model, based on a finite element method, is first validated by reproducing some known analytical results. This model is then used to address open questions that were up to now inaccessible using theoretical and experimental approaches. Growth rates and mode selection of the instability are systematically studied as a function of the aspect ratio of the ellipsoid and as a function of the inclination of the rotation axis compared to the deformation plane. We also quantify the saturation amplitude of the flow driven by the instability and calculate the viscous dissipation that it causes. This tidal dissipation can be of major importance for some geophysical situations and we thus derive general scaling laws which are applied to typical planetary cores.

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 The full non-linear evolution of the tidal instability is studied numerically in an ellipsoidal fluid domain relevant for planetary cores applications. contribution 0.98 0.94 0.06 asserted 1.00
s1 Our numerical model, based on a finite element method, is first validated by reproducing some known analytical results. method 0.99 0.89 0.02 asserted 1.00
s2 This model is then used to address open questions that were up to now inaccessible using theoretical and experimental approaches. gap 0.60 0.61 0.05 asserted 0.98
s3 Growth rates and mode selection of the instability are systematically studied as a function of the aspect ratio of the ellipsoid and as a function of the inclination of the rotation axis compared to the deformation plane. contribution 0.84 0.95 0.13 asserted 1.00
s4 We also quantify the saturation amplitude of the flow driven by the instability and calculate the viscous dissipation that it causes. result 0.57 0.97 0.10 asserted 1.00
s5 This tidal dissipation can be of major importance for some geophysical situations and we thus derive general scaling laws which are applied to typical planetary cores. interpretation 0.76 0.94 0.41 hedged possibility 0.56

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 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

The full non-linear evolution of the tidal instability is studied numerically in an ellipsoidal fluid domain relevant for planetary cores applications. Our numerical model, based on a finite element method, is first validated by reproducing some known analytical results. This model is then used to address open questions that were up to now inaccessible using theoretical and experimental approaches. Growth rates and mode selection of the instability are systematically studied as a function of the aspect ratio of the ellipsoid and as a function of the inclination of the rotation axis compared to the deformation plane. We also quantify the saturation amplitude of the flow driven by the instability and calculate the viscous dissipation that it causes. This tidal dissipation can be of major importance for some geophysical situations and we thus derive general scaling laws which are applied to typical planetary cores.

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