Astrophysics · arXiv:astro-ph/0312622 v1 · submitted 26 Dec 2003
The Formation of Self-Gravitating Cores in Turbulent Magnetized Clouds
The paper says
“They also confirm that local gravitational collapse is not prevented by magnetohydrodynamic waves driven by turbulent flows, even when the turbulent Jeans mass exceeds the mass in the simulation volume.”
from the abstract · picked out as the main claim by a classifier
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The paper
Abstract
We use ZEUS-MP to perform high resolution, three-dimensional, super-Alfvenic turbulent simulations in order to investigate the role of magnetic fields in self-gravitating core formation within turbulent molecular clouds. Statistical properties of our super-Alfvenic model without gravity agree with previous similar studies. Including self-gravity, our models give the following results. They are consistent with the turbulent fragmentation prediction of the core mass distribution of Padoan & Nordlund. They also confirm that local gravitational collapse is not prevented by magnetohydrodynamic waves driven by turbulent flows, even when the turbulent Jeans mass exceeds the mass in the simulation volume. Comparison of results between 256^3 and 512^3 zone simulations reveals convergence in the collapse rate. Analysis of self-gravitating cores formed in the simulation shows that: (1) All cores formed are magnetically supercritical by at least an order of magnitude. (2) A power law relation between central magnetic field strength and density B_c propto rho_c^1/2 is observed despite the cores being strongly supercritical. (3) Specific angular momentum j propto R^3/2 for cores with radius R. (4) Most cores are prolate and triaxial in shape, in agreement with the results of Gammie et al.
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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 0.15 · human participants 0.01 · controlled comparison 0.39 · randomized assignment 0.01 · states quantitative result 0.94 · compares with prior results 0.97 · mentions code or data availability 0.02
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 |
|---|---|---|---|---|
| We use ZEUS-MP to perform high resolution, three-dimensional, super-Alfvenic turbulent simulations in order to investigate the role of magnetic fields in self-gravitating core formation within turbulent molecular clouds. | method 0.89 | 0.96 | 0.04 | asserted 0.92 |
| Statistical properties of our super-Alfvenic model without gravity agree with previous similar studies. | result 0.83 | 0.75 | 0.03 | asserted 0.99 |
| Including self-gravity, our models give the following results. | contribution 0.51 | 0.74 | 0.04 | asserted 0.61 |
| They are consistent with the turbulent fragmentation prediction of the core mass distribution of Padoan & Nordlund. | result 0.86 | 0.79 | 0.15 | hedged possibility 0.66 |
| They also confirm that local gravitational collapse is not prevented by magnetohydrodynamic waves driven by turbulent flows, even when the turbulent Jeans mass exceeds the mass in the simulation volume. | result 0.98 | 0.89 | 0.31 | asserted 1.00 |
| Comparison of results between 256^3 and 512^3 zone simulations reveals convergence in the collapse rate. | result 0.88 | 0.96 | 0.05 | asserted 1.00 |
| Analysis of self-gravitating cores formed in the simulation shows that: (1) All cores formed are magnetically supercritical by at least an order of magnitude. | result 1.00 | 0.96 | 0.17 | asserted 1.00 |
| (2) A power law relation between central magnetic field strength and density B_c propto rho_c^{1/2} is observed despite the cores being strongly supercritical. | result 1.00 | 0.94 | 0.11 | asserted 1.00 |
| (3) Specific angular momentum j propto R^{3/2} for cores with radius R. | result 1.00 | 0.93 | 0.06 | asserted 1.00 |
| (4) Most cores are prolate and triaxial in shape, in agreement with the results of Gammie et al. | result 1.00 | 0.82 | 0.07 | asserted 0.90 |
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
How the labels were made
Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,522 input tokens.
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 1 Pith paper
Reviewed papers on Pith that cite this one. The full citation record
- Interstellar Turbulence I: Observations and Processes astro-ph · Apr 2004
How the literature uses it
Papers whose main result relates to this one's
States the same result 1 paper
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We then find that magnetic fields cannot prevent local collapse unless they provide magnetostatic support.
Gravitational Collapse in Turbulent Molecular Clouds. II. Magnetohydrodynamical Turbulence · 0.98
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