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Maximum mass cutoff in the neutron star mass distribution and the prospect of forming supramassive objects in the double neutron star mergers
High Energy Astrophysical Phenomena · Submitted 9 Sep 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim If such a cutoff is interpreted as the maximum gravitational mass of nonrotating cold neutron stars, the prospect of forming supramassive remnants is found to be quite promising for the double neutron star mergers with a total gravitational mass less than or equal to 2.7$M_\odot$ unless the thermal pions could substantially soften the equation of state for the very hot neutron star matter.
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The abstract, sentence by sentence
The sample of neutron stars with a measured mass is growing quickly. With the latest sample, we adopt both a flexible Gaussian mixture model and a Gaussian plus Cauchy-Lorentz component model to infer the mass distribution of neutron stars and use the Bayesian model selection to explore evidence for multimodality and a sharp cutoff in the mass distribution. The two models yield rather similar results. Consistent with previous studies, we find evidence for a bimodal distribution together with a cutoff at a mass of $M_{\rm max}=2.26_{-0.05}^{+0.12}M_\odot$ (68% credible interval; for the Gaussian mixture model). If such a cutoff is interpreted as the maximum gravitational mass of nonrotating cold neutron stars, the prospect of forming supramassive remnants is found to be quite promising for the double neutron star mergers with a total gravitational mass less than or equal to 2.7$M_\odot$ unless the thermal pions could substantially soften the equation of state for the very hot neutron star matter. These supramassive remnants have a typical kinetic rotational energy of approximately $1-2\times 10^{53}$ ergs. Together with a high neutron star merger rate approximately $10^{3}~{\rm Gpc^{-3}~yr^{-3}}$, the neutron star mergers are expected to be significant sources of EeV($10^{18}$eV) cosmic-ray protons.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The sample of neutron stars with a measured mass is growing quickly. | background 1.00 | 0.07 | 0.01 | asserted 1.00 |
| s1 | With the latest sample, we adopt both a flexible Gaussian mixture model and a Gaussian plus Cauchy-Lorentz component model to infer the mass distribution of neutron stars and use the Bayesian model selection to explore evidence for multimodality and a sharp cutoff in the mass distribution. | method 0.96 | 0.94 | 0.03 | asserted 0.93 |
| s2 | The two models yield rather similar results. | result 0.95 | 0.78 | 0.02 | asserted 1.00 |
| s3 | Consistent with previous studies, we find evidence for a bimodal distribution together with a cutoff at a mass of $M_{\rm max}=2.26_{-0.05}^{+0.12}M_\odot$ (68% credible interval; for the Gaussian mixture model). | result 1.00 | 0.94 | 0.38 | asserted 0.78 |
| s4 | If such a cutoff is interpreted as the maximum gravitational mass of nonrotating cold neutron stars, the prospect of forming supramassive remnants is found to be quite promising for the double neutron star mergers with a total gravitational mass less than or equal to 2.7$M_\odot$ unless the thermal pions could substantially soften the equation of state for the very hot neutron star matter. | interpretation 0.98 | 0.88 | 0.62 | hedged possibility 0.73 |
| s5 | These supramassive remnants have a typical kinetic rotational energy of approximately $1-2\times 10^{53}$ ergs. | result 0.97 | 0.79 | 0.05 | asserted 0.97 |
| s6 | Together with a high neutron star merger rate approximately $10^{3}~{\rm Gpc^{-3}~yr^{-3}}$, the neutron star mergers are expected to be significant sources of EeV($10^{18}$eV) cosmic-ray protons. | interpretation 0.90 | 0.55 | 0.20 | hedged possibility 0.87 |
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The paper
Original abstract
The sample of neutron stars with a measured mass is growing quickly. With the latest sample, we adopt both a flexible Gaussian mixture model and a Gaussian plus Cauchy-Lorentz component model to infer the mass distribution of neutron stars and use the Bayesian model selection to explore evidence for multimodality and a sharp cutoff in the mass distribution. The two models yield rather similar results. Consistent with previous studies, we find evidence for a bimodal distribution together with a cutoff at a mass of $M_{\rm max}=2.26_{-0.05}^{+0.12}M_\odot$ (68% credible interval; for the Gaussian mixture model). If such a cutoff is interpreted as the maximum gravitational mass of nonrotating cold neutron stars, the prospect of forming supramassive remnants is found to be quite promising for the double neutron star mergers with a total gravitational mass less than or equal to 2.7$M_\odot$ unless the thermal pions could substantially soften the equation of state for the very hot neutron star matter. These supramassive remnants have a typical kinetic rotational energy of approximately $1-2\times 10^{53}$ ergs. Together with a high neutron star merger rate approximately $10^{3}~{\rm Gpc^{-3}~yr^{-3}}$, the neutron star mergers are expected to be significant sources of EeV($10^{18}$eV) cosmic-ray protons.
