RECORD
Gravitational waves from very massive stars collapsing to a black hole
High Energy Astrophysical Phenomena · Submitted 24 Jan 2019
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The detection of the gravitational-wave signal will provide a potential opportunity for verifying the presence of VMSs with mass $\gtrsim 300M_\odot$ and their pair-unstable collapse in the universe.
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 compute gravitational waves emitted by the collapse of a rotating very massive star (VMS) core leading directly to a black hole in axisymmetric numerical-relativity simulations. The evolved rotating VMS is derived by a stellar evolution calculation and its initial mass and the final carbon-oxygen core mass are $320M_\odot$ and $\approx 150M_\odot$, respectively. We find that for the moderately rapidly rotating cases, the peak strain amplitude and the corresponding frequency of gravitational waves are $\sim 10^{-22}$ and $f \approx 300$--600\,Hz for an event at the distance of $D=50$~Mpc. Such gravitational waves will be detectable only for $D \lesssim 10$~Mpc by second generation detectors, advanced LIGO, advanced VIRGO, and KAGRA, even if the designed sensitivity for these detectors is achieved. However, third-generation detectors will be able to detect such gravitational waves for an event up to $D \sim 100$~Mpc. The detection of the gravitational-wave signal will provide a potential opportunity for verifying the presence of VMSs with mass $\gtrsim 300M_\odot$ and their pair-unstable collapse in the universe.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We compute gravitational waves emitted by the collapse of a rotating very massive star (VMS) core leading directly to a black hole in axisymmetric numerical-relativity simulations. | contribution 0.94 | 0.97 | 0.09 | asserted 0.99 |
| s1 | The evolved rotating VMS is derived by a stellar evolution calculation and its initial mass and the final carbon-oxygen core mass are $320M_\odot$ and $\approx 150M_\odot$, respectively. | method 0.98 | 0.85 | 0.03 | asserted 1.00 |
| s2 | We find that for the moderately rapidly rotating cases, the peak strain amplitude and the corresponding frequency of gravitational waves are $\sim 10^{-22}$ and $f \approx 300$--600\,Hz for an event at the distance of $D=50$~Mpc. | result 1.00 | 0.97 | 0.14 | asserted 1.00 |
| s3 | Such gravitational waves will be detectable only for $D \lesssim 10$~Mpc by second generation detectors, advanced LIGO, advanced VIRGO, and KAGRA, even if the designed sensitivity for these detectors is achieved. | result 0.54 | 0.69 | 0.17 | asserted 0.88 |
| s4 | However, third-generation detectors will be able to detect such gravitational waves for an event up to $D \sim 100$~Mpc. | result 0.71 | 0.65 | 0.20 | asserted 0.51 |
| s5 | The detection of the gravitational-wave signal will provide a potential opportunity for verifying the presence of VMSs with mass $\gtrsim 300M_\odot$ and their pair-unstable collapse in the universe. | interpretation 1.00 | 0.23 | 0.46 | hedged possibility 0.99 |
What was examined, and what was not
- arXiv listing abstract v1
- 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 compute gravitational waves emitted by the collapse of a rotating very massive star (VMS) core leading directly to a black hole in axisymmetric numerical-relativity simulations. The evolved rotating VMS is derived by a stellar evolution calculation and its initial mass and the final carbon-oxygen core mass are $320M_\odot$ and $\approx 150M_\odot$, respectively. We find that for the moderately rapidly rotating cases, the peak strain amplitude and the corresponding frequency of gravitational waves are $\sim 10^{-22}$ and $f \approx 300$--600\,Hz for an event at the distance of $D=50$~Mpc. Such gravitational waves will be detectable only for $D \lesssim 10$~Mpc by second generation detectors, advanced LIGO, advanced VIRGO, and KAGRA, even if the designed sensitivity for these detectors is achieved. However, third-generation detectors will be able to detect such gravitational waves for an event up to $D \sim 100$~Mpc. The detection of the gravitational-wave signal will provide a potential opportunity for verifying the presence of VMSs with mass $\gtrsim 300M_\odot$ and their pair-unstable collapse in the universe.
Human review
References
How the literature uses it
2 arXiv papers cite this in 2 sentences
Papers citing it · 1 sentence without a confident label
Cites it as background 1 paper
-
Studies such as [ref] , [ref] and [ref] modelled the formation of direct collapse black holes from primordial gas, [ref] investigated the merger rates of black holes at high redshifts ($z≥15$), and [ref] computed the gravitational waves that would be emitted by the collapse of a $320$ Pop III star.
Grids of stellar models with rotation: V. Models from 1.7 to 120 Msun at zero metallicity · Introduction · 0.89
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.