{"total":12,"items":[{"citing_arxiv_id":"2606.23929","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch","primary_cat":"nucl-th","submitted_at":"2026-06-22T20:49:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09247","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Bayesian analysis of the shear modulus in the neutron-star crust","primary_cat":"astro-ph.HE","submitted_at":"2026-06-08T09:20:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the estimated frequencies (see Table 2). Therefore, we think that the use of a NS-mass-independent value of⟨vs⟩nB as found using Eq. (22) remains a good approximation. Article number, page 7 A&A proofs:manuscript no. paper_shear_revised2 60 80 100 120 140rWS [fm] (a) 1 CLDM 2 CLDM 2 CLDM gaussian prior HFB BSk24 CLDM BSk24 20 25 30 35 40 45 50Z (b) 0.5 1.0 1.5 2.0 2.5 nB [10 4 fm 3] 0.0 0.2 0.4 0.6 0.8 [10 5 MeV fm 3] (c) 0.5 1.0 1.5 2.0 2.5 nB [10 4 fm 3] 1.2 1.4 1.6 1.8vs [108 cm s 1] (d) Fig. 1: Wigner-Seitz-cell radius (panel a), proton numberZof the ions (panel b), shear modulusµ(panel c), and shear speed (panel d) as a function of baryon number density in the outer crust. Shaded areas correspond to1σand2σ confidence intervals for the uniform prior, while dash-dotted red lines delimit the2σconfidence interval for the non-"},{"citing_arxiv_id":"2606.06378","ref_index":15,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On the Possibility of a Strong First-Order Phase Transition in Neutron Stars","primary_cat":"nucl-th","submitted_at":"2026-06-04T16:45:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian analysis favors a strong first-order phase transition in cold dense QCD matter whose onset lies above the central density of the most massive observed neutron stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18731","ref_index":212,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T17:53:13+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18560","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Astrophysics equation of state inference with Bayesian chiral effective field theory uncertainties","primary_cat":"nucl-th","submitted_at":"2026-05-18T15:40:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian EOS inference with χEFT uncertainty priors and LIGO/NICER data yields posteriors consistent with prior work, a stiffening above 3n0, negligible pQCD impact, and an inferred symmetry-energy slope L of 42.6-56.7 MeV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14264","ref_index":87,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The compact neutron star in 4U 1746-37 revisited: Reassessing the mass and radius","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T02:08:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Significant X-ray flux blocking in 4U 1746-37 allows the neutron star to have canonical mass and radius values of 1.59 solar masses and 13 km or 2.12 solar masses and 9.8 km.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.05428","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Reconstruction of fast-rotating neutron star observables with the neural network","primary_cat":"astro-ph.HE","submitted_at":"2026-04-07T04:46:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.06696","ref_index":52,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Bayesian Constraints on the Neutron Star Equation of State with a Smooth Hadron-Quark Crossover","primary_cat":"nucl-th","submitted_at":"2026-02-06T13:34:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of a smooth hadron-quark crossover EOS finds current observations tightly constrain the density dependence of nuclear symmetry energy while leaving highest-density hadronic and quark-matter parameters only weakly constrained.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.18044","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Constrained Gaussian-process bridge prior for neutron-star equation-of-state inference","primary_cat":"astro-ph.HE","submitted_at":"2025-12-19T20:24:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.07172","ref_index":85,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Chiral, parity-doublet, effective-Lagrangian mean-field theories for nuclear and astrophysical phenomenology","primary_cat":"hep-ph","submitted_at":"2025-12-08T05:11:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of parity-doublet models in effective field theory that accommodate a chirally invariant mass m0 to describe baryons across vacuum, nuclear, and astrophysical densities.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"Oneofthestrongestmotivationsforparity-doubletmodelsliesintheirimplicationsfortheequationofstate of dense matter and the structure of compact stars [84]. The chiral-invariant massm0 effectively governs how rapidly the nucleon effective masses decrease with increasing density. This, in turn, impacts the pressure-density relation and the maximum neutron-star mass achievable within the model [85]. Similar correlations between nuclear and neutron-star radii have been discussed in Ref. [86]. Calculations by Motohiroet al.[34]; and subsequent refinements by Minamikawaet al.[35] and Mukher- jeeet al.[48], Dexheimeret al.[87]; show that parity-doublet equations of state can support neutron-star masses of2.0−2.2M ⊙, consistent with recent pulsar observations [88, 89], while remaining compatible with"},{"citing_arxiv_id":"2510.23750","ref_index":19,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Study of Neutron Star Properties under the Two-Flavor Quark NJL Model","primary_cat":"astro-ph.HE","submitted_at":"2025-10-27T18:30:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Hybrid neutron star EOS constructed from DDME2 hadronic and two-flavor NJL quark models with quintic interpolation requires early crossover near saturation density to satisfy PSR J0740+6620 mass and NICER radius constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.05841","ref_index":37,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Compact star properties from an extended linear sigma model","primary_cat":"hep-ph","submitted_at":"2019-07-12T17:03:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The (axial-)vector meson extended linear sigma model yields an equation of state for quark matter that satisfies astrophysical constraints on compact star masses and radii.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}