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The observed neutron star mass distribution as a probe of the supernova explosion mechanism
Solar and Stellar Astrophysics · Submitted 24 Apr 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The double NS system masses thus directly point to the mass coordinate where the supernova explosion was initiated, making them an excellent probe of the supernova explosion mechanism.
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The abstract, sentence by sentence
The observed distribution of neutron star (NS) masses reflects the physics of core-collapse supernova explosions and the structure of the massive stars that produce them at the end of their evolution. We present a Bayesian analysis that directly compares the NS mass distribution observed in double NS systems to theoretical models of NS formation. We find that models with standard binary mass ratio distributions are strongly preferred over independently picking the masses from the initial mass function, although the strength of the inference depends on whether current assumptions for identifying the remnants of the primary and secondary stars are correct. Second, NS formation models with no mass fallback are favored because they reduce the dispersion in NS masses. The double NS system masses thus directly point to the mass coordinate where the supernova explosion was initiated, making them an excellent probe of the supernova explosion mechanism. If we assume no fallback and simply vary the mass coordinate separating the remnant and the supernova ejecta, we find that for solar metallicity stars the explosion most likely develops at the edge of the iron core at a specific entropy of about 2.8 k_B. The primary limitations of our study are the poor knowledge of the supernova explosion mechanism and the lack of broad range of SN model explosions of LMC to solar metallicity.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The observed distribution of neutron star (NS) masses reflects the physics of core-collapse supernova explosions and the structure of the massive stars that produce them at the end of their evolution. | background 1.00 | 0.06 | 0.05 | asserted 1.00 |
| s1 | We present a Bayesian analysis that directly compares the NS mass distribution observed in double NS systems to theoretical models of NS formation. | contribution 0.60 | 0.96 | 0.04 | asserted 0.96 |
| s2 | We find that models with standard binary mass ratio distributions are strongly preferred over independently picking the masses from the initial mass function, although the strength of the inference depends on whether current assumptions for identifying the remnants of the primary and secondary stars are correct. | result 1.00 | 0.96 | 0.19 | asserted 0.99 |
| s3 | Second, NS formation models with no mass fallback are favored because they reduce the dispersion in NS masses. | result 1.00 | 0.90 | 0.13 | asserted 0.99 |
| s4 | The double NS system masses thus directly point to the mass coordinate where the supernova explosion was initiated, making them an excellent probe of the supernova explosion mechanism. | interpretation 0.99 | 0.69 | 0.63 | asserted 1.00 |
| s5 | If we assume no fallback and simply vary the mass coordinate separating the remnant and the supernova ejecta, we find that for solar metallicity stars the explosion most likely develops at the edge of the iron core at a specific entropy of about 2.8 k_B. | result 0.98 | 0.95 | 0.23 | hedged possibility 0.62 |
| s6 | The primary limitations of our study are the poor knowledge of the supernova explosion mechanism and the lack of broad range of SN model explosions of LMC to solar metallicity. | limitation 1.00 | 0.47 | 0.02 | asserted 1.00 |
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The paper
Original abstract
The observed distribution of neutron star (NS) masses reflects the physics of core-collapse supernova explosions and the structure of the massive stars that produce them at the end of their evolution. We present a Bayesian analysis that directly compares the NS mass distribution observed in double NS systems to theoretical models of NS formation. We find that models with standard binary mass ratio distributions are strongly preferred over independently picking the masses from the initial mass function, although the strength of the inference depends on whether current assumptions for identifying the remnants of the primary and secondary stars are correct. Second, NS formation models with no mass fallback are favored because they reduce the dispersion in NS masses. The double NS system masses thus directly point to the mass coordinate where the supernova explosion was initiated, making them an excellent probe of the supernova explosion mechanism. If we assume no fallback and simply vary the mass coordinate separating the remnant and the supernova ejecta, we find that for solar metallicity stars the explosion most likely develops at the edge of the iron core at a specific entropy of about 2.8 k_B. The primary limitations of our study are the poor knowledge of the supernova explosion mechanism and the lack of broad range of SN model explosions of LMC to solar metallicity.
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References
How the literature uses it
2 arXiv papers cite this in 4 sentences
Papers citing it · 3 sentences without a confident label
Compares with it 1 paper
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Interestingly, however, [ref] favor a NS formation scenario with no or very little mass fallback, which is consistent with the tendency of our models compared to piston-driven explosion models.
Progenitor-Explosion Connection and Remnant Birth Masses for Neutrino-Driven Supernovae of Iron-Core Progenitors · Conclusions · 0.83
What it cites · 20 sentences without a confident label
Builds on 2 papers
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We replace the parametric models of observed NS masses used by [ref] and [ref] with predictions of NS masses based on the actual physics of progenitors and supernova explosions so that we can directly constrain, compare and assess the validity of physical models for the explosion.
The Neutron Star Mass Distribution · Introduction · 0.80
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We replace the parametric models of observed NS masses used by [ref] and [ref] with predictions of NS masses based on the actual physics of progenitors and supernova explosions so that we can directly constrain, compare and assess the validity of physical models for the explosion.
On the Mass Distribution and Birth Masses of Neutron Stars · Introduction · 0.80
Uses the method or tool of 2 papers
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We present the resulting probability distribution and comparison with other models in the Appendix.], as has been done for some studies of explosion physics [ref] .
Is Strong SASI Activity the Key to Successful Neutrino-Driven Supernova Explosions? · Discussions & Conclusions · 0.84
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We present the resulting probability distribution and comparison with other models in the Appendix.], as has been done for some studies of explosion physics [ref] .
The Hydrodynamic Origin of Neutron Star Kicks · Discussions & Conclusions · 0.84
Uses data or values from 3 papers
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We illustrate this method on a sample of double neutron stars from [ref] which did not experience significant mass accretion and should reflect the distribution of NS birth masses.
On the Mass Distribution and Birth Masses of Neutron Stars · Discussions & Conclusions · 0.99
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The masses of these NSs cluster at $∼1.35$ with a dispersion of only $∼0.06$ [ref] , and the mean masses of the pulsars and their companions differ by only $0.03$ [ref] .
The Neutron Star Mass Distribution · Introduction · 0.86
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We thank Thomas Janka for providing us with the NS mass distribution of [ref] and to the editor of our paper for allowing us to add the Appendix.
Progenitor-Explosion Connection and Remnant Birth Masses for Neutrino-Driven Supernovae of Iron-Core Progenitors · Acknowledgments · 0.98
Compares with 3 papers
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Thus, the reduction of fallback in the [ref] NS mass distribution provides a better match to the observed masses of DNS binaries, but not as good match as the [ref] $$ core models with no fallback.
Progenitor-Explosion Connection and Remnant Birth Masses for Neutrino-Driven Supernovae of Iron-Core Progenitors · The NS mass distribution of Ugliano et al. (2012) · 0.98
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This width is several times smaller than the typical width of the DNS mass distributions of [ref] and [ref] .
The Neutron Star Mass Distribution · NSs as members of a binary · 0.98
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This width is several times smaller than the typical width of the DNS mass distributions of [ref] and [ref] .
On the Mass Distribution and Birth Masses of Neutron Stars · NSs as members of a binary · 0.98
Cites as background 1 paper
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Present day studies are focused on whether multi-dimensional effects will aid the explosion [ref] .
Is Strong SASI Activity the Key to Successful Neutrino-Driven Supernova Explosions? · Introduction · 0.89
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