Solar and Stellar Astrophysics · arXiv:1002.4914 v1 · submitted 26 Feb 2010
2D and 3D Core-Collapse Supernovae Simulation Results Obtained with the CHIMERA Code
The paper says
“These have all exhibited explosions and are currently in the expanding phase with the shock at between 5,000 and 20,000 km.”
from the abstract · picked out as the main claim by a classifier
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Abstract
Much progress in realistic modeling of core-collapse supernovae has occurred recently through the availability of multi-teraflop machines and the increasing sophistication of supernova codes. These improvements are enabling simulations with enough realism that the explosion mechanism, long a mystery, may soon be delineated. We briefly describe the CHIMERA code, a supernova code we have developed to simulate core-collapse supernovae in 1, 2, and 3 spatial dimensions. We then describe the results of an ongoing suite of 2D simulations initiated from a 12, 15, 20, and 25 solar mass progenitor. These have all exhibited explosions and are currently in the expanding phase with the shock at between 5,000 and 20,000 km. We also briefly describe an ongoing simulation in 3 spatial dimensions initiated from the 15 solar mass progenitor.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 1.00
What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.34 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.95 · compares with prior results 0.08 · mentions code or data availability 0.04
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v1). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| Much progress in realistic modeling of core-collapse supernovae has occurred recently through the availability of multi-teraflop machines and the increasing sophistication of supernova codes. | background 1.00 | 0.05 | 0.03 | asserted 1.00 |
| These improvements are enabling simulations with enough realism that the explosion mechanism, long a mystery, may soon be delineated. | background 0.97 | 0.06 | 0.09 | hedged possibility 1.00 |
| We briefly describe the CHIMERA code, a supernova code we have developed to simulate core-collapse supernovae in 1, 2, and 3 spatial dimensions. | method 0.82 | 0.90 | 0.04 | asserted 0.98 |
| We then describe the results of an ongoing suite of 2D simulations initiated from a 12, 15, 20, and 25 solar mass progenitor. | contribution 0.67 | 0.93 | 0.06 | asserted 0.90 |
| These have all exhibited explosions and are currently in the expanding phase with the shock at between 5,000 and 20,000 km. | result 1.00 | 0.94 | 0.28 | asserted 1.00 |
| We also briefly describe an ongoing simulation in 3 spatial dimensions initiated from the 15 solar mass progenitor. | contribution 0.76 | 0.93 | 0.04 | asserted 0.95 |
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
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- full text
- figures and tables
- references and citing sentences
- relations to other papers
Levels run
- P abstract
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- S sections
- T body sentences
- C citations
- R cross-paper relations
How the labels were made
Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 4,962 input tokens, $0.0002 reported.
Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON
Cited by 7 Pith papers
Reviewed papers on Pith that cite this one. The full citation record
- The origin of Potassium in Galactic chemical evolution - The effect of C-O shell mergers in massive stars astro-ph.GA · Nov 2026
- Gravitational Waves from Core-Collapse Supernovae: Dependence on the Progenitor Star, Rotation Rate and Nuclear Equation of State astro-ph.HE · Sep 2026
- Neutrino Quantum Kinetics hep-ph · Sep 2013
- Halo Modification of a Supernova Neutronization Neutrino Burst astro-ph.HE · Feb 2013
- Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity astro-ph.SR · Oct 2011
- Neutrino mass ordering from the next Galactic supernova at DUNE, HK, and JUNO hep-ph · Jun 2026
- Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae astro-ph.HE · Oct 2011
How the literature uses it
16 arXiv papers cite this in 28 sentences
Papers citing it · 24 sentences without a confident label
Uses its data or values 1 paper
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These models tend to start exploding at around 300 m after bounce, and the explosion energy for the longest running model of the 25 M$_⊙$ progenitor is reaching to 1 B at 1.2 s after bounce [ref] .
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae · On core-collapse supernova simulations · 0.82
Compares with it 1 paper
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It is noteworthy that the neutrino emission and the shock evolution are similarly sensitive to the neutrino interaction rates (in agreement with the findings of [ref] ).
Core-Collapse Supernovae: Explosion Dynamics, Neutrinos and Gravitational Waves · General Relativistic Effects in Multi-Dimensional Supernova Models · 0.86
Cites it as background 2 papers
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First steps in this direction were reported in Refs. [ref] , but the models are either not evolved for interestingly long post-bounce times or the employed numerical resolution is poor and the neutrino data are not conclusive with respect to the effects discussed here.
Probing Lorentz Violation in Neutrino Propagation from a Core-Collapse Supernova · Two-Dimensional Simulation of a Core-Collapse Supernova · 0.81
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Neutrinos play a fundamental role in extreme astrophysical environments, such as core collapse supernovae and neutron star binary mergers, where they, in part, determine the dynamical evolution of the explosion and set the ambient conditions for the ensuing nucleosynthesis, e.g., Refs. [ref] .
Time Scales in Many-Body Fast Neutrino Flavor Conversion · Introduction · 0.98
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