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References
How the literature uses it
10 arXiv papers cite this in 19 sentences
Papers citing it · 10 sentences without a confident label
Uses its method or tool 1 paper
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We infer the mass distribution parameters and the maximum mass cutoff using the hierarchical Bayesian inference [ref] with the following likelihood [equation] where $N$ is the size of NS sample, $P(m_i^k|θ⃗)$ is a two-component Gaussian mixture mass distribution model parameterized with $θ⃗$ (see Eq.(1) in [ref] ), and $m_i^k$ is the $k$-th sample of the $i$-th mass measurement.
Maximum gravitational mass $M_{\rm TOV}=2.25^{+0.08}_{-0.07}M_\odot$ inferred at about $3\%$ precision with multimessenger data of neutron stars · Methods · 0.99
Uses its data or values 1 paper
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The first has a mean of $1.34$, a standard deviation of $0.07$, and a relative weight[See Ref. [ref] for a definition of the relative weight.] of $0.65$.
Incorporating neutron star physics into gravitational wave inference with physics-informed priors using normalizing flows · Population models · 0.89
Compares with it 2 papers
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The $M_max$ obtained in this work is slightly larger than our previous finding $M_max∼2.26M_⊙$ [ref] , which is primarily attributed to the enlargement of the data sample.
Maximum gravitational mass $M_{\rm TOV}=2.25^{+0.08}_{-0.07}M_\odot$ inferred at about $3\%$ precision with multimessenger data of neutron stars · The $M_max$ inferred in the mass function modeling · 0.99
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By comparing our constraints on maximum mass of NS with previous $M_TOV$ determinations in , e.g., Refs. [ref] , we find that current observational and theoretical knowledge of the NS population and its EoS, favors a binary black hole merger scenario for GW190814.
Constraints on the phase transition and nuclear symmetry parameters from PSR $\mathrm{J}0740+6620$ and multimessenger data of other neutron stars · Summary · 0.98
Cites it as background 1 paper
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Other investigations have also calculated the $M_TOV$ from the mass distribution of NSs [ref] and the observations of short gamma-ray bursts [ref] in particular the multimessenger observations of GW170817/GRB 170817A [ref] .
Mass and radius of the most massive neutron star: The probe of the equation of state and perturbative QCD · Introduction · 0.88
What it cites · 2 sentences without a confident label
Uses data or values from 1 paper
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NS-NS 1.322$±$0.011 [ref] GW170817A NS-NS $1.47^+0.09_-0.07$ [ref] GW170817B NS-NS $1.27^+0.06_-0.07$ [ref] GW190425A NS-NS $1.56^+0.06_-0.08$ [ref] GW190425B NS-NS $1.74^+0.10_-0.06$ [ref] J1411+2551 NS-NS 0.1223898 2.538$±$0.022 [ref] J1518+4904 NS-NS 0.115988 2.7183$±$0.0007 [ref] J1811-1736 NS-NS 0.128121 2.57$±$0.10 [ref] J1829+2456 NS-NS 0.29413 2.59$±$0.02 [ref] J1913+1102 NS-NS 0.136344 2.875$±$0.014 [ref] J1930-1852 NS-NS 0.34690765 2.54$±$0.03 [ref] J1946+2052 NS-NS 0.268184 2.50$±$0.04 [ref] B1855+09 NS-WD 1.37$±$0.13 [ref] J0337+1715 NS-WD 1.4359$±$0.0003 [ref] J0348+0432 NS-WD 2.01$±$0.04 [ref] J0437-4715 NS-WD 1.44$±$0.07 [ref] J0621+1002 NS-WD $1.53^+0.10_-0.20$ [ref] J0740+6620 NS-WD $2.14^+0.10_-0.09$ [ref] J0751+1807 NS-WD 1.64$±$0.15 [ref] J1012+5307 NS-WD 1.83$±$0.11 [ref] J1141-6545 NS-WD 1.27$±$0.01 [ref] J1600-3053 NS-WD $2.3^+0.7_-0.6$ [ref] J1614-2230 NS-WD 1.908
The millisecond pulsar mass distribution: Evidence for bimodality and constraints on the maximum neutron star mass · Neutron star data · 0.99
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