{"paper":{"title":"Hyper-neutron stars from an ab initio calculation","arxiv_id":"2502.14435","primary_cat":"nucl-th","submitted_at":"2025-02-20T10:38:30+00:00","version_compiled":"v1"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"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.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.05,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":1.0,"id":"s1","own":false,"role":"background","text":"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.","hedge":{"p":0.9,"label":"asserted"},"own_p":0.05,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.94,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.98,"id":"s2","own":false,"role":"gap","text":"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.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.06,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.98,"method":0.0,"result":0.0,"background":0.02,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.79,"id":"s3","own":true,"role":"method","text":"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.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.62,"role_probabilities":{"gap":0.0,"method":0.79,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.21,"interpretation":0.0}},{"i":4,"p":0.96,"id":"s4","own":true,"role":"method","text":"We include $N\\Lambda$, $\\Lambda\\Lambda$ two-body forces, $NN\\Lambda$, and $N\\Lambda\\Lambda$ three-body forces.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.84,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.24,"role_probabilities":{"gap":0.0,"method":0.96,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.04,"interpretation":0.0}},{"i":5,"p":0.78,"id":"s5","own":true,"role":"contribution","text":"Consequently, we determine essential astrophysical quantities such as the neutron star mass, radius, tidal deformability, and the universal $I$-Love-$Q$ relation.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.11,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.2,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.78,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"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.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.35,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":0.84,"id":"s7","own":false,"role":"interpretation","text":"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.","hedge":{"p":0.86,"label":"asserted"},"own_p":0.49,"main_claim_p":0.27,"quantitative":false,"quantitative_p":0.36,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.16,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.84}},{"i":8,"p":1.0,"id":"s8","own":true,"role":"contribution","text":"Also, for the first time in \\textit{ab initio} calculations, we investigate both non-rotating and rotating neutron star configurations.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":9,"p":0.88,"id":"s9","own":true,"role":"result","text":"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.","hedge":{"p":0.75,"label":"hedged_possibility"},"own_p":0.95,"main_claim_p":0.2,"quantitative":true,"quantitative_p":0.5,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.88,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.12}}]},"compiled":{"main_claim":{"p":0.72,"text":"These predictions are in good agreement with the latest astrophysical constraints derived from observations of massive neutron stars, gravitational waves, and joint mass-radius 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