{"total":13,"items":[{"citing_arxiv_id":"2606.29576","ref_index":89,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quark and hybrid stars with renormalization group improvement of NNLO perturbative QCD","primary_cat":"nucl-th","submitted_at":"2026-06-28T19:42:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"RGOPT-resummed NNLO pQCD EoS for massive quarks in beta equilibrium is fitted and applied to construct pure quark stars (X=3.08-3.58) and hybrid stars (X~2-2.98) compatible with PSR J0740+6620 and GW190814.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23929","ref_index":92,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.26308","ref_index":166,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nuclear Physics of Binary Neutron Star Mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-05-25T19:59:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21578","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational wave detectability range informed by external messengers","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The Targeted Detectability Range (TDR) incorporates sky localization, inclination constraints, and mass bounds from external messengers to evaluate gravitational-wave detectability for gamma-ray bursts observed during LIGO-Virgo-KAGRA's first three runs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19761","ref_index":51,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Magnetized neutron stars: perturbative versus fully-numerical approaches","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T12:36:57+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Direct comparison of Konno-99 perturbative and LORENE numerical methods for poloidal magnetized neutron stars shows perturbative validity for observed fields up to ~10^16 G and numerical resolution limits below ~10^10 G.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14447","ref_index":115,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons","primary_cat":"nucl-th","submitted_at":"2026-05-14T06:41:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-energy slopes between 40 and 58 MeV, with HESS J1731-347 and GW170817 data playing,","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"SimultaneousM−Rmeasurements of various pulsars (by NICER and HESS collaborations) and tidal deformability measurement of 1.4M ⊙ compact star from GW170817 (by LIGO collaboration) are listed below. 1. For PSR J0030+0451M= 1.40 +0.13 −0.12 M⊙ andR= 11.71 +0.88 −0.83 km reported by Vinciguerraet al.[22]. 2. For PSR J0740+6620M= 2.08 +0.07 −0.07 M⊙ andR= 12.92 +2.09 −1.13 km reported by Dittmannet al.[115]. 3. For PSR J0437-4715M= 1.418 +0.037 −0.037 M⊙ andR= 11.36 +0.95 −0.63 km reported by Choudhuryet al.[23]. 4. For PSR J1231-1411M= 1.04 +0.05 −0.03 M⊙ andR= 12.6 +0.3 −0.3 km reported by Salmiet al.[27]. 5. For PSR J0614-3329M= 1.44 +0.06 −0.07 M⊙ andR= 10.29 +1.01 −0.86 km reported by Mauviardet al.[116]. 6. For HESS J1731-347M= 0.77 +0.20 −0.17 M⊙ andR= 10."},{"citing_arxiv_id":"2604.09154","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"From binding and saturation to criticality in nuclear matter with lattice effective field theory","primary_cat":"nucl-th","submitted_at":"2026-04-10T09:40:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Improved leading-order lattice Hamiltonians lower the liquid-gas critical temperature of symmetric nuclear matter to 13.50(17)-13.71(19) MeV while improving zero-temperature binding energies and saturation point.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"C98, 025804 (2018), 1807.00596. [7] A. Carbone and A. Schwenk, Phys. Rev. C100, 025805 (2019), 1904.00924. [8] J. Keller, K. Hebeler, and A. Schwenk, Phys. Rev. Lett.130, 072701 (2023), 2204.14016. [9] C. J. Horowitz and A. Schwenk, Nucl. Phys. A776, 55 (2006), nucl-th/0507033. [10] C. J. Horowitz and A. Schwenk, Phys. Lett. B638, 153 (2006), nucl-th/0507064. [11] S. Typel, G. Ropke, T. Klahn, D. Blaschke, and H. H. Wolter, Phys. Rev. C81, 015803 (2010), 0908.2344. 20 0.0 0.4 0.8 1.2 1.6 (MeV 1) 310 290 270 250 E (MeV) 36Ar 0.0 0.4 0.8 1.2 1.6 (MeV 1) 350 330 310 290 40Ca ESU(4) ESU(4) + V3S1 + V1S0 ELO3 0.0 0.4 0.8 1.2 1.6 (MeV 1) 220.0 186.7 153.3 120.0 E (MeV) 24Mg 0.0 0.4 0.8 1.2 1.6 (MeV 1) 240 210 180"},{"citing_arxiv_id":"2604.06308","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Anisotropic hybrid stars: Interplay of superconductivity and magnetic field leading to gravitational waves","primary_cat":"astro-ph.HE","submitted_at":"2026-04-07T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New phenomenological anisotropy profiles in hybrid stars, driven by superconductivity and magnetic fields, lead to enhanced masses and continuous gravitational wave emission.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Bucciantini, and L. Del Zanna, Astron. Astrophys.654, A162 (2021), arXiv:2106.00603 [astro- ph.HE]. [19] P. Haensel and A. Y. Potekhin, Astron. Astrophys.428, 191 (2004), arXiv:astro-ph/0408324. [20] R. L. Bowers and E. P. T. Liang, Astrophys. J.188, 657 (1974). [21] L. L. Lopes and H. C. Das, Eur. Phys. J. C84, 1049 (2024), arXiv:2405.00072 [astro-ph.HE]. [22] J. M. Z. Pretel and C. Zhang, JCAP10, 032 (2024), arXiv:2401.12519 [nucl-th]. [23] I. Easson and C. J. Pethick, Phys. Rev. D16, 275 (1977). [24] S. K. Lander, N. Andersson, and K. Glampedakis, Mon. Not. R. Astron. Soc.419, 732 (2012), arXiv:1106.6322 [astro-ph.SR]. [25] L. Paulucci, E. J. Ferrer, V. de la Incera, and J. E. Hor- vath, Phys. Rev. D83, 043009 (2011), arXiv:1010."},{"citing_arxiv_id":"2511.07226","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Renormalization-Group Invariant Parity-Doublet Model for Nuclear and Neutron-Star Matter","primary_cat":"nucl-th","submitted_at":"2025-11-10T15:46:14+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.08707","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutrino diagnostics of hadron-quark phase transition in Neutron Stars","primary_cat":"astro-ph.HE","submitted_at":"2025-10-09T18:11:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Neutrino light curves from neutron stars may show an enhanced peak-to-plateau ratio, a density-tracing delay, and transient spectral hardening as diagnostics of hadron-quark phase transitions on 10-50 ms timescales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04654","ref_index":84,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Phase transitions in neutron stars and their links to gravitational waves","primary_cat":"astro-ph.HE","submitted_at":"2019-07-05T19:07:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"are the binding energy per nucleon ( E0), the nuclear incompressibility ( K0), the isospin asymmetry energy (J) and its slope ( L0), and the effective mass ( m∗/mN), all fixed to their n0 values. However, the standard RMF approximation is not parameterized to fix L0 at the saturation density, a quantity that has become more tightly constrained in recent years and may have a significant effect on the composition and properties of NSs (see Refs. [84, 85] and references therein). One of the ways to set L0 is to consider medium effects of the effective interaction, choosing density functionals for the meson-baryon couplings. More specifically, the density dependence is extracted from Dirac-Brueckner calculations in which nucleon interactions in the nuclear medium are obtained from nucleon-nucleon potentials consistent with scattering experiments [86]."},{"citing_arxiv_id":"1907.06597","ref_index":63,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hot quark matter and (proto-) neutron stars","primary_cat":"nucl-th","submitted_at":"2019-07-05T16:10:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"An extended PNJL model locates the QCD critical end point and predicts that proto-neutron stars contain hyperons and Delta-isobars but no deconfined quarks, which appear only in cold neutron stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}