RECORD
A comprehensive set of simulations of high-velocity collisions between main sequence stars
Astrophysics · Submitted 26 Mar 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that the outcome of collisions depends sensitively on the stellar structure and that, in most cases, using polytropic models is inappropriate.
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.
Open the compiled record
The abstract, sentence by sentence
We report on a very large set of simulations of collisions between two main sequence (MS) stars. These computations were done with the ``Smoothed Particle Hydrodynamics'' method. Realistic stellar structure models for evolved MS stars were used. In order to sample an extended domain of initial parameters space (masses of the stars, relative velocity and impact parameter), more than 15000 simulations were carried out. We considered stellar masses ranging between 0.1 and 75 Msun and relative velocities up to a few thousands km/s. To limit the computational burden, a resolution of 2000-30000 particles per star was used. The primary goal of this study was to build a complete database from which the result of any collision can be interpolated. This allows us to incorporate the effects of stellar collisions with an unprecedented level of realism into dynamical simulations of galactic nuclei and other dense stellar clusters. We make the data describing the initial condition and outcome (mass and energy loss, angle of deflection) of all our simulations freely available on the Internet. We find that the outcome of collisions depends sensitively on the stellar structure and that, in most cases, using polytropic models is inappropriate. Published fitting formulas for the collision outcomes, established from a limited set of collisions, prove of limited use because they do not allow robust extrapolation to other stellar structures or relative velocities.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We report on a very large set of simulations of collisions between two main sequence (MS) stars. | contribution 1.00 | 0.96 | 0.03 | asserted 0.98 |
| s1 | These computations were done with the ``Smoothed Particle Hydrodynamics'' method. | method 1.00 | 0.88 | 0.02 | asserted 1.00 |
| s2 | Realistic stellar structure models for evolved MS stars were used. | method 1.00 | 0.62 | 0.02 | asserted 1.00 |
| s3 | In order to sample an extended domain of initial parameters space (masses of the stars, relative velocity and impact parameter), more than 15000 simulations were carried out. | method 0.93 | 0.96 | 0.03 | asserted 0.99 |
| s4 | We considered stellar masses ranging between 0.1 and 75 Msun and relative velocities up to a few thousands km/s. | method 0.93 | 0.87 | 0.02 | asserted 1.00 |
| s5 | To limit the computational burden, a resolution of 2000-30000 particles per star was used. | method 0.72 | 0.90 | 0.02 | asserted 1.00 |
| s6 | The primary goal of this study was to build a complete database from which the result of any collision can be interpolated. | contribution 0.98 | 0.74 | 0.06 | asserted 0.98 |
| s7 | This allows us to incorporate the effects of stellar collisions with an unprecedented level of realism into dynamical simulations of galactic nuclei and other dense stellar clusters. | interpretation 0.69 | 0.42 | 0.09 | asserted 0.87 |
| s8 | We make the data describing the initial condition and outcome (mass and energy loss, angle of deflection) of all our simulations freely available on the Internet. | contribution 0.99 | 0.92 | 0.04 | asserted 1.00 |
| s9 | We find that the outcome of collisions depends sensitively on the stellar structure and that, in most cases, using polytropic models is inappropriate. | result 0.98 | 0.96 | 0.47 | asserted 1.00 |
| s10 | Published fitting formulas for the collision outcomes, established from a limited set of collisions, prove of limited use because they do not allow robust extrapolation to other stellar structures or relative velocities. | result 0.57 | 0.52 | 0.27 | asserted 1.00 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
We report on a very large set of simulations of collisions between two main sequence (MS) stars. These computations were done with the ``Smoothed Particle Hydrodynamics'' method. Realistic stellar structure models for evolved MS stars were used. In order to sample an extended domain of initial parameters space (masses of the stars, relative velocity and impact parameter), more than 15000 simulations were carried out. We considered stellar masses ranging between 0.1 and 75 Msun and relative velocities up to a few thousands km/s. To limit the computational burden, a resolution of 2000-30000 particles per star was used. The primary goal of this study was to build a complete database from which the result of any collision can be interpolated. This allows us to incorporate the effects of stellar collisions with an unprecedented level of realism into dynamical simulations of galactic nuclei and other dense stellar clusters. We make the data describing the initial condition and outcome (mass and energy loss, angle of deflection) of all our simulations freely available on the Internet. We find that the outcome of collisions depends sensitively on the stellar structure and that, in most cases, using polytropic models is inappropriate. Published fitting formulas for the collision outcomes, established from a limited set of collisions, prove of limited use because they do not allow robust extrapolation to other stellar structures or relative velocities.
Human review
References
How the literature uses it
1 arXiv paper cite this in 3 sentences
Papers citing it · 2 sentences without a confident label
Builds on it 1 paper
-
We improve upon the SPH simulations presented in [ref] by using accurate stellar profiles and exploring the effects of stellar age on collision outcomes.
Machine Learning Methods for Stellar Collisions. I. Predicting Outcomes of SPH Simulations · Introduction · 0.88
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.