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Numerical Simulation of General Relativistic Stellar Collapse

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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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Cristian R. Ghezzi, Patricio S. Letelier

General Relativity and Quantum Cosmology · Submitted 19 Dec 2003

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

The authors' main claim Here we discuss the capabilities of the code that make it well suited for numerical relativity on a personal computer and some caveats based on the experiments we have made with it.

how it is stated · asserted 0.93 read the record →

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arXiv IDgr-qc/0312090 (version 1)
Pith IDYK4ZOHIB, Pith's permanent record of this paper and its review
CitationCristian R. Ghezzi, Patricio S. Letelier. "Numerical Simulation of General Relativistic Stellar Collapse." arXiv:gr-qc/0312090 (2003). https://pith.science/paper/YK4ZOHIB
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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, 3,623 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.89 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.42 · compares with prior results 0.24 · mentions code or data availability 0.04.

The abstract, sentence by sentence

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

We present preliminar results and tests of a new general relativistic code to simulate the hydrodynamic collapse of a 21 solar masses star. We have assumed spherical symmetry and used the formalism of Misner and Sharp to construct a finite-difference scheme to solve the Einstein's equations, energy-momentum conservation equations and baryonic conservation equation. The code is similar to the one originally developed by May and White (1967). Here we discuss the capabilities of the code that make it well suited for numerical relativity on a personal computer and some caveats based on the experiments we have made with it.

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 We present preliminar results and tests of a new general relativistic code to simulate the hydrodynamic collapse of a 21 solar masses star. contribution 1.00 0.92 0.12 asserted 0.99
s1 We have assumed spherical symmetry and used the formalism of Misner and Sharp to construct a finite-difference scheme to solve the Einstein's equations, energy-momentum conservation equations and baryonic conservation equation. method 1.00 0.91 0.04 asserted 1.00
s2 The code is similar to the one originally developed by May and White (1967). background 0.67 0.09 0.03 asserted 1.00
s3 Here we discuss the capabilities of the code that make it well suited for numerical relativity on a personal computer and some caveats based on the experiments we have made with it. limitation 0.69 0.87 0.13 asserted 0.93

What kind of paper the classifier reports this is: method or tool 0.83 · 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

We present preliminar results and tests of a new general relativistic code to simulate the hydrodynamic collapse of a 21 solar masses star. We have assumed spherical symmetry and used the formalism of Misner and Sharp to construct a finite-difference scheme to solve the Einstein's equations, energy-momentum conservation equations and baryonic conservation equation. The code is similar to the one originally developed by May and White (1967). Here we discuss the capabilities of the code that make it well suited for numerical relativity on a personal computer and some caveats based on the experiments we have made with it.

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