RECORD
Hyper-neutron stars from an ab initio calculation
Nuclear Theory · Submitted 20 Feb 2025
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These predictions are in good agreement with the latest astrophysical constraints derived from observations of massive neutron stars, gravitational waves, and joint mass-radius measurements.
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
The equation of state (EoS) of neutron matter plays a decisive role to understand the neutron star properties and the gravitational waves from neutron star mergers. At sufficient densities, the appearance of hyperons generally softens the EoS, leading to a reduction in the maximum mass of neutron stars well below the observed values of about 2 solar masses. Even though repulsive three-body forces are known to solve this so-called ``hyperon puzzle'', so far performing \textit{ab initio} calculations with a substantial number of hyperons for neutron star properties has remained elusive. Starting from the newly developed auxiliary field quantum Monte Carlo algorithm to simulate hyper-neutron matter (HNM) without any sign oscillations, we derive three distinct EoSs by employing the state-of-the-art Nuclear Lattice Effective Field Theory. We include $N\Lambda$, $\Lambda\Lambda$ two-body forces, $NN\Lambda$, and $N\Lambda\Lambda$ three-body forces. Consequently, we determine essential astrophysical quantities such as the neutron star mass, radius, tidal deformability, and the universal $I$-Love-$Q$ relation. The maximum mass, radius and tidal deformability of a $1.4M_\odot$ neutron star are predicted to be $2.17(1)(1)~M_\odot$, $R_{1.4M\odot}=13.10(1)(7)~$km, and $\Lambda_{1.4M_\odot}=597(5)(18)$, respectively, based on our most realistic EoS. These predictions are in good agreement with the latest astrophysical constraints derived from observations of massive neutron stars, gravitational waves, and joint mass-radius measurements. Also, for the first time in \textit{ab initio} calculations, we investigate both non-rotating and rotating neutron star configurations. The results indicate that the impact of rotational dynamics on the maximum mass is small, regardless of whether hyperons are present in the EoS or not.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The equation of state (EoS) of neutron matter plays a decisive role to understand the neutron star properties and the gravitational waves from neutron star mergers. | background 1.00 | 0.05 | 0.03 | asserted 1.00 |
| s1 | At sufficient densities, the appearance of hyperons generally softens the EoS, leading to a reduction in the maximum mass of neutron stars well below the observed values of about 2 solar masses. | background 1.00 | 0.05 | 0.04 | asserted 0.90 |
| s2 | Even though repulsive three-body forces are known to solve this so-called ``hyperon puzzle'', so far performing \textit{ab initio} calculations with a substantial number of hyperons for neutron star properties has remained elusive. | gap 0.98 | 0.06 | 0.04 | asserted 0.99 |
| s3 | Starting from the newly developed auxiliary field quantum Monte Carlo algorithm to simulate hyper-neutron matter (HNM) without any sign oscillations, we derive three distinct EoSs by employing the state-of-the-art Nuclear Lattice Effective Field Theory. | method 0.79 | 0.96 | 0.07 | asserted 1.00 |
| s4 | We include $N\Lambda$, $\Lambda\Lambda$ two-body forces, $NN\Lambda$, and $N\Lambda\Lambda$ three-body forces. | method 0.96 | 0.84 | 0.03 | asserted 0.97 |
| s5 | Consequently, we determine essential astrophysical quantities such as the neutron star mass, radius, tidal deformability, and the universal $I$-Love-$Q$ relation. | contribution 0.78 | 0.96 | 0.11 | asserted 1.00 |
| s6 | The maximum mass, radius and tidal deformability of a $1.4M_\odot$ neutron star are predicted to be $2.17(1)(1)~M_\odot$, $R_{1.4M\odot}=13.10(1)(7)~$km, and $\Lambda_{1.4M_\odot}=597(5)(18)$, respectively, based on our most realistic EoS. | result 1.00 | 0.96 | 0.35 | asserted 0.99 |
| s7 | These predictions are in good agreement with the latest astrophysical constraints derived from observations of massive neutron stars, gravitational waves, and joint mass-radius measurements. | interpretation 0.84 | 0.49 | 0.27 | asserted 0.86 |
| s8 | Also, for the first time in \textit{ab initio} calculations, we investigate both non-rotating and rotating neutron star configurations. | contribution 1.00 | 0.96 | 0.05 | asserted 0.99 |
| s9 | The results indicate that the impact of rotational dynamics on the maximum mass is small, regardless of whether hyperons are present in the EoS or not. | result 0.88 | 0.95 | 0.20 | hedged possibility 0.75 |
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
The equation of state (EoS) of neutron matter plays a decisive role to understand the neutron star properties and the gravitational waves from neutron star mergers. At sufficient densities, the appearance of hyperons generally softens the EoS, leading to a reduction in the maximum mass of neutron stars well below the observed values of about 2 solar masses. Even though repulsive three-body forces are known to solve this so-called ``hyperon puzzle'', so far performing \textit{ab initio} calculations with a substantial number of hyperons for neutron star properties has remained elusive. Starting from the newly developed auxiliary field quantum Monte Carlo algorithm to simulate hyper-neutron matter (HNM) without any sign oscillations, we derive three distinct EoSs by employing the state-of-the-art Nuclear Lattice Effective Field Theory. We include $N\Lambda$, $\Lambda\Lambda$ two-body forces, $NN\Lambda$, and $N\Lambda\Lambda$ three-body forces. Consequently, we determine essential astrophysical quantities such as the neutron star mass, radius, tidal deformability, and the universal $I$-Love-$Q$ relation. The maximum mass, radius and tidal deformability of a $1.4M_\odot$ neutron star are predicted to be $2.17(1)(1)~M_\odot$, $R_{1.4M\odot}=13.10(1)(7)~$km, and $\Lambda_{1.4M_\odot}=597(5)(18)$, respectively, based on our most realistic EoS. These predictions are in good agreement with the latest astrophysical constraints derived from observations of massive neutron stars, gravitational waves, and joint mass-radius measurements. Also, for the first time in \textit{ab initio} calculations, we investigate both non-rotating and rotating neutron star configurations. The results indicate that the impact of rotational dynamics on the maximum mass is small, regardless of whether hyperons are present in the EoS or not.
Human review
References
How the literature uses it
3 arXiv papers cite this in 3 sentences
Papers whose main result relates to this one's
States the same result 1 paper
-
Consequently, we determine essential astrophysical quantities such as the mass-radius relation, the speed of sound and the tidal deformability of neutron stars.
Papers citing it · 1 sentence without a confident label
Cites it as background 2 papers
-
Numerous studies have been conducted to understand and model such scenarios (see e.g. [ref] , and references therein).
Properties of neutron stars with hyperons within a generalized relativistic approach · Introduction · 0.99
-
NLEFT has also been extended to hypernuclei systems, hyper-neutron and hyper-nuclear matters [ref] , and more recently to reaction and response observables through studies of neutron–alpha scattering and nuclear $β$ decay [ref] .
From binding and saturation to criticality in nuclear matter with lattice effective field theory · Introduction · 0.83
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